Author name code: thompson-barbara
ADS astronomy entries on 2022-09-14
author:"Thompson, Barbara J."
------------------------------------------------------------------------  

Title: Defining the Middle Corona
Authors: West, Matthew J.; Seaton, Daniel B.; Wexler, David B.;
   Raymond, John C.; Del Zanna, Giulio; Rivera, Yeimy J.; Kobelski,
   Adam R.; DeForest, Craig; Golub, Leon; Caspi, Amir; Gilly, Chris R.;
   Kooi, Jason E.; Alterman, Benjamin L.; Alzate, Nathalia; Banerjee,
   Dipankar; Berghmans, David; Chen, Bin; Chitta, Lakshmi Pradeep; Downs,
   Cooper; Giordano, Silvio; Higginson, Aleida; Howard, Russel A.; Mason,
   Emily; Mason, James P.; Meyer, Karen A.; Nykyri, Katariina; Rachmeler,
   Laurel; Reardon, Kevin P.; Reeves, Katharine K.; Savage, Sabrina;
   Thompson, Barbara J.; Van Kooten, Samuel J.; Viall, Nicholeen M.;
   Vourlidas, Angelos
Bibcode: 2022arXiv220804485W
Altcode:
  The middle corona, the region roughly spanning heliocentric altitudes
  from $1.5$ to $6\,R_\odot$, encompasses almost all of the influential
  physical transitions and processes that govern the behavior of
  coronal outflow into the heliosphere. Eruptions that could disrupt
  the near-Earth environment propagate through it. Importantly, it
  modulates inflow from above that can drive dynamic changes at lower
  heights in the inner corona. Consequently, this region is essential
  for comprehensively connecting the corona to the heliosphere and for
  developing corresponding global models. Nonetheless, because it is
  challenging to observe, the middle corona has been poorly studied by
  major solar remote sensing missions and instruments, extending back to
  the Solar and Heliospheric Observatory (SoHO) era. Thanks to recent
  advances in instrumentation, observational processing techniques,
  and a realization of the importance of the region, interest in the
  middle corona has increased. Although the region cannot be intrinsically
  separated from other regions of the solar atmosphere, there has emerged
  a need to define the region in terms of its location and extension
  in the solar atmosphere, its composition, the physical transitions
  it covers, and the underlying physics believed to be encapsulated by
  the region. This paper aims to define the middle corona and give an
  overview of the processes that occur there.

Title: Remote Sensing of Coronal Forces during a Solar Prominence
    Eruption
Authors: Uritsky, V. M.; Thompson, B. J.; DeVore, C. R.
Bibcode: 2022ApJ...935...47U
Altcode: 2022arXiv220502344U
  We present a new methodology-the Keplerian Optical Dynamics Analysis
  (KODA)-for quantifying the dynamics of erupting magnetic structures
  in the solar corona. The technique involves adaptive spatiotemporal
  tracking of propagating intensity gradients and their characterization
  in terms of time-evolving Keplerian areas swept out by the position
  vectors of moving plasma blobs. Whereas gravity induces purely ballistic
  motions consistent with Kepler's second law, noncentral forces such as
  the Lorentz force introduce nonzero torques resulting in more complex
  motions. KODA algorithms enable direct evaluation of the line-of-sight
  component of the net torque density from the image-plane projection
  of the areal acceleration. The method is applied to the prominence
  eruption of 2011 June 7, observed by the Solar Dynamics Observatory's
  Atmospheric Imaging Assembly. Results obtained include quantitative
  estimates of the magnetic forces, field intensities, and blob masses
  and energies across a vast region impacted by the postreconnection
  redistribution of the prominence material. The magnetic pressure
  and energy are strongly dominant during the early, rising phase of
  the eruption, while the dynamic pressure and kinetic energy become
  significant contributors during the subsequent falling phases. Measured
  intensive properties of the prominence blobs are consistent with those
  of typical active-region prominences; measured extensive properties
  are compared with those of the whole pre-eruption prominence and the
  post-eruption coronal mass ejection of 2011 June 7, all derived by
  other investigators and techniques. We show that KODA provides valuable
  information on spatially and temporally dependent characteristics of
  coronal eruptions that is not readily available via alternative means,
  thereby shedding new light on the environment and evolution of these
  solar events.

Title: Science Autonomy for Ocean Worlds Astrobiology: A Perspective
Authors: Theiling, Bethany P.; Chou, Luoth; Da Poian, Victoria;
   Battler, Melissa; Raimalwala, Kaizad; Arevalo, Ricardo, Jr.; Neveu,
   Marc; Ni, Ziqin; Graham, Heather; Elsila, Jamie; Thompson, Barbara
Bibcode: 2022AsBio..22..901T
Altcode:
  No abstract at ADS

Title: The Solaris Solar Polar MIDEX-Class Mission Concept: Revealing
    the Mysteries of the Sun's Poles
Authors: Hassler, Donald M.; Harra, Louise K.; Gibson, Sarah; Thompson,
   Barbara; Gusain, Sanjay; Berghmans, David; Linker, Jon; Basu, Sarbani;
   Featherstone, Nicholas; Hoeksema, J. Todd; Viall, Nicholeen; Newmark,
   Jeffrey; Munoz-Jaramillo, Andres; Upton, Lisa A.
Bibcode: 2022cosp...44.1528H
Altcode:
  Solaris is an exciting, innovative &amp; bold mission of discovery to
  reveal the mysteries of the Sun's poles. Solaris was selected for Phase
  A development as part of NASA's MIDEX program. Solaris builds upon
  the legacy of Ulysses, which flew over the solar poles, but Solaris
  provides an entirely new feature remote sensing, or IMAGING. Solaris
  will be the first mission to image the poles of the Sun from ~75
  degrees latitude and provide new insight into the workings of the
  solar dynamo and the solar cycle, which are at the foundation of our
  understanding of space weather and space climate. Solaris will also
  provide enabling observations for improved space weather research,
  modeling and prediction with time series of polar magnetograms and
  views of the ecliptic from above, providing a unique view of the
  corona, coronal dynamics, and CME eruption. To reach the Sun's poles,
  Solaris will first travel to Jupiter, and use Jupiter's gravity to
  slingshot out of the ecliptic plane, and fly over the Sun's poles
  at ~75 degrees latitude. Just as our understanding of Jupiter &amp;
  Saturn were revolutionized by polar observations from Juno and Cassini,
  our understanding of the Sun will be revolutionized by Solaris.

Title: Developing a vision for maturing the Heliophysics
infrastructure towards open science: The LIKED online resource and
    the DIARieS analysis ecosystem.
Authors: Ringuette, Rebecca; Thompson, Barbara; Mcgranaghan, Ryan;
   Engell, Alexander; Gerland, Oliver
Bibcode: 2022cosp...44.3521R
Altcode:
  The Heliophysics infrastructure is filled with a plethora of useful
  resources such as data archives, software packages, analysis tutorials,
  educational resources, related publications, and the people involved
  in developing these resources. However, these resources are not
  interlinked or interoperable, presenting a problematic barrier for
  progress towards open science in Heliophysics. We summarize a vision
  to address these barriers using currently available modern technology
  and techniques resulting in two new infrastructure components: LIKED,
  a LIbrary KnowledgE and Discovery (LIKED) online resource for finding
  and accessing knowledge and infrastructure resources; and DIARieS, an
  analysis ecosystem to simplify Discovery, Implementation, Analysis,
  Reproducibility, and Sharing (DIARieS) of scientific results and
  environments. LIKED addresses the findability and accessibility
  barriers for Heliophysics resources by building upon the successes
  of Wikipedia and the technologies supporting internet search engines
  (e.g. Google). DIARieS builds upon the new capabilities that will be
  possible through LIKED and various modern technologies (e.g. Kubernetes
  clusters and containerization) combined with innovative ideas to
  offer a viable solution for open science, including interoperability,
  reproducibility, and interactive dissemination. The creation of these
  new infrastructure elements requires coordination between various
  members and groups in the Heliophysics and related communities. We thus
  request feedback from the extended COSPAR community on this vision,
  and point those interested to the two related papers submitted to the
  2022 COSPAR Space Weather Roadmap.

Title: Exploring Structures and Flows with NASA's under-construction
    PUNCH mission
Authors: DeForest, Craig; Gibson, Sarah; Thompson, Barbara;
   Malanushenko, Anna; Desai, Mihir; Elliott, Heather; Viall, Nicholeen;
   Cranmer, Steven; de Koning, Curt
Bibcode: 2022cosp...44.1077D
Altcode:
  The Polarimeter to UNify the Corona and Heliosphere is a NASA Small
  Explorer to image the corona and heliosphere as parts of a single
  system. PUNCH comprises four ~50kg smallsats, each carrying one imaging
  instrument, that work together to form a single "virtual coronagraph"
  with a 90° field of view, centered on the Sun. Scheduled for joint
  launch with NASA's SPHEREx mission, PUNCH starts its two-year prime
  science phase in 2025. PUNCH will generate full polarized image
  sequences of Thomson-scattered light from free electrons in the corona
  and young solar wind, once every four minutes continuously. This
  enables tracking the young solar wind and turbulent structures within
  it as they disconnect from the Sun itself, as well as large transients
  such as CMEs, CIRs, and other shocks within the young solar wind. A
  student-contributed X-ray spectrometer (STEAM) will address questions
  of coronal heating and flare physics. We present motivating science,
  expected advances, mission status, and how to get involved with PUNCH
  science now.

Title: Connecting the Sun/Corona/Heliosphere Through the Combination
    of Remote Sensing Data Products and PSP Observations
Authors: Alzate, Nathalia; Nieves-Chinchilla, Teresa; Thompson,
   Barbara; Di Matteo, Simone; Morgan, Huw; Seaton, Daniel
Bibcode: 2022cosp...44.1349A
Altcode:
  Understanding the Sun/Corona/Heliosphere system requires effectively
  establishing a link between in situ measurements and remote observations
  by characterizing structure and plasma properties of the inner
  corona. Additionally, we need to resolve the line-of-sight (LOS)
  limitations of coronagraph and EUV observations to properly identify
  the location of structures and their temporal density changes. Our
  advanced image processing techniques can reveal structures (on various
  timescales) in both EUV and visible-light data providing continuous
  tracking of brightness enhancements from the coronal base out to the
  radial extended corona. Our most recent work using STEREO/COR1 and
  GOES-R/SUVI has proven crucial in linking the low to high corona and has
  facilitated the interpretation of PSP data. Further, our time-dependent
  rotational tomography of coronal data yields empirically derived
  coronal density distribution directly comparable to PSP measurements
  at perihelion. We present our current work that combines PSP data
  with RS EUV/WL observations of the corona, via the use of coronal
  rotational tomography from SOHO/LASCO and STEREO/COR2 observations,
  which provides the capabilities to reconstruct features in the solar
  wind and subsequently study the evolution between EUV/WL and in situ
  of the plasma flows that give rise to them.

Title: Solar Energetic Particle (SEP) events forecasting in the
    framework of SPRINTS
Authors: Engell, Alexander; Thompson, Barbara; Richardson, Ian G.;
   Dayeh, Maher; Falconer, David
Bibcode: 2022cosp...44.1147E
Altcode:
  We present the Space Radiation Intelligence System (SPRINTS) and its
  current capabilities to forecast solar energetic particles (SEP) using
  streamlined data-driven and machine-learning processes. SPRINTS is
  designed as a community ecosystem to ensure scientific transparency and
  can be deployed to any infrastructure environment. Its current data is
  comprised of GOES X-ray and proton data from 1986-present and ACE/DSCOVR
  from 1997-present in a Timescale database with APIs. The time-series
  database is supported by flare, SEP, and CME event catalogs as well as
  event associated catalogs such as flares associated with SEPs, CMEs and
  radio bursts. Within the framework of SPRINTS, these catalogs can be
  improved through scientific crowd-sourcing methods (e.g., versioning)
  thereby allowing critical alignment of both underlying data and event
  relationships. This forms a ML-ready dataset process for the community
  interested in establishing consistent train, test and validation and
  verification processes when building models to predict flares, SEPs,
  and CMEs. SPRINTS is coupled to the MagPy (i.e., MAG4) forecasting
  capability whereby it takes probabilistic forecast parameters of
  interest based on free-energy proxies for flare parameters including
  flare flux, fluence and peak ratio of the long and short X-ray channels
  required by the post-eruptive machine-learned models developed. This
  gives a continuous pre- and post-eruptive forecasting capability as new
  information (e.g., flare eruptions and CME kinematic) becomes available
  to the system. We will present initial models results for the Air
  Force Research Laboratory SEP forecast requirements (10 MeV @ 10 pfu,
  10 MeV @40 pfu, 30 MeV @10 pfu, 50 MeV @10 pfu, 100 MeV @ 1 pfu) at 12
  hour and 24 hour cadences. SPRINTS is currently providing forecasts in
  real-time through a REST API and has supporting dashboards near-real
  time forecasts, historical analysis, and event relationship analysis.

Title: Expected results for the cradle of the Solar Wind with the
    Polarimeter to UNify the Corona and Heliosphere (PUNCH)
Authors: DeForest, Craig; Gibson, Sarah; De Koning, Curt A.; Thompson,
   Barbara; Malanushenko, Anna; Desai, Mihir; Elliott, Heather; Viall,
   Nicholeen; Cranmer, Steven
Bibcode: 2022cosp...44.1324D
Altcode:
  The Polarimeter to UNify the Corona and Heliosphere is a NASA Small
  Explorer to image the corona and heliosphere as parts of a single
  system. Imaging the corona and heliosphere together from a constellation
  of four synchronized smallsats, PUNCH will — starting in 2025 —
  provide a unique window on global structure and cross-scale processes
  in the outer corona and young solar wind. PUNCH science is informed
  by, and complements, the results of PSP and Solar Orbiter; and will
  synergize with PROBA3/ASPIICS. We present early prototype results from
  STEREO/SECCHI and current preparation work to enable PUNCH science
  when data arrive, discuss anticipated results from the deeper-field,
  higher time resolution imaging that PUNCH will provide, and describe
  how to get involved with PUNCH science now.

Title: Facilitating Heliophysics Data Discovery with Cloud
Collaboration: Development for the HSO Connect Program
Authors: Alshatnawi, Amr; Thompson, Barbara; Ireland, Jack; Roberts,
   D. Aaron; Damas, M. Chantale
Bibcode: 2021AGUFMSA15B1930A
Altcode:
  The HSO (Heliophysics System Observatory) Connect programs goal is to
  link the Heliophysics community together, and establish a connection for
  collaboration and data sharing. It is often difficult for researchers to
  share data and also find new resources, which leads many of them to use
  a specific data set or resource for most of their research. Since there
  are numerous data sources, developing an environment for data sharing
  is very beneficial as it will allow scientists to reach different data
  more easily and efficiently. The focus of this project was to develop
  and test different cloud collaboration environments. To achieve this
  the NASA Amazon Web Services cloud was used by the HelioAnalytics
  team for collaboration on code development. This cloud allowed the
  development of the Heliophysics JupyterHub, which was used to create
  Jupyter notebooks that researched multiple instances of data and model
  products from different missions. JupyterHub also allows users to
  configure their environment, so they can access and request different
  data. In order to share these notebooks and data, a GitHub site was
  created for the HSO Connect project. The objective of the GitHub site
  is to facilitate data resources and code sharing. This site will also
  contain different data models, tools, and services that will support
  the goal of the program. Developing and using these different cloud
  collaboration tools will provide a more efficient and simple way to
  access and share data, it will also improve code development as it will
  allow participants to share along with work on each others code. The
  outcome achieved from using these cloud collaboration tools will help
  connect observations from HSO missions with other observations from
  different Science Mission Directorate missions.

Title: Report on a Workshop to Understand Heliophysics Research
    Infrastructure
Authors: Thomas, Brian; Candey, Robert; Fung, Shing; Ireland, Jack;
   Jian, Lan; Kirk, Michael; Kuznetsova, Maria; McGranaghan, Ryan;
   Roberts, D. Aaron; Thompson, Barbara
Bibcode: 2021AGUFMSH44C..01T
Altcode:
  We report observations and findings from a three-day virtual workshop
  on heliophysics research infrastructure. The workshop, held on May
  17-19, 2021, was organized by the NASA Goddard Space Flight Center
  to examine the current NASA heliophysics research infrastructure
  and determine which elements were most utilized, what gaps exist in
  these elements between current utility and desired capability and,
  from a user standpoint, what a future state for the infrastructure
  might look like. Approximately 40 subject matter experts (SMEs)
  with backgrounds in heliophysics research, computer science and
  research infrastructure were gathered to consider these topics. Key
  gaps identified include enhancements to science data products,
  improved support for collaboration and open science, and a need for
  more sophisticated information discovery. We will discuss these gaps
  and how they connect to the participants imagined future state which
  emphasizes a faster ability to get to the good stuff by improved
  service delivery and infrastructure support.

Title: Towards a Coherent View of the Sun/Corona/Heliosphere:
    Combining Remote Sensing Data Products with PSP In Situ Measurements
Authors: Alzate, Nathalia; Morgan, Huw; Seaton, Daniel; Thompson,
   Barbara; Nieves-Chinchilla, Teresa; Di Matteo, Simone; Viall, Nicholeen
Bibcode: 2021AGUFMSH24C..02A
Altcode:
  In situ (IS) heliospheric measurements and remote sensing
  observations contribute crucial information to our understanding of
  the Sun/Corona/Heliosphere as a single system. In Situ measurements by,
  e.g., Parker Solar Probe (PSP), are detailed and precise measurements of
  physical observables (e.g., magnetic field components), which cannot
  be gained from remote observations. Remote sensing observations,
  in turn, provide the large-scale context, which is absent from
  the in situ data taken at one point in space. Therefore, to
  understand the Sun/Corona/Heliosphere system, we need to effectively
  establish a link between in situ measurements and remote sensing
  observations by characterizing structure and plasma properties of
  the inner corona. Additionally, we need to resolve the line-of-sight
  limitations of white-light (WL) coronagraph and Extreme Ultraviolet
  (EUV) observations to properly identify the location of structures and
  their temporal density changes. Previous studies have identified outward
  propagating density variations in the solar wind (on timescales of hours
  up to ~3 days) that have a plasma composition of coronal origin and that
  can be traced down through the field of view of STEREO/COR2 (~2.5-15
  Rs). Our advanced image processing techniques can reveal structures
  (on various timescales) in both EUV and WL data providing continuous
  tracking of brightness enhancements from the coronal base out to the
  radial extended corona. Our most recent work using STEREO/COR1 and
  GOES-R/SUVI observations has proven crucial in linking the low to high
  corona and has facilitated the interpretation of PSP data. Further, our
  time-dependent rotational tomography of coronal data yields empirically
  derived coronal density distribution directly comparable to PSP
  measurements at perihelion. We present our current work that combines
  PSP data with remote sensing EUV/WL observations of the corona, via the
  use of coronal rotational tomography from SOHO/LASCO and STEREO/COR2
  observations, which provides the capabilities to reconstruct features
  in the solar wind and subsequently study the evolution between EUV/WL
  and in situ of the plasma flows that give rise to them.

Title: Heliophysics: A small field with big data science
Authors: Thompson, Barbara; Bard, Christopher; Dorelli, John;
   McGranaghan, Ryan; Kirk, Michael; Narock, Ayris
Bibcode: 2021AGUFM.U51B..01T
Altcode:
  Heliophysics is a relatively small community, compared to other NASA
  Science Divisions (Astrophysics, Planetary, and Earth Science). However,
  Heliophysics has cross-cutting cross-disciplinary relationships that
  easily connect to, and are applied to, all of other science domains. To
  start, the Sun is a typical astrophysical object. It is a rotating
  sphere with an extended atmosphere, it exhibits seasons and islands
  of activity, and there are local processes that strongly couple to
  global dynamics; this connects well to many problems in the Earth
  Sciences. Also, the Suns atmosphere extends to form the heliosphere,
  drives processes and interacts with all of the planetary environments,
  and reaches to the heliopause and interstellar medium. Additionally,
  Heliophysics relies on a wide variety of instrumentation: In
  situ, remote sensing, spectroscopy, as well as constellation &amp;
  multi-viewpoint observatories. The field is faced with common data
  science challenges, such as: (1) Multi-domain, multi-variate processes
  (2) Wide range of scales: temporal, spatial, energetic, spectral,
  etc. (3) Forecasting, data assimilation, operational modeling. Though
  relatively new, Heliophysics is a well-developed community with strong
  roots that can support strong branches. Our ability to connect means
  that we can benefit from other areas, and vice versa. By emphasizing
  cross-disciplinary collaboration and resource development, we can form
  a foundation for Open Science across multiple research domains.

Title: Early Results from Whole Heliosphere Planetary Interactions
    (WHPI) Campaigns
Authors: Thompson, Barbara; Allen, Robert; de Toma, Giuliana; Gibson,
   Sarah; Qian, Liying
Bibcode: 2021AGUFMSH11A..03T
Altcode:
  The Whole Heliosphere and Planetary Interactions (WHPI) is an
  international initiative focused around the solar minimum period that
  aims to understand the interconnected sun-heliospheric-planetary system,
  by facilitating and encouraging interdisciplinary activities. Particular
  WHPI science foci include the global connected structure of the
  heliosphere and planetary space environments/atmospheres, the
  origins and impacts of high-speed solar wind streams, CMEs from
  sun-to-heliopause, and comparative solar minima. This is achieved
  through a series of coordinated observing campaigns, including Parker
  Solar Probe perihelia, and virtual interactions including a dedicated
  workshop where observers and modelers get together to discuss, compare,
  and combine research results. We present a summary of the outcomes and
  activities of the WHPI science workshop held September 13-17, 2021,
  and an update on the repository of data (observations and models,
  Sun to solar wind to planets) that have been gathered.

Title: SynCOM: Synthetic Corona Outflow Model for the Heliophysics
    community
Authors: Moraes Filho, Valmir; Uritsky, Vadim; Thompson, Barbara;
   DeForest, Craig
Bibcode: 2021AGUFMSH24C..06M
Altcode:
  Numerous methods for measuring coronal flow velocities have been
  developed over the years. These measurements are central to our
  understanding of the origin of the solar wind and serving to upcoming
  missions that address this problem, such as the Polarimeter to Unify the
  Corona and Heliosphere (PUNCH) mission. However, many of the existing
  flow tracking methods provide qualitatively reasonable outcomes, their
  quantitative validation across the wide range of coronal altitudes
  remains a problem. The lack of precise knowledge about the targeted
  velocity field is the primary obstacle, making it impossible to compare
  algorithms attempting to estimate flow parameters for the same coronal
  structure. To address this problem, we are designing the Synthetic
  Corona Outflow Model (SynCOM) an empirical data-driven model of a
  dynamic solar corona based on previous high-resolution observations. The
  SynCOM model mimics the transient and quasi-periodical behavior present
  in the actual solar corona, such as the one observed by STEREO-A/COR
  2. The SynCOM outputs exhibit a true-to-life radial decay of the
  polarized brightness and include stochastic components accounting for
  physical fluctuations of plasma outflows and instrumental noise. Since
  the model has a predefined distribution of flow velocity and an
  adjustable signal-to-noise ratio, it can be used for testing a variety
  of data analysis methods used to measure coronal flows. Adjusting SynCOM
  settings for specific coronal conditions and instrumental parameters
  enables a straightforward comparison of accuracy and performance of
  different data analysis methods and measurement techniques designed
  to quantify velocity and acceleration in the corona. In this work,
  we will present examples of the application of SynCOM for verifying
  observational requirements for detecting coronal flows beyond the
  range of altitudes covered by previously operated coronagraphs; and
  benchmarking popular flow tracking codes used by the coronal physics
  community, and cross-validating their outputs.

Title: Acceleration in the Low Corona of CMEs Associated with Solar
    Energetic Particle Events
Authors: St Cyr, O.; Richardson, Ian; Thompson, Barbara; Burkepile,
   Joan; Balmaceda, Laura; Fry, Dan; Parker, Linda
Bibcode: 2021AGUFMSH55F1914S
Altcode:
  We report here on the initial accelerations of coronal mass ejections
  (CMEs) associated with 25 MeV solar energetic proton events (SEPs)
  during the period 1980-2017. Primary CME observations in the low corona
  were obtained at Mauna Loa Solar Observatory (MLSO) and, where possible,
  they were combined with spacebased observations from the SMM C/P,
  P78-1 Solwind, and SOHO LASCO coronagraphs. We identified &gt;100
  SEPs with associated MLSO observations of CMEs, and we were able to
  combine many of those with the spacebased coronagraphs to reveal the
  initial and middle-coronal acceleration of the SEP-associated CMEs. We
  were able to determine both an instantaneous maximum acceleration as
  well as an average acceleration in the low corona. We compare these
  measured values with proxy determinations of acceleration and with
  their use in predicting SEP properties.

Title: Solar Energetic Particle Events Associated With Coronal Mass
    Ejections Observed by the Mauna Loa Solar Observatory
Authors: Richardson, Ian; St Cyr, O.; Burkepile, Joan; Thompson,
   Barbara
Bibcode: 2021AGUFMSH55F1910R
Altcode:
  Over 100 solar energetic particle (SEP) events including ~25 MeV
  protons associated with coronal mass ejections (CMEs) observed by the
  Mauna Loa Solar Observatory (MLSO) coronagraphs have been identified
  in 1980-2017. These SEP events were detected by instrumentation
  on spacecraft such as SOHO, Wind, ACE, IMP 8, ISEE 3, Helios and
  Ulysses. They range from three Ground Level Enhancements, also
  observed at high energies by neutron monitors, to small events that
  are barely evident above the instrumental background, as well as Fe-
  or electron-rich or poor events. We summarize the properties of these
  SEP events and the associated solar phenomena (e.g., CMEs observed
  by MLSO and, if available, spacecraft coronagraphs, flares, radio
  emissions) and discuss several examples. We demonstrate how ground-based
  coronagraphs can provide an early assessment of the CME parameters prior
  to the arrival of particles at Earth. We also discuss whether these CME
  parameters are related to the properties of the associated SEP events.

Title: Magnetic Field Curvature In A Filament Channel Derived From
    Oscillation Measurements And MHD Modeling
Authors: Kucera, T. A.; Luna, M.; Torok, T.; Muglach, K.; Downs, C.;
   Sun, X.; Thompson, B.; Karpen, J.; Gilbert, H.
Bibcode: 2021AAS...23811306K
Altcode:
  We have used measurements of repeated large amplitude longitudinal
  oscillations (LALOs) in an active region filament to diagnose the
  curvature of the magnetic field in the filament channel and compared the
  results with predictions of an MHD flux-rope model based on magnetograms
  of the region. In May and June of 2014 Active Region 12076 exhibited a
  complex of filaments undergoing repeated oscillations over the course
  of twelve days. The central filament channel exhibited emerging and then
  canceling magnetic flux that resulted in multiple activations, filament
  eruptions, and eight oscillation events, which we analyzed using GONG
  H-alpha data. Luna and Karpen (2012) model LALOs as oscillations of
  magnetized filament plasma moving along dipped magnetic field lines
  with gravity as a restoring force. Under this model the period of these
  oscillations can be used to estimate the curvature of the magnetic
  field in the location of the filament threads. Utilizing this, we find
  that the measured periods in the central filament ranging from 34-74
  minutes should correspond to magnetic field curvatures of about 30-136
  Mm. We also derive radii of curvature for the central filament channel
  using a flux-rope model that is based on an SDO/HMI magnetogram of the
  region. The rope is constructed using the analytic expressions by Titov
  et al. (2018) and then numerically relaxed towards a force-free state in
  the zero-beta MHD approximation, where gravity and thermal pressure are
  neglected. For comparison, we also employ a nonlinear force-free field
  (NLFFF) extrapolation of the active region. We compare the results
  of these different ways of attempting to determine the field in the
  filament channel.

Title: Non-Robotic Science Autonomy Development
Authors: Theiling, Bethany; Brinckerhoff, William; Castillo-Rogez,
   Julie; Chou, Luoth; Da Poian, Victoria; Graham, Heather; Hosseini,
   Sona S.; Lyness, Eric; MacKinnon, James; Neveu, Marc; Raimalwala,
   Kaizad; Thompson, Barbara
Bibcode: 2021BAAS...53d.048T
Altcode: 2021psad.rept..048T
  Non-robotic science autonomy is the ability of an instrument
  to analyze its own data for calibration, optimization, and
  real-time decision-making, and processing software for rapid data
  interpretation. Advancing science autonomy will enhance science return
  and enable missions with prohibitive data link rates / time and in
  extreme environments.

Title: Solar Flares and Coronal Mass Ejections
Authors: Thompson, Barbara J.; Qiu, Jiong; Lugaz, Noe; Webb, David F.
Bibcode: 2021GMS...258..179T
Altcode:
  No abstract at ADS

Title: Information Architecture and Data Utilization: Two Overarching
    Clusters Supporting the COSPAR International Space Weather Action Team
    (ISWAT) Initiative
Authors: Fung, Shing; Thompson, Barbara; Masson, Arnaud
Bibcode: 2021cosp...43E2394F
Altcode:
  Space weather research and forecasting require the availability and
  accessibility of pertinent datasets. Depending on the applications:
  research analysis, modeling, or space weather forecast operations,
  the requirements of data types, data volume, and data sources (e.g.,
  real-time data sources, data repositories, or modeling centers), can
  be quite different. Different data products, ranging from space-based
  and ground-based measurements, to model results, and to event lists or
  catalogs, can have diverse organizations and formats. Complexity in
  data resources, data types, and measurement or parameter types could
  lead to proliferation of services and tools required to search, access,
  and analyze the data. The recently inaugurated COSPAR ISWAT initiative
  (https://www.iswat-cospar.org/iswat-cospar) aspires to provide a
  global hub for collaborations addressing challenges across the field
  of space weather, and more generally heliophysics. Among the various
  topical clusters, Information Architecture and Data Utilization are two
  overarching clusters designed to address effective and efficient data
  access and analysis across all ISWAT activities. While Information
  Architecture aims to facilitate the development of a global network
  of distributed resources for space weather research, analysis,
  forecasting and capabilities assessment, Data Utilization focuses
  on issues regarding preparation of observational data sets ready for
  data assimilation, model validation and utilization as input to data
  science algorithms. This presentation describes the various tasks being
  pursued by these overarching clusters. With the newest developments in
  data science and advancements of machine learning and deep learning, we
  will try to identify ways to help make heliophysics and space weather
  data more readily and directly usable in data science analysis and
  machine learning algorithms.

Title: ISWAT information architecture and data utilization overarching
    clusters, a natural follow up of IHDEA
Authors: Masson, Arnaud; De Zeeuw, Darren; Thompson, Barbara; Roberts,
   D. Aaron; Arviset, Christophe; De Marchi, Guido; Fung, Shing
Bibcode: 2021cosp...43E2422M
Altcode:
  The International Heliophysics Data Environment Alliance (IHDEA) emerged
  as a result of the first International Heliophysics Data Environment
  (IHDE) meeting held at the European Space and Astronomy Centre (ESAC),
  Madrid, Spain, late 2018. Meeting attendees representing NASA, ESA,
  JAXA, and CNES have all agreed that increasing collaboration and
  coordination through the use of standard formats (for both data and
  metadata) and community-based data tools are critical for enabling
  interoperability of data systems and services while improving sharing
  of space-based, ground-based, and model-based heliophysics data
  sets. IHDEA was officially created late 2019 based on a charter and
  bylaws agreed by all agencies mentioned above and Nagoya university-ISEE
  (https://ihdea.net). It is a collaborative organization whose goal is to
  guide the development of a data environment in which the international
  heliophysics and space weather research community can seamlessly find,
  access, and use all electronically accessible, heliophysics relevant
  data sets. The specific mission of the IHDEA is to facilitate global
  access to, and exchange of, high quality scientific data products
  managed across international boundaries. This will be achieved by
  adhering to, and promote the use of, a set of governing metadata
  and data standards, data exchange protocols, visualization and data
  analysis tools. The role of the IHDEA is to serve as the focal point
  to engage the heliophysics data centres and the scientific community,
  foster communication, and identify and develop the standards and
  services that will best serve the heliophysics and space weather
  science needs. As a natural follow up, IHDEA representatives are
  actively participating to the information architecture and data analysis
  overarching groups/clusters of the International Space Weather Action
  Teams (ISWAT). Four action teams have emerged within these clusters
  including: use of metadata to facilitate data science, data preparation
  to advance machine Learning, on Digital Object Identifiers (DOI) to
  support space weather and develop the use of Kamodo to enhance the
  visualization in Python of the output of models. Thanks to the first
  ISWAT conference held in February, each of these teams has defined a
  list of actions. This presentation will be the opportunity to present
  IHDEA, review the list of actions from these teams and invite the
  heliophysics community at large to get involved in this endeavor.

Title: WHPI: A New Initiative on Solar Minimum
Authors: De Toma, Giuliana; Gibson, Sarah; Qian, Liying; Thompson,
   Barbara
Bibcode: 2021cosp...43E.916D
Altcode:
  The Whole Heliosphere and Planetary Interactions (WHPI) is an
  international initiative focused around the solar minimum period
  that aims to understand the interconnected Sun-heliospheric-planetary
  system. The simpler magnetic configuration and infrequency of solar
  eruptions makes solar minimum an ideal time to determine how the Sun's
  radiative output, magnetic field and outflowing solar wind plasma
  interact with the background heliosphere, the Earth and the other
  planets. WHPI follows two similar initiatives during the previous solar
  minima in 1996 and 2008-2009. The success of these efforts relies on a
  broad participation of scientists worldwide and across disciplines. In
  2019-2020 WHPI coordinated 3 different observing campaigns, each a
  solar rotation long: The first was on Mar 12 - Apr 8, 2019 and targeted
  two large, recurrent coronal holes and the associated high-speed solar
  wind streams, the second one on Jun 29 - Jul 26 2019 was centered on
  the total solar eclipse, and the third one on Jan 15 - Feb 11 2020
  corresponded to the 4th Parker Solar Probe (PSP) encounter when the
  Earth and many space observatories were near-radially aligned with
  PSP. We describe the WHPI effort as an example of interdisciplinary
  collaboration and report on the preliminary science results obtained
  during the WHPI campaigns.

Title: SunCET: The Sun Coronal Ejection Tracker Concept
Authors: Mason, James Paul; Chamberlin, Phillip C.; Seaton, Daniel;
   Burkepile, Joan; Colaninno, Robin; Dissauer, Karin; Eparvier, Francis
   G.; Fan, Yuhong; Gibson, Sarah; Jones, Andrew R.; Kay, Christina; Kirk,
   Michael; Kohnert, Richard; Pesnell, W. Dean; Thompson, Barbara J.;
   Veronig, Astrid M.; West, Matthew J.; Windt, David; Woods, Thomas N.
Bibcode: 2021JSWSC..11...20M
Altcode: 2021arXiv210109215M
  The Sun Coronal Ejection Tracker (SunCET) is an extreme ultraviolet
  imager and spectrograph instrument concept for tracking coronal mass
  ejections through the region where they experience the majority
  of their acceleration: the difficult-to-observe middle corona. It
  contains a wide field of view (0-4 R<SUB>⊙</SUB>) imager and a 1 Å
  spectral-resolution-irradiance spectrograph spanning 170-340 Å. It
  leverages new detector technology to read out different areas of the
  detector with different integration times, resulting in what we call
  "simultaneous high dynamic range", as opposed to the traditional high
  dynamic range camera technique of subsequent full-frame images that
  are then combined in post-processing. This allows us to image the
  bright solar disk with short integration time, the middle corona
  with a long integration time, and the spectra with their own,
  independent integration time. Thus, SunCET does not require the use
  of an opaque or filtered occulter. SunCET is also compact - ~15 × 15
  × 10 cm in volume - making it an ideal instrument for a CubeSat or a
  small, complementary addition to a larger mission. Indeed, SunCET is
  presently in a NASA-funded, competitive Phase A as a CubeSat and has
  also been proposed to NASA as an instrument onboard a 184 kg Mission
  of Opportunity.

Title: Tracking CME substructure evolution through the solar wind
Authors: Gibson, S. E.; DeForest, C.; de Koning, C. A.; Fan, Y.;
   Malanushenko, A. V.; Merkin, V. G.; Provornikova, E.; Thompson, B. J.;
   Webb, D. F.
Bibcode: 2020AGUFMSH0280005G
Altcode:
  Future coronagraphs and heliospheric imagers, in particular those
  to be launched on the PUNCH mission, will have the capability to
  track the evolution of CME substructures as the CME moves through and
  interacts with the solar wind. We present analysis using polarization
  data obtained from forward modeling simulations of CMEs in the corona
  and inner heliosphere. We use these data to track the evolution
  of substructures in three dimensions, and consider the diagnostic
  potential of internal substructure vs structure at the front of the
  CME. In particular, we develop methods for extracting information
  about chirality of CME magnetic flux ropes from polarization data.

Title: Contemporary Analysis Methods for Coronagraph and Heliospheric
    Imager Data
Authors: Thompson, B. J.; Attie, R.; Chhiber, R.; Cranmer, S. R.;
   DeForest, C.; Gallardo-Lacourt, B.; Gibson, S. E.; Jones, S. I.;
   Moraes Filho, V.; Reginald, N. L.; Uritsky, V. M.; Viall, N. M.
Bibcode: 2020AGUFMSH031..05T
Altcode:
  Coronagraphs, polarimeters, and heliospheric imagers are providing
  new insight into how structures in the solar wind form and develop as
  they flow from the inner corona into the heliosphere. With this comes
  a whole new frontier of physical observables in 3D, including kinetic
  (velocity and acceleration), thermodynamic (density, temperature, and
  shock boundary), and magnetic field properties. These measurements
  inform and challenge models of global solar wind flow, turbulence,
  and CME propagation. We will discuss recent advances in quantifying
  physical properties of the corona and solar wind using coronagraph
  and heliospheric imager data, and make predictions of what new models
  and instrumentation (including the in-development PUNCH mission)
  will bring us in the future.

Title: Snapshots of Solar Minimum: Data and Model Results From the
    Past Two Solar Minima
Authors: Thompson, B. J.; Gibson, S. E.
Bibcode: 2020AGUFMSH0180002T
Altcode:
  We present an overview of the data and models collected for the
  Whole Sun Month (WSM; 1996) Whole Heliosphere Interval (WHI;
  2008), two international campaigns to study the three-dimensional
  solar-heliospheric-planetary connected system near solar minimum. The
  data and models from WSM, which occurred during the solar minimum
  between Cycles 22 and 23, provided new insight into how solar magnetic
  structure forms the corona and inner heliosphere. WSM inspired the
  Whole Heliosphere Interval campaign during the next solar minimum, and
  the scientific goals expanded to study how solar minimum structures
  affect processes in geospace. The data from WHI extended from below
  the solar photosphere, through interplanetary space, and down to
  Earth's mesosphere. Nearly 200 people participated in aspects of WHI
  studies, analyzing and interpreting data from nearly 100 instruments and
  models in order to elucidate the physics of fundamental heliophysical
  processes. WSM and WHI studies traced the solar activity and structure
  into the heliosphere and geospace, and provided new insight into
  the nature of the interconnected heliophysical system near solar
  minimum. This presentation gives insight into the motivation for the
  Whole Heliosphere and Planetary Interactions campaigns.

Title: SunCET: A CubeSat Mission Dedicated to the Middle Corona
Authors: Mason, J. P.; Seaton, D. B.; Chamberlin, P. C.; Burkepile,
   J.; Colaninno, R. C.; Dissauer, K.; Eparvier, F. G.; Fan, Y.; Gibson,
   S. E.; Jones, A. R.; Kay, C.; Kirk, M. S.; Kohnert, R.; Thompson,
   B. J.; Veronig, A.; West, M. J.; Woods, T. N.
Bibcode: 2020AGUFMSH0300006M
Altcode:
  No abstract at ADS

Title: Velocity Flow Fields Derived from Coronagraph Data
Authors: Moraes Filho, V.; DeForest, C.; Thompson, B. J.; Uritsky,
   V. M.
Bibcode: 2020AGUFMSH0280004M
Altcode:
  In anticipation of the PUNCH mission, we examine deep exposure data
  from the special campaign of the STEREO SECCHI COR2 instrument. Data
  collected over April 14-16, 2014, representing altitudes of 4-15 solar
  radii, show clear flow structures throughout the field of view. We
  examine the variations in the derived flow as a function of altitude
  and polar angle, to present a picture of the solar wind velocities
  and acceleration through the corona and inner heliosphere.

Title: Understanding Solar Energetic Particle Events and CME Dynamics
    in the Low Corona using MLSO and Spacebased Coronagraph Observations -
    Progress Report
Authors: St Cyr, O. C.; Richardson, I. G.; Thompson, B. J.; Burkepile,
   J.; Balmaceda, L.; Fry, D. J.
Bibcode: 2020AGUFMSH0090006S
Altcode:
  We report here on the initial accelerations of coronal mass ejections
  (CMEs) associated with 25 MeV solar energetic proton events (SEPs)
  during the period 1980-1996. Primary CME observations in the low
  corona were obtained at Mauna Loa Solar Observatory (MLSO) and,
  where possible, they were combined with spacebased observations from
  the SMM C/P and P78-1 Solwind coronagraphs. We identified 21 SEPs
  with associated MLSO observations, and we were able to combine 12
  of those with the spacebased coronagraphs to reveal the initial and
  mid-coronal acceleration of the SEP-associated CMEs. We compared them
  with 13 fast CMEs detected by MLSO during the same period with no
  SEPs. The low-to-middle coronal accelerations of the SEP-associated
  CMEs was significantly larger than for those without SEPs. We will
  show examples of these statistics, and we will describe our progress
  extending this work into the SOHO-LASCO era (1996-present).

Title: HSO Connect: Creating User-driven Infrastructure for Space
    Science
Authors: Kirk, M. S.; Fung, S. F.; Ireland, J.; Jian, L.; Kuznetsova,
   M. M.; MacNeice, P. J.; DiBraccio, G. A.; McGranaghan, R. M.; Roberts,
   D. A.; Thomas, B. A.; Thompson, B. J.; Weigand, C.; Zheng, Y.
Bibcode: 2020AGUFMSH0180008K
Altcode:
  The NASA Heliophysics System Observatory (HSO Connect) project is an
  initiative to gain the most utility from data available for space
  physics. The HSO Connect community comprises GSFC/NASA, NCAR's
  Whole Heliosphere and Planetary Interactions (WHPI) program and
  the Parker Solar Probe (PSP) project team at APL (Applied Physics
  Lab). <P />The purpose of HSO Connect is to unify the community and
  provide observations coordinated around the PSP mission and other high
  profile Heliophysics projects requiring unique integration. We share
  the HSO Connect approach to curating and providing resources critical
  to discovery, including observational data, related data products,
  and basic tools to analyze the observations as well as providing the
  same access to models and simulations which explain the data. <P />To
  support an interoperable and reusable data system to last beyond the
  HSO Connect lifetime, we have worked with the community of end users to
  identify, from their perspective, the most impactful "questions" which
  they want HSO Connect to answer for them (for example, "Where the data
  associated with phenomenon "X" might be stored and accessible?"). We
  have utilized this feedback to prioritize how to better combine existing
  capabilities and to identify which infrastructure capabilities need
  to be augmented or created. We will show how we have utilized the
  community feedback to determine both impact and ease of implementation,
  used this information to derive critical requirements for HSO Connect
  and used this information to align existing capabilities and create
  missing infrastructure within resourcing limits.

Title: Filament Oscillations in Active Region 12076
Authors: Kucera, T. A.; Muglach, K.; Luna Bennasar, M.; Karpen, J.;
   Thompson, B.; Gilbert, H.
Bibcode: 2020AAS...23633004K
Altcode:
  We present an analysis of repeated large amplitude longitudinal
  oscillations (LALO) in filaments in Active Region 12076 in May
  and June of 2014. Most of the oscillations were associated with a
  region of emerging and then canceling magnetic flux that resulted
  in multiple activations and filament eruptions. We analyze twelve
  separate oscillations that occur in a complex of filaments in the
  active region over twelve days. Luna and Karpen (2012) model LALO
  in filaments oscillations of magnetized filament plasma moving along
  dipped magnetic field lines with gravity as a restoring force. Under
  this model the period of these oscillations can be used to estimate
  the curvature of the magnetic field in the location of the filament,
  providing observationally derived values to compare with models of the
  magnetic field in the active region corona. Periods ranged from 26-74
  minutes, corresponding to magnetic field curvatures of about 20-130 Mm.

Title: VizieR Online Data Catalog: APOGEE-2 data from DR16 (Majewski+,
    2017)
Authors: Majewski, S. R.; Schiavon, R. P.; Frinchaboy, P. M.;
   Allende Prieto, C.; Barkhouser, R.; Bizyaev, D.; Blank, B.; Brunner,
   S.; Burton, A.; Carrera, R.; Chojnowski, S. D.; Cunha, K.; Epstein,
   C.; Fitzgerald, G.; Garcia Perez, A. E.; Hearty, F. R.; Henderson,
   C.; Holtzman, J. A.; Johnson, J. A.; Lam, C. R.; Lawler, J. E.;
   Maseman, P.; Meszaros, S.; Nelson, M.; Nguyen, D. C.; Nidever, D. L.;
   Pinsonneault, M.; Shetrone, M.; Smee, S.; Smith, V. V.; Stolberg, T.;
   Skrutskie, M. F.; Walker, E.; Wilson, J. C.; Zasowski, G.; Anders,
   F.; Basu, S.; Beland, S.; Blanton, M. R.; Bovy, J.; Brownstein, J. R.;
   Carlberg, J.; Chaplin, W.; Chiappini, C.; Eisenstein, D. J.; Elsworth,
   Y.; Feuillet, D.; Fleming, S. W.; Galbraith-Frew, J.; Garcia, R. A.;
   Garcia-Hernandez, D. A.; Gillespie, B. A.; Girardi, L.; Gunn, J. E.;
   Hasselquist, S.; Hayden, M. R.; Hekker, S.; Ivans, I.; Kinemuchi,
   K.; Klaene, M.; Mahadevan, S.; Mathur, S.; Mosser, B.; Muna, D.;
   Munn, J. A.; Nichol, R. C.; O'Connell, R. W.; Parejko, J. K.; Robin,
   A. C.; Rocha-Pinto, H.; Schultheis, M.; Serenelli, A. M.; Shane, N.;
   Silva Aguirre, E. V.; Sob Eck, J. S.; Thompson, B.; Troup, N. W.;
   Weinberg, D. H.; Zamora, O.
Bibcode: 2020yCat..51540094M
Altcode:
  The second generation of the Apache Point Observatory Galactic Evolution
  Experiment (APOGEE-2) observes the "archaeological" record embedded
  in hundreds of thousands of stars to explore the assembly history and
  evolution of the Milky Way Galaxy. <P />APOGEE-2 maps the dynamical
  and chemical patterns of Milky Way stars with data from the 1-meter
  NMSU Telescope and the 2.5-meter Sloan Foundation Telescope at the
  Apache Point Observatory in New Mexico (APOGEE-2N), and the 2.5-meter
  du Pont Telescope at Las Campanas Observatory in Chile (APOGEE-2S). <P
  />(2 data files).

Title: VizieR Online Data Catalog: APOGEE-2 data from DR16 (Majewski+,
    2017)
Authors: Majewski, S. R.; Schiavon, R. P.; Frinchaboy, P. M.;
   Allende Prieto, C.; Barkhouser, R.; Bizyaev, D.; Blank, B.; Brunner,
   S.; Burton, A.; Carrera, R.; Chojnowski, S. D.; Cunha, K.; Epstein,
   C.; Fitzgerald, G.; Garcia Perez, A. E.; Hearty, F. R.; Henderson,
   C.; Holtzman, J. A.; Johnson, J. A.; Lam, C. R.; Lawler, J. E.;
   Maseman, P.; Meszaros, S.; Nelson, M.; Nguyen, D. C.; Nidever, D. L.;
   Pinsonneault, M.; Shetrone, M.; Smee, S.; Smith, V. V.; Stolberg, T.;
   Skrutskie, M. F.; Walker, E.; Wilson, J. C.; Zasowski, G.; Anders,
   F.; Basu, S.; Beland, S.; Blanton, M. R.; Bovy, J.; Brownstein, J. R.;
   Carlberg, J.; Chaplin, W.; Chiappini, C.; Eisenstein, D. J.; Elsworth,
   Y.; Feuillet, D.; Fleming, S. W.; Galbraith-Frew, J.; Garcia, R. A.;
   Garcia-Hernandez, D. A.; Gillespie, B. A.; Girardi, L.; Gunn, J. E.;
   Hasselquist, S.; Hayden, M. R.; Hekker, S.; Ivans, I.; Kinemuchi,
   K.; Klaene, M.; Mahadevan, S.; Mathur, S.; Mosser, B.; Muna, D.;
   Munn, J. A.; Nichol, R. C.; O'Connell, R. W.; Parejko, J. K.; Robin,
   A. C.; Rocha-Pinto, H.; Schultheis, M.; Serenelli, A. M.; Shane, N.;
   Silva Aguirre, E. V.; Sob Eck, J. S.; Thompson, B.; Troup, N. W.;
   Weinberg, D. H.; Zamora, O.
Bibcode: 2020yCat.3284....0M
Altcode:
  The second generation of the Apache Point Observatory Galactic Evolution
  Experiment (APOGEE-2) observes the "archaeological" record embedded
  in hundreds of thousands of stars to explore the assembly history and
  evolution of the Milky Way Galaxy. <P />APOGEE-2 maps the dynamical
  and chemical patterns of Milky Way stars with data from the 1-meter
  NMSU Telescope and the 2.5-meter Sloan Foundation Telescope at the
  Apache Point Observatory in New Mexico (APOGEE-2N), and the 2.5-meter
  du Pont Telescope at Las Campanas Observatory in Chile (APOGEE-2S). <P
  />(2 data files).

Title: Fast and Wide CMEs without Observed &gt;20 MeV Protons
Authors: Lario, D.; Kwon, R. Y.; Balmaceda, L.; Richardson, I. G.;
   Krupar, V.; Thompson, B. J.; Cyr, O. C. St; Zhao, L.; Zhang, M.
Bibcode: 2020ApJ...889...92L
Altcode:
  Statistical studies have found a close association between large solar
  energetic particle (SEP) events and fast and wide coronal mass ejections
  (CMEs). However, not all fast and wide CMEs have an associated SEP
  event. From the Coordinated Data Analysis Web catalog of CMEs observed
  by the Solar and Heliospheric Observatory (SOHO) between 2009 January
  1 and 2014 September 30, we select fast (plane-of-sky speed &gt;1000
  km s<SUP>-1</SUP>) and wide (plane-of-sky angular width &gt;120°)
  CMEs and determine whether &gt;20 MeV protons were detected by either
  SOHO or the Solar TErrestrial RElations Observatory (STEREO-A or
  STEREO-B). Among the 123 selected CMEs, only 11 did not produce a &gt;20
  MeV proton intensity increase at any of the three spacecraft. We use
  multispacecraft coronagraph observations to reevaluate the speeds
  and widths of the CMEs. The 11 CMEs without observed &gt;20 MeV
  protons tend to be in the narrow and slow end of the distribution
  of the selected CMEs. We consider several factors that might play a
  role in the nonobservation of high-energy particles in these events,
  including (1) the ambiguous determination of the CME parameters,
  (2) the inefficiency of the particle sources to produce &gt;20 MeV
  protons, (3) the lack of magnetic connection between particle sources
  and any spacecraft, and (4) the lack of particles accelerated and
  released during the parent solar eruptions. Whereas the extent of
  the high Mach number regions formed in front of the CME is limited,
  the characteristic that seems to distinguish those fast and wide CMEs
  that lack observed &gt;20 MeV protons is a deficit in the release of
  particles during the solar eruptions.

Title: A New Expansive Catalog of Irradiance Coronal Dimming
Authors: Mason, J.; Attie, R.; Arge, C.; Thompson, B.; Woods, T.
Bibcode: 2020AAS...23535906M
Altcode:
  When coronal mass ejections (CMEs) depart the corona, they leave behind
  a transient void. Such a region evacuated of plasma is known as coronal
  dimming and it contains information about the kinematics of the CME that
  produced it. The dimming can be so great that it reduces the overall
  energy output of the star in particular emission lines, i.e., dimming
  is observable in spectral irradiance. This should be generally true for
  magnetically active stars.We use the Solar Dynamics Observatory (SDO)
  EUV Variability Experiment (EVE) data to search for and parameterize
  dimming. We search these light curves for dimming around &gt;8,500
  ≥C1 solar flares. In prior work, we have found that it is important
  to remove the gradual flare phase from dimming light curves in order
  to obtain slopes and magnitudes that are consistent with what can
  be obtained by spatially isolating flaring loops in spectral image
  data. Applying that method, we come to a total of ~13 million light
  curves in which to search for dimming. We parameterize each light curve
  in terms of magnitude, slope, and duration. Again in prior work, we've
  found that irradiance dimming magnitude and slope are indicators of
  CME mass and speed, respectively. Here, we briefly describe the feature
  detection and characterization algorithms developed and applied to the
  irradiance light curves. Machine learning techniques have been used for
  some of the backend processing pipeline. We also present statistics on
  the catalog itself. All of the code is open source python available
  on GitHub (github.com/jmason86/James-s-EVE-Dimming-Index-JEDI). This
  method may be capable of not only detecting CMEs from other stars,
  but estimating their kinetic energy and frequency of occurrence;
  information needed for assessing exoplanet habitability.

Title: Why do fast and wide CMEs not always produce observable solar
    energetic particles?
Authors: Lario, D.; Kwon, R. Y.; Balmaceda, L.; Richardson, I. G.;
   Zhang, M.; Zhao, L.; Krupar, V.; Thompson, B. J.
Bibcode: 2019AGUFMSH21B..02L
Altcode:
  Statistical studies have found a close association between large
  solar energetic particle (SEP) events and fast and wide coronal
  mass ejections (CMEs). However, not all fast and wide CMEs have an
  associated SEP event. The lack of an intense solar flare during the
  parent solar eruption (Marque et al., 2006) or the slow evolution
  of the CME speed at the origin of the solar eruption (Gopalswamy et
  al., 2017) have been pointed out as possible factors that play a role
  in the absence of high-energy particles. The observation by a given
  spacecraft of the putative SEPs accelerated during these fast CMEs may
  also depend on whether the spacecraft establishes magnetic connection
  with the source of the SEPs and/or on how these SEPs propagate through
  the interplanetary medium. From the list of CMEs in the CDAW LASCO
  catalog during January 2009 - September 2014, we have selected fast
  (plane-of-sky speeds &gt;1000 km/s) and wide (angular width &gt;120
  deg) CMEs and determined whether &gt;25 MeV protons were detected by
  STEREO-A, STEREO-B or SOHO. Among the 123 selected CMEs, only eleven
  CMEs did not produce a &gt;25 MeV proton intensity increase at any
  of the three spacecraft. By characterizing the shocks driven by these
  CMEs, the magnetic connection established between the traveling shock
  and each one of the three spacecraft, and the radio emission observed
  during these events, we analyze the factors responsible for the absence
  of observed &gt;25 MeV proton increases in these events.

Title: Tracking supergranulation near the poles with SDO/HMI
Authors: Attié, R.; Kirk, M. S.; Tremblay, B.; Muglach, K.; Hess
   Webber, S. A.; Pesnell, W. D.; Thompson, B. J.
Bibcode: 2019AGUFMSH13B..01A
Altcode:
  Due to the spherical curvature of the Sun, solar observers suffer
  from an increasing loss of resolution as we move away from the solar
  equator. Thus knowledge of the photospheric flows near the poles
  has eluded the scope of traditional flow tracking algorithms that
  are using granules as tracers of the underlying flows. Using the new
  "Balltracking" framework which we adapted to the observations from
  SDO/HMI, we present an unprecedented analysis of the horizontal flow
  fields at latitudes beyond +/- 60 degrees. The flow fields are derived
  every 4 hours at a spatial resolution of 4 Mm. Using flow segmentation
  techniques, we extract geometric and spectral information on the
  supergranular cells and compare them with those of the supergranulation
  at lower latitude. The correlation with the dynamics of moving magnetic
  features is also investigated.

Title: Antidisciplinary: Tackling the technical and social challenges
    to data science-driven discovery
Authors: McGranaghan, R. M.; Crichton, D. J.; Thompson, B. J.;
   Guhathakurta, M.; Camporeale, E.; Doyle, R. J.
Bibcode: 2019AGUFMSA11C3227M
Altcode:
  Data science refers to the set of tools, technologies, and teams that
  alter the paradigm by which data are collected, managed and analyzed
  . Data science is, therefore, decidedly broader than 'machine learning,'
  and includes instead the full data lifecycle . Never has the need for
  effective data science innovation been greater than now when at every
  turn data-driven discovery is both burdened and invigorated by the
  growth of data volumes, varieties, veracities, and velocities. <P />This
  growing scale of science requires dramatic shifts in collaborative
  research, requiring projects to climb the gradations of collaboration
  from unidisciplinary, to multi-, inter-, and transdisciplinary (Figure
  1, [Hall et al., 2014; NRC, 2015]), and perhaps even to an entirely new
  level that defies any traditional boundary, or anti disciplinary ( <A
  href="https://joi.ito.com/weblog/2014/10/02/antidisciplinar.html">https://joi.ito.com/weblog/2014/10/02/antidisciplinar.html</A>).
  We will discuss the cutting-edge efforts advancing collaborative
  research in Space Physics and Aeronomy, highlight progress, and
  synthesize the lessons to provide a vision for future innovation
  in data science for Heliophysics. We will specifically focus on
  three trail-blazing initiatives: 1) the NASA Frontier Development
  Laboratory; 2) the HelioAnalytics group at the Goddard Space Flight
  Center in cooperation with the NASA Jet Propulsion Laboratory's Data
  Science Working Group; and 3) an International Space Sciences Institute
  project. References: Hall, K.L., Stipelman, B., Vogel, A.L., Huang,
  G., and Dathe, M. (2014). Enhancing the Ef- fectiveness of Team-based
  Research: A Dynamic Multi-level Systems Map of Integral Factors in
  Team Science. Presented at the Fifth Annual Science of Team Science
  Confer- ence, August, Austin, TX. NRC (National Research Council)
  (2015). Enhancing the Effectiveness of Team Science. Washington, DC:
  The National Academies Press. https://doi.org/10.17226/19007.

Title: Coronal Mass Ejections Observed by the Mauna Loa Solar
    Observatory Coronagraphs and Their Association with Solar Energetic
    Particle Events - A Progress Report
Authors: Richardson, I. G.; St Cyr, O. C.; Thompson, B. J.; Burkepile,
   J.; Cane, H. V.
Bibcode: 2019AGUFMSH21B..05R
Altcode:
  Studies using spacebased coronagraph measurements of the middle corona
  indicate that coronal mass ejection (CME) dynamics provide information
  about the characteristics of the resulting solar energetic particle
  (SEP) event. For example, the peak SEP intensity at a given location in
  space is dependent on the CME speed and direction and is also correlated
  with the CME brightness. Furthermore, the SEP spectral hardness appears
  to be related to the initial CME acceleration but this conclusion
  is based on proxies for the acceleration below the field of view of
  spacebased coronagraphs. Combining spacebased coronagraph observations
  with groundbased observations of the low corona would eliminate the need
  for such proxies and allow CME formation and the initial acceleration
  to be observed directly. This paper is a report of progress on a study
  of SEPs associated with CMEs detected since 1980 by coronameters at
  the Mauna Loa Solar Observatory (MLSO) that can measure directly the
  formation and initial accelerations of CMEs low in the corona (i.e.,
  &lt; 2 Rs) that occur during a nominal observing window of 17 - 02
  UT. The MLSO observations of the initial CME signatures are combined
  with observations from spacebased coronagraphs. We then compare the CME
  characteristics with the properties of the related SEPs observed by
  spacecraft near Earth and elsewhere in the heliosphere. The ultimate
  goal is to assess whether there are certain characteristics of MLSO
  CMEs that may indicate a likely association with SEP events, and if
  so, whether a network of groundbased coronagraphs might be used for
  SEP forecasting and for improving understanding of SEP acceleration
  low in the corona.

Title: The PUNCH Bowl: Data System and Data Products for NASA's
    PUNCH Mission
Authors: Thompson, B. J.; DeForest, C.; Gibson, S. E.
Bibcode: 2019AGUFMSA11C3231T
Altcode:
  The Polarimeter to UNify the Corona and Heliosphere (PUNCH) mission
  requires a flexible data system because the anticipated user base will
  be using the data to tackle a wide range of science problems. Some will
  be using PUNCH data in the classic "imager" context, while others will
  be accessing the data to study solar wind dynamics. <P />The PUNCH Bowl
  provide PUNCH data, metadata, analysis tools, and higher-level PUNCH
  data products, which are derived from heliospheric images to provide
  additional information about structure and motion. Additionally, the
  PUNCH Bowl is your access point for PUNCH Recipes: all of the tools,
  code and routines that optimize the use of PUNCH data and streamline
  your access. By running the "recipes" users can easily trace and
  reproduce the steps used by others with minimal effort. The PUNCH Bowl
  is maintained and supported by the PUNCH science team, but welcomes
  contributions from users to ensure that everyone is able to easily
  access all available tools and methods.

Title: AWARE: An Algorithm for the Automated Characterization of
    EUV Waves in the Solar Atmosphere
Authors: Ireland, Jack; Inglis, Andrew R.; Shih, Albert Y.; Christe,
   Steven; Mumford, Stuart; Hayes, Laura A.; Thompson, Barbara J.;
   Hughitt, V. Keith
Bibcode: 2019SoPh..294..158I
Altcode: 2018arXiv180407325I
  Extreme ultraviolet (EUV) waves are large-scale propagating
  disturbances observed in the solar corona, frequently associated with
  coronal mass ejections and flares. They appear as faint, extended
  structures propagating from a source region across the structured
  solar corona. Since their discovery, over 200 papers discussing their
  properties, causes, and physical nature have been published. However,
  despite this their fundamental properties and the physics of their
  interactions with other solar phenomena are still not understood. To
  further the understanding of EUV waves, we have constructed the
  Automated Wave Analysis and Reduction (AWARE) algorithm for the
  measurement of EUV waves. AWARE is implemented in two stages. In the
  first stage, we use a new type of running difference image, the running
  difference persistence image, which enables the efficient isolation of
  propagating, bright wavefronts as they travel across the corona. In the
  second stage, AWARE detects the presence of a wavefront, and measures
  the distance, velocity, and acceleration of that wavefront across the
  Sun. The fit of propagation models to the wave progress isolated in
  the first stage is achieved using the Random Sample Consensus (RANSAC)
  algorithm. AWARE is tested against simulations of EUV wave propagation,
  and is applied to measure EUV waves in observational data from the
  Atmospheric Imaging Assembly (AIA). We also comment on unavoidable
  systematic errors that bias the estimation of wavefront velocity and
  acceleration. In addition, the full AWARE software suite comes with a
  package that creates simulations of waves propagating across the disk
  from arbitrary starting points.

Title: The SDO/EVE Solar Irradiance Coronal Dimming Index
    Catalog. I. Methods and Algorithms
Authors: Mason, James Paul; Attie, Raphael; Arge, Charles N.; Thompson,
   Barbara; Woods, Thomas N.
Bibcode: 2019ApJS..244...13M
Altcode:
  When a coronal mass ejection departs, it leaves behind a temporary
  void. That void is known as coronal dimming, and it contains
  information about the mass ejection that caused it. Other physical
  processes can cause parts of the corona to have transient dimmings,
  but mass ejections are particularly interesting because of their
  influence in space weather. Prior work has established that dimmings
  are detectable even in disk-integrated irradiance observations, i.e.,
  Sun-as-a-star measurements. The present work evaluates four years of
  continuous Solar Dynamics Observatory Extreme Ultraviolet Experiment
  (EVE) observations to greatly expand the number of dimmings we may
  detect and characterize, and collects that information into James’s
  EVE Dimming Index catalog. This paper details the algorithms used
  to produce the catalog, provides statistics on it, and compares it
  with prior work. The catalog contains 5051 potential events (rows),
  which correspond to all robustly detected solar eruptive events in this
  time period as defined by &gt;C1 flares. Each row has a corresponding
  27,349 elements of metadata and parameterizations (columns). In total,
  this catalog is the result of analyzing 7.6 million solar ultraviolet
  light curves.

Title: Application usability levels: a framework for tracking project
    product progress
Authors: Halford, Alexa J.; Kellerman, Adam C.; Garcia-Sage, Katherine;
   Klenzing, Jeffrey; Carter, Brett A.; McGranaghan, Ryan M.; Guild,
   Timothy; Cid, Consuelo; Henney, Carl J.; Ganushkina, Natalia Yu.;
   Burrell, Angeline G.; Terkildsen, Mike; Welling, Daniel T.; Murray,
   Sophie A.; Leka, K. D.; McCollough, James P.; Thompson, Barbara J.;
   Pulkkinen, Antti; Fung, Shing F.; Bingham, Suzy; Bisi, Mario M.;
   Liemohn, Michael W.; Walsh, Brian M.; Morley, Steven K.
Bibcode: 2019JSWSC...9A..34H
Altcode: 2019arXiv190708663H
  The space physics community continues to grow and become both more
  interdisciplinary and more intertwined with commercial and government
  operations. This has created a need for a framework to easily identify
  what projects can be used for specific applications and how close
  the tool is to routine autonomous or on-demand implementation and
  operation. We propose the Application Usability Level (AUL) framework
  and publicizing AULs to help the community quantify the progress
  of successful applications, metrics, and validation efforts. This
  framework will also aid the scientific community by supplying the
  type of information needed to build off of previously published work
  and publicizing the applications and requirements needed by the user
  communities. In this paper, we define the AUL framework, outline the
  milestones required for progression to higher AULs, and provide example
  projects utilizing the AUL framework. This work has been completed
  as part of the activities of the Assessment of Understanding and
  Quantifying Progress working group which is part of the International
  Forum for Space Weather Capabilities Assessment.

Title: AWARE: An algorithm for the automated characterization of
    EUV waves in the solar atmosphere
Authors: Ireland, Jack; Inglis, Andrew; Shih, Albert Y.; Christe,
   Steven; Mumford, Stuart; Hayes, Laura A.; Thompson, Barbara J.;
   Hughitt, V. Keith
Bibcode: 2019AAS...23410707I
Altcode:
  Extreme ultraviolet (EUV) waves are large-scale propagating
  disturbances observed in the solar corona, frequently associated with
  coronal mass ejections and flares. They appear as faint, extended
  structures propagating from a source region across the structured solar
  corona. Since their discovery, over two hundred papers discussing their
  properties, causes and physical nature have been published. However,
  despite this their fundamental properties and the physics of their
  interactions with other solar phenomena are still not understood. To
  further the understanding of EUV waves, we have constructed the
  Automated Wave Analysis and REduction (AWARE) algorithm for the
  measurement of EUV waves. AWARE is implemented in two stages. In the
  first stage, we use a new type of running difference image, the running
  difference persistence image, which enables the efficient isolation
  of propagating, brightening wavefronts as they propagate across the
  corona. In the second stage, AWARE detects the presence of a wavefront,
  and measures the distance, velocity and acceleration of that wavefront
  across the Sun. The fit of propagation models to the wave progress
  isolated in the first stage is achieved using the Random Sample and
  Consensus (RANSAC) algorithm. AWARE is tested against simulations of EUV
  wave propagation, and is applied to measure EUV waves in observational
  data from the Atmospheric Imaging Assembly (AIA). We also comment on
  unavoidable systematic errors that bias the estimation of wavefront
  velocity and acceleration. In addition, the full AWARE software suite
  comes with a package that creates simulations of waves propagating
  across the disk from arbitrary starting points.

Title: Automatic Determination of Magnetosonic/Whistler Events in
    the Solar Wind
Authors: Fordin, Samuel Karl; Shay, Michael; Wilson, Lynn, III;
   Thompson, Barbara; Kirk, Michael
Bibcode: 2019shin.confE.165F
Altcode:
  23 years of observations by the WIND spacecraft has yielded a
  rich array of high-resolution magnetic field data, where a large
  fraction displays small-scale structures. In particular, the solar
  wind is full of magnetosonic-whistler-like fluctuations and kinetic
  Alfven fluctuations that appear in both the field magnitude and its
  components. Much of the previous work in the turbulence community
  has focused on kinetic Alfven waves (KAWs) and the properties of
  the associated spectral power law, with a break which occurs in the
  0.1-5.0 Hz range. This frequency range corresponds to the spacecraft
  frame frequency of magnetosonic-whistlers (MWs). Because solar wind
  heating models depend on the sources of dissipation, the ability to
  consistently distinguish between KAWs and MWs is vital to verifying
  these models. Given the breadth of magnetic field data available,
  machine learning is the most practical approach to classifying the
  myriad small-scale structures observed in the magnetic field data. To
  this end, a subset of current WIND data will be labeled and used as
  a training set for a machine learning algorithm aimed at classifying
  small-scale structures. This algorithm can then be used to catalog
  the entire WIND magnetic field dataset.

Title: Coronal Mass Ejections Observed by the Mauna Loa Solar
    Observatory Coronagraphs Associated with Solar Energetic Particle
    Events - A Progress Report
Authors: Richardson, Ian G.; St. Cyr, O. C.; Thompson, B. J.;
   Burkpile, J.
Bibcode: 2019shin.confE..26R
Altcode:
  Studies using spacebased coronagraph measurements of the middle
  corona indicate that CME dynamics provide information about the
  characteristics of the resulting SEP event. For example, the peak
  SEP intensity at a given location in space is dependent on the CME
  speed and direction [e.g., Kahler, 2001; Richardson et al., 2014,
  2018] and is also correlated with the CME brightness [Kahler &amp;
  Vourlidas, 2005]. Furthermore, the SEP spectral hardness appears to
  be related to the initial CME acceleration [Gopalswamy et al., 2015,
  2017], but this conclusion is based on proxies for the acceleration
  below the field of view of spacebased coronagraphs. Combining spacebased
  coronagraph observations with groundbased observations of the low corona
  would eliminate the need for such proxies and allow CME formation
  and the initial acceleration to be observed directly. This paper is
  a progress report on a study of SEPs associated with CMEs detected
  since 1980 by coronameters at the Mauna Loa Solar Observatory (MLSO)
  that can measure directly the formation and initial accelerations
  of CMEs low in the corona (i.e., &lt; 2 Rs). The MLSO observations
  of the initial CME signatures are combined with observations from
  spacebased coronagraphs. We then compare the CME characteristics
  with the properties of the related SEPs observed by spacecraft near
  Earth and elsewhere in the heliosphere. In particular, we have now
  identified all of the 1980-1996 MLSO CMEs with associated SEPs observed
  for example by the IMP 8, ISEE-3 and Helios spacecraft, and summarize
  their properties. We also note some of the challenges in associating
  CMEs with SEPs and solar events in the pre-SOHO/WIND/ACE era.

Title: The Whole Heliosphere and Planetary Interactions (WHPI)
    Initiative
Authors: Kolinski, Don; Gibson, Sarah; Thompson, Barbara; Bagenal,
   Fran; de Toma, Giuliana; McGranaghan, Ryan; DiBraccio, Gina
Bibcode: 2019shin.confE.108K
Altcode:
  The Whole Heliosphere and Planetary Interactions (WHPI) is a scientific
  initiative with hundreds of participants worldwide to coordinate
  observations and modeling of the solar-heliospheric-planetary system
  during solar minimum and to promote and facilitate inter-disciplinary
  activities. We do this by organizing observing campaigns and dedicated
  science workshops to bring scientists from different scientific fields
  together. The aim of WHPI is to better understand how the Sun’s output
  affects the heliosphere and planets. The simpler magnetic configuration
  of the Sun and the infrequency of CMEs make solar minimum an ideal
  time to make such connection. Science objectives of WHPI include:
  characterizing the 3D magnetic structure of the Sun and heliosphere
  during the current minimum, following the propagation and evolution of
  the Sun’s magnetic field through the solar wind and its interaction
  with the magnetospheres of the Earth and other planets, quantifying
  the effects of the solar radiative output the Earth and other planets,
  and investigating the effect of a deep and prolonged solar minimum on
  the entire heliosphere. With this poster, we invite the SHINE community
  to join the WHPI initiative.

Title: VizieR Online Data Catalog: Precision cluster abund. for
    APOGEE using SDSS DR14 (Donor+, 2018)
Authors: Donor, J.; Frinchaboy, P. M.; Cunha, K.; Thompson, B.;
   O'Connell, J.; Zasowski, G.; Jackson, K. M.; McGrath, B. M.; Almeida,
   A.; Bizyaev, D.; Carrera, R.; Garcia-Hernandez, D. A.; Nitschelm,
   C.; Pan, K.; Zamora, O.
Bibcode: 2019yCat..51560142D
Altcode:
  The primary spectroscopic data for OCCAM comes from the APOGEE
  (Majewski et al. 2017AJ....154...94M), which is part of the
  Sloan Digital Sky Survey-III and IV surveys (SDSS; Eisenstein et
  al. 2011AJ....142...72E; Blanton et al. 2017AJ....154...28B), utilizing
  the 2.5 m Sloan Foundation telescope (Gunn et al. 2006AJ....131.2332G)
  at Apache Point Observatory. APOGEE is a near-infrared (1.514-1.696
  μm) spectroscopic survey, primarily focusing on the Galactic disk
  (Zasowski et al. 2013AJ....146...81Z, 2017AJ....154..198Z). The survey
  uses multi-fiber spectrographs (Wilson et al. 2012SPIE.8446E..0HW),
  allowing for simultaneous observations of 300 stars. The targets
  selected for analysis were observed from 2011 August to 2014 July
  (APOGEE-1), and from 2014 July to 2016 July (APOGEE-2). These data were
  released as part of the 14th Data Release of SDSS (DR14; Abolfathi et
  al. 2018ApJS..235...42A), which included APOGEE data for over 250000
  stars. For this study, we analyzed all stars within 2x the cluster
  radius (Kharchenko et al. 2013, J/A+A/558/A53) for 19 clusters that
  resulted in a sample of 1361 stars. <P />(5 data files).

Title: Irradiance Coronal Dimming and its Connection to CME Kinetics
Authors: Mason, James Paul; Arge, Nick; Krista, Larisza; Reinard,
   Alysha; Thompson, Barbara J.; Webb, David F.; Wilson, Jake; Woods,
   Thomas N.
Bibcode: 2018csc..confE..86M
Altcode:
  When coronal mass ejections (CMEs) depart the corona, they leave
  behind a transient void. Such a region evacuated of plasma is known
  as a coronal dimming and it contains information about the kinetics
  of the CME that produced it. The dimming can be so great in the
  extreme ultraviolet (EUV) that it reduces the overall energy output
  of the sun in particular emission lines, i.e., dimming is observable
  in spectral irradiance. We use the Solar Dynamics Observatory (SDO)
  EUV Variability Experiment (EVE) data to search for and parameterize
  dimming. We focus our search on the 39 extracted emission lines data
  product. We are searching these light curves for dimming around all
  of the &gt;8,500 ≥C1 solar flares in the SDO era. Our method of
  combining these 39 light curves to remove the flare peak results in
  1,521 light curves for every solar flare. Thus, we come to a total of
  13 million light curves in which to search for dimming. The question
  is: which ones are sensitive to CME-induced dimming? To answer this
  and related questions, I'm using machine learning techniques built
  into python's scikit-learn library. I will describe the results of
  applying these techniques to the EVE data to produce the catalog,
  to the catalog itself, and to comparisons with other related
  catalogs. All of the code is open source python available on GitHub
  (https://github.com/jmason86/James-s-EVE-Dimming-Index-JEDI).

Title: Dynamic Mapping of Solar Eruptions
Authors: Thompson, Barbara J.; DeVore, C. Richard; Hovis-Afflerbach,
   Beryl A. C.; Uritsky, Vadim
Bibcode: 2018csc..confE..11T
Altcode:
  We present the results of a prominence mapping effort designed to
  extract the dynamics of erupting prominences and CMEs. The material from
  partially erupting prominences can fall back to the sun, tracing out the
  topology of the mid- and post-eruptive corona. One question involving
  the range of observed behavior is the role of magnetic field topology
  and evolution in determining the motion of the erupting prominence
  material. A variable-g ballistic approximation is applied to study
  the motion of the material, using the deviations from constant angular
  momentum as a means of quantifying the local Lorentz (and other) forces
  on each piece of material. Variations in dynamic behavior can be traced
  back to changes in the local magnetic field. We discuss the use of the
  prominence trajectories as a means of diagnosing eruptive topologies.

Title: Precursors of magnetic flux emergence in the moat flows of
    active region AR12673
Authors: Attie, Raphael; Kirk, Michael; Thompson, Barbara; Muglach,
   Karin; Norton, Aimee
Bibcode: 2018csc..confE..34A
Altcode:
  We report on observations of magnetic disturbances in active region
  AR12673 between Sep. 1 and Sep. 3, 2017 seen as a disruption of the moat
  flow several hours before the onset of strong flux emergence near the
  main sunspot. The moat flow is commonly known as a radially oriented
  strong outflow of photospheric plasma surrounding sunspots which ends
  abruptly and thus shapes an annular pattern around the penumbra. Using
  highly accurate methods of tracking this photospheric flow applied
  to SDO/HMI data, we are able to describe the evolution of the moat
  surrounding the main sunspot of AR 12673. We find that several hours
  before the emergence of strong magnetic flux near the main sunspot the
  moat boundaries are broken at these very same locations. This behavior
  is observed both on Sep. 1st and Sep. 3rd. There is no such behavior
  observed in the absence of flux emergence. These observational results
  pose the question of how often they occur in other active regions and
  whether the disruption of the moat flow might be, like in this case,
  an indication of impending enhanced magnetic activity or simply a
  coincidental event.

Title: Driving Scientific Discovery with Machine Learning and AI at
    the NASA GSFC Center for HelioAnalytics
Authors: Thompson, Barbara J.; Kirk, Michael S.; Sarantos, Menelaos
Bibcode: 2018csc..confE..81T
Altcode:
  What is HelioAnalytics? This is a broad term meant to cover all the
  ways that we harness advanced statistics, informatics and computer
  science methods to achieve our science. Our focus is on problems that
  we can attack with modern methods that we cannot attack otherwise. A
  keener understanding of how information is derived from data, and how
  machine learning can be harnessed to accomplish this, will expand
  the discovery potential for key heliophysics research topics and
  missions. We report on a new program to integrate modern information
  science, statistics, and scientific knowledge to advance the fundamental
  physics of connected sun-heliosphere-geospace system. The Center for
  HelioAnalytics is an "expert group" at NASA GSFC focusing on topics
  such as machine learning, neural networks, and data analytics in order
  to expand the discovery potential for key heliophysics research topics
  and missions. We define "HelioAnalytics" as a hybrid of Heliophysics
  + Machine Learning + Statistics + Information Design. Each of these
  are fields that are well developed in their own right; HelioAnalytics
  is the cross-disciplinary convergence of communities of physicists,
  statisticians, and computer scientists. HelioAnalytics is intended to
  foster research into advanced methodologies for heliophysical research,
  and to promulgate such methods into the broader community.

Title: Extracting Solar Physics from 151 Million EUV Images
Authors: Kirk, Michael S.; Thompson, Barbara; Attie, Raphael;
   Viall-Kepko, Nicki; Young, Peter
Bibcode: 2018csc..confE..88K
Altcode:
  Beginning in 2010, the Solar Dynamics Observatory's Atmospheric Imaging
  Assembly (SDO AIA) revolutionized solar imaging with its high temporal
  and spatial resolution and coverage. The archive of extreme ultraviolet
  (EUV) images is now over 150 million and continues to grow. Automated
  algorithms consistently clean these images to remove magnetospheric
  particle impacts on the CCD cameras, but it has been found that compact,
  intense solar brightenings are often removed as well. There are now over
  3 trillion "spiked pixels" that have been removed from EUV images. We
  estimate that 0.001% of those are of solar origin and removed by mistake
  - an unexplored dataset of about 30 million events. We take a novel
  approach and survey the entire set of AIA "spike" data to identify and
  group compact brightenings across the entire SDO mission. We then use
  the spike database to form statistics on compact solar brightenings
  without having to process large volumes of full-disk AIA data. The
  qualities of the "spikes" with a solar origin represent the most
  complete archive of compact EUV bright points ever assembled.

Title: AWARE: An algorithm for the automated characterization of
    EUV waves in the solar atmosphere
Authors: Ireland, Jack; Inglis, Andrew; Shih, Albert; Christe, Steven;
   Mumford, Stuart; Hayes, Laura; Thompson, Barbara; Hughitt, Keith
Bibcode: 2018csc..confE..21I
Altcode:
  Extreme ultraviolet (EUV) waves are large-scale propagating
  disturbances observed in the solar corona, frequently associated with
  coronal mass ejections and flares. They appear as faint, extended
  structures propagating from a source region across the structured solar
  corona. Since their discovery, over two hundred papers discussing their
  properties, causes and physical nature have been published. However,
  despite this their fundamental properties and the physics of their
  interactions with other solar phenomena are still not understood. To
  further the understanding of EUV waves, we have constructed the
  Automated Wave Analysis and REduction (AWARE) algorithm for the
  measurement of EUV waves. AWARE is implemented in two stages. In the
  first stage, we use a new type of running difference image, the running
  difference persistence image, which enables the efficient isolation
  of propagating, brightening wavefronts as they propagate across the
  corona. In the second stage, AWARE detects the presence of a wavefront,
  and measures the distance, velocity and acceleration of that wavefront
  across the Sun. The fit of propagation models to the wave progress
  isolated in the first stage is achieved using the Random Sample and
  Consensus (RANSAC) algorithm. AWARE is tested against simulations of EUV
  wave propagation, and is applied to measure EUV waves in observational
  data from the Atmospheric Imaging Assembly (AIA). We also comment on
  unavoidable systematic errors that bias the estimation of wavefront
  velocity and acceleration. In addition, the full AWARE software suite
  comes with a package that creates simulations of waves propagating
  across the disk from arbitrary starting points.

Title: Tracing the Origins of the Solar Wind by Tracking Flows and
    Disturbances in Coronagraph Data
Authors: Thompson, Barbara J.; Attie, Raphael; DeForest, Craig E.;
   Gibson, Sarah E.; Hess Webber, Shea A.; Ireland, Jack; Kirk, Michael
   S. F.; Kwon, Ryun Young; McGranaghan, Ryan; Viall, Nicholeen M.
Bibcode: 2018shin.confE..47T
Altcode:
  The challenge of identifying transient motions in solar imagery has
  been addressed in a number of ways. A variety of methods have been
  developed to detect and characterize the motion and extent of coronal
  mass ejections, for example. We discuss the adaptation of CME and
  solar transient detection methods to trace smaller-scale perturbations
  consistent with solar wind motions in the inner heliosphere (out to 10
  RSun). We evaluate several methods, and compare the speed and structure
  results to model predictions. In particular, we discuss how high-cadence
  heliospheric imagery can be used to track small scale solar density
  variations throughout the solar wind, serving as a proxy for in situ
  velocity detection, but with global and continuous coverage.

Title: A Framework for Tracking Progress Towards Usability:
    Application Usability Levels.
Authors: Halford, Alexa; Thompson, Barbara; Kellerman, Adam; Pulkkinen,
   Antti; Garcia-Sage, Katherine
Bibcode: 2018cosp...42E1353H
Altcode:
  As our community continues to grow and become more intertwined with
  industry and other fields, there is a need for a framework that can
  allow researchers and end users to identify applications for the
  research, quantify metrics for each specific application, and enable
  communication between the researchers and end users. To this end, the
  Assessment of Understanding and Quantifying Progress International
  Forum for Space Weather Capabilities Assessment working group has
  developed the Application Usability Level (AUL) framework. The
  AUL framework was developed by implementing lessons learned from
  Technology Readiness Levels (TRLs) used by the instrument community
  and Application Readiness Levels (ARLs) used by the Applied Science
  program in NASA's Earth Science Division, as well as modifying the
  levels and their milestones to better suit the needs of the Space
  Weather and Heliophysics communities. In this talk we will introduce
  the AUL framework and show examples of how it can be applied to
  research for the Space Weather and Heliophysics communities. For more
  information on the AULs and other work being done by the Assessment of
  Understanding and Quantifying Progress International Forum for Space
  Weather Capabilities Assessment working group, please see our website at
  the CCMC https://ccmc.gsfc.nasa.gov/assessment/topics/trackprogress.php

Title: Prediction of Solar Energetic Particle Peak Intensity using
    CME Speed and Direction in Solar Cycles 24 and 23
Authors: Richardson, Ian; Mays, Leila M.; Thompson, Barbara J.
Bibcode: 2018shin.confE.104R
Altcode:
  We assess whether a formula obtained by Richardson et al. (2014)
  (Solar Phys., 289, 3059, DOI 10.1007/s11207-014-0524-8) relating the
  peak intensity of 14-24 MeV protons in a solar energetic particle event
  at 1 AU to the solar event location and the speed of the associated
  coronal mass ejection (CME), may be used to “predict" the intensity of
  a solar energetic particle event. Starting with a set of all 334 CMEs in
  the CCMC/SWRC DONKI real-time database during October, 2011-July 2012,
  selected without consideration of whether they were associated with
  SEP events, we use the CME speed and direction to predict the proton
  intensity at Earth or the STEREO spacecraft using this formula. Since
  most ( 85%) of these CMEs were not associated with SEP events, many
  “false alarms" result. We demonstrate that considering the type
  II or type III radio emissions that may accompany the CMEs can help
  to improve the forecast skill, which we assess using several skill
  scores. The method is also applied to over 1100 CMEs in solar cycle 23.

Title: 13 Million Light Curves, 122 Million Parameters, and the
    Connection to Coronal Mass Ejections
Authors: Mason, James; Thompson, Barbara; Woods, Thomas; Webb, David;
   Arge, Charles
Bibcode: 2018cosp...42E2194M
Altcode:
  When coronal mass ejections (CMEs) depart the corona, they leave
  behind a transient void. Such a region evacuated of plasma is known as
  a coronal dimming and it contains information about the kinetics of
  the CME that produced it. The dimming can be so great in the extreme
  ultraviolet (EUV) that it reduces the overall energy output of the
  sun in particular emission lines, i.e., dimming is observable in
  spectral irradiance. This should be generally true for magnetically
  active stars. The Solar Dynamics Observatory (SDO) EUV Variability
  Experiment (EVE) data provide an excellent opportunity to search for and
  parameterize dimming. We focus our search on the 39 extracted emission
  lines data product. We search these light curves for dimming around
  all of the &gt;8,500 ≥C1 solar flares observed by the Geostationary
  Operational Environmental Satellite (GOES) X-ray Sensor (XRS) in the
  SDO era. In prior work, we have found that it is important to remove
  the gradual flare phase from dimming light curves in order to obtain
  slopes and magnitudes that are consistent with what can be obtained by
  spatially isolating flaring loops in spectral image data. To do this,
  we peak-match and subtract two different emission line light curves. In
  this exhaustive search and characterization of dimming, we therefore
  consider every permutation of the 39 emission lines as well as the
  "uncorrected" light curves, resulting in 1,521 light curves for every
  ≥C1 solar flare. Thus, we come to a total of 13 million light curves
  in which to search for dimming. We parameterize each light curve in
  terms of magnitude, slope, and duration and correlate these with CME
  speed and mass. Thus, we obtain a robust relationship between irradiance
  coronal dimming and CME kinetics.Here, we briefly describe the feature
  detection and characterization algorithms developed and applied to the
  13 million EUV irradiance light curves. Machine learning techniques
  have been used for both this backend processing pipeline and to analyze
  the results. All of the code is open source python available on GitHub
  (https://github.com/jmason86/James-s-EVE-Dimming-Index-JEDI). We then
  provide preliminary results on the comparison between our new catalog
  and the established Coordinated Data Analysis Workshops' CME Catalog.

Title: Advance detection of strong photospheric flux emergence
    revealed by disruption of moat flows
Authors: Attié, Raphael; Thompson, Barbara J.; Muglach, Karin;
   Norton, Aimee Ann
Bibcode: 2018tess.conf30602A
Altcode:
  We report on observations of precursors of magnetic disturbances in AR
  12673 seen as a disruption of the moat flow several hours before the
  onset of strong flux emergence near the main sunspot. The moat flow is
  commonly known as a radially oriented strong outflow of photospheric
  plasma surrounding sunspots which ends abruptly and thus shapes an
  annular pattern around the penumbra. Using highly accurate methods of
  tracking this photospheric flow applied to SDO/HMI data, we are able
  to describe the evolution of the moat surrounding the main sunspot of
  AR 12673. We find that several hours before the emergence of strong
  magnetic flux near the main sunspot the moat boundaries are broken at
  these very same locations. Because we detect this specific behavior both
  on Sep. 1st and Sep. 3rd, our observations suggest that the disruption
  of the moat flow is a precursor of the enhanced magnetic activity
  which, in this case, led to the strong flaring activity starting on
  Sep 6th. This study is part of a broader statistical survey that
  aims at characterizing emerging active regions. In light of these
  new observations, our survey will also determine to what extent such
  a disruption of the moat flow is followed by strong flux emergence
  around sunspots, i.e., is this a peculiar response specific to AR
  12673, or is it a characteristic disturbance defining a subset of
  active regions prone to flaring activity?

Title: Tracking Flows and Disturbances in Coronagraph Data
Authors: Thompson, Barbara J.; Attie, Raphael; DeForest, Craig E.;
   Gibson, Sarah E.; Hess Webber, Shea A.; Inglis, Anfew R.; Ireland,
   Jack; Kirk, Michael S.; Kwon, RyunYoung; Viall, Nicholeen M.
Bibcode: 2018tess.conf30922T
Altcode:
  The challenge of identifying transient motions in solar imagery has
  been addressed in a number of ways. A variety of methods have been
  developed to detect and characterize the motion and extent of coronal
  mass ejections, for example. We discuss the adaptation of CME and
  solar transient detection methods to trace smaller-scale perturbations
  consistent with solar wind motions in the inner heliosphere (over 10
  RSun). We evaluate several methods, and compare the speed and structure
  results to model predictions. In particular, we discuss how high-cadence
  heliospheric imagery can be used to track small scale solar density
  variations throughout the solar wind, serving as a proxy for in situ
  velocity detection, but with global and continuous coverage.

Title: Observations of \sim25 MeV Energetic Particle Events Made by
    the High Energy Telescopes During the STEREO Mission
Authors: Richardson, Ian G.; von Rosenvinge, Tycho T.; Cane, Hilary
   V.; Thompson, Barbara J.; Kwon, RyunYoung
Bibcode: 2018tess.conf21367R
Altcode:
  We summarize some of the results from the High Energy Telescopes (HETs)
  on the STEREO spacecraft which made observations of 0.7-4 MeV electrons
  and 13.6-100 MeV protons since the beginning of the mission in late
  2006, including the detection of over 300 solar energetic particle
  events that included 25 MeV protons, of which around 40 were observed
  at both STEREO spacecraft and at the Earth. We also show observations
  during the most recent events in September-October, 2017, and consider
  the lessons learned from the STEREO HET observations.

Title: Tracking algorithms and machine learning for the
    characterization of active regions over the solar cycle 24
Authors: Attié, Raphael; Thompson, Barbara J.; Kirk, Mechael S.;
   Norton, Aimee Ann
Bibcode: 2018tess.conf31604A
Altcode:
  Since the year 2010, SDO is sending more than a terabyte of solar
  observations per day. <P />By offering such an unprecedented large
  and varied data sets, this mission has propelled the solar physics
  community into the era of "Big Data" analytics. As an answer to this
  new technical and scientific challenge, we present here a threefold
  innovative framework for efficient data mining and analysis of the solar
  photosphere using SDO/HMI: <P />(i) A method for tracking the horizontal
  photospheric flows uses an improved version of "Balltracking". We will
  present the most recent version of this feature tracking algorithm,
  its advantage over other more traditional methods like Local
  Correlation Tracking (LCT) and how it has been specifically tuned
  to handle the massive HMI datastream. Coupled with flow segmentation
  algorithms, it offers an unprecedented view of the evolution of the
  supergranulation. <P />(ii) A method for tracking the magnetic flux
  using HMI data called "Magnetic Balltracking". We will show how it
  enables us to accurately track magnetic elements on magnetograms in
  the Lagrange reference frame, and systematically derive parameters
  such as the position, velocity, and fragments area and how we use
  it to automate the detection of flux emergence. <P />(iii) The above
  methods define a tracking framework whose output feed databases that
  become the input of machine learning algorithms for classification
  purposes. We will show how this expands our knowledge-base e.g. on
  the properties of large-scale photospheric flows prior to and after
  the emergence of active regions, and on how the flows interact with
  the magnetic field over large areas and long time scales. <P />Through
  these examples we will demonstrate how this framework contributes to
  a sensible characterization of the evolution of active regions during
  the whole solar cycle.

Title: Correlating Flare Oscillations with Photospheric Wave Responses
Authors: Hess Webber, Shea A.; Thompson, Barbara J.; Zhao, Junwei
Bibcode: 2018tess.conf30493H
Altcode:
  Applying the Time-Convolution Mapping Method (TCMM) to multiple SDO/AIA
  wavelengths, we track plasma oscillations in the chromosphere and low
  corona during several X-class flares. These results will be used to
  determine travel times for the oscillations along the flare loops. The
  ultimate goal is to correlate these travel times with photospheric wave
  responses. Understanding how flare oscillations effect the photosphere
  can detail the mechanics and solar environment around flaring active
  regions.

Title: Prediction of Solar Energetic Particle Peak Intensity using
    CME Speed and Direction in Solar Cycle 24 and Earlier Cycles
Authors: Richardson, Ian G.; Mays, M. Leila; Thompson, Barbara J.
Bibcode: 2018tess.conf21369R
Altcode:
  From a survey of solar energetic particle events observed by both the
  STEREO spacecraft and at the Earth in 2009-2012 during solar cycle 24,
  Richardson et al. (Solar Physics, 289,3059, 2014) obtained a formula
  relating the SEP peak intensity at 14-24 MeV with the speed of the
  associated coronal mass ejection and its direction with respect to the
  observing spacecraft. This suggests that the formula might in turn be
  used, if the CME parameters are known, to "predict" the intensity of
  the related SEP event. However, since only a small fraction of CMEs
  are actually associated with SEPs at this energy, many "false alarms"
  occur. These may be reduced by, for example, considering a minimum CME
  width, or other phenomena, such as type II and type III radio emissions,
  accompanying the CME. For a subset of cycle 24 CMEs, in around three
  quarters of cases where the observed proton intensity at 14-24 MeV
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  &lt;/use&gt; &lt;/g&gt; &lt;/g&gt; &lt;/svg&gt;% of cases. However,
  since cycle 24 SEP events were used to generate the formula, it
  is also possible that this contributes the good agreement between
  observed and predicted SEP intensities. We have therefore applied it
  to CMEs in solar cycle 23, using CME speeds from the CDAW catalog and
  directions inferred from the location of the associated flare, and
  find that there is a similar level of agreement. For earlier cycles,
  we use CME observations from the Solwind and SMM coronagraphs associated
  with SEP events. In addition, for SEP events in earlier cycles where
  the SEP intensity and flare location are known, the speed of the
  associated CME might be estimated using the formula, assuming that it
  also holds for these earlier cycles, thereby indicating the speeds of
  SEP-associated CMEs even if there are no coronagraph observations.

Title: Correlating Flare Oscillations with Photospheric Wave Responses
Authors: Hess Webber, Shea A.; Thompson, Barbara J.; Zhao, Junwei
Bibcode: 2018ress.meetE...1H
Altcode:
  Applying the Time-Convolution Mapping Method (TCMM) to multiple SDO/AIA
  wavelengths, we track plasma oscillations in the chromosphere and low
  corona during several X-class flares. These results will be used to
  determine travel times for the oscillations along the flare loops. The
  ultimate goal is to correlate these travel times with photospheric wave
  responses. Understanding how flare oscillations effect the photosphere
  can detail the mechanics and solar environment around flaring active
  regions.

Title: Space Weather Research and Forecasting Capabilities at the
    Community Coordinated Modeling Center (CCMC)
Authors: Collado-Vega, Y. M.; Kuznetsova, M.; Mays, L.; Pulkkinen,
   A.; Zheng, Y.; Muglach, K.; Thompson, B.; Chulaki, A.; Taktakishvili,
   A.; CCMC Team
Bibcode: 2018LPICo2063.3090C
Altcode:
  The Community Coordinated Modeling Center (CCMC) supports and enables
  the research and development of the latest and future space weather
  models and facilitates the deployment of the latest advances in research
  of space weather operations.

Title: Physical Conditions in the Solar Corona Derived from the
    Total Solar Eclipse Observations obtained on 2017 August 21 Using
    a Polarization Camera
Authors: Gopalswamy, N.; Yashiro, Seiji; Reginald, Nelson; Thakur,
   Neeharika; Thompson, Barbara J.; Gong, Qian
Bibcode: 2018AAS...23122008G
Altcode:
  We present preliminary results obtained by observing the solar corona
  during the 2017 August 21 total solar eclipse using a polarization
  camera mounted on an eight-inch Schmidt-Cassegrain telescope. The
  observations were made from Madras Oregon during 17:19 to 17:21
  UT. Total and polarized brightness images were obtained at four
  wavelengths (385, 398.5, 410, and 423 nm). The polarization camera had a
  polarization mask mounted on a 2048x2048 pixel CCD with a pixel size of
  7.4 microns. The resulting images had a size of 975x975 pixels because
  four neighboring pixels were summed to yield the polarization and total
  brightness images. The ratio of 410 and 385 nm images is a measure
  of the coronal temperature, while that at 423 and 398.5 nm images
  is a measure of the coronal flow speed. We compared the temperature
  map from the eclipse observations with that obtained from the Solar
  Dynamics Observatory’s Atmospheric Imaging Assembly images at six EUV
  wavelengths, yielding consistent temperature information of the corona.

Title: Studying the Kinematic Behavior of Coronal Mass Ejections
    and Other Solar Phenomena using the Time-Convolution Mapping Method
Authors: Hess Webber, Shea A.; Thompson, Barbara J.; Kwon, Ryun Young;
   Ireland, Jack
Bibcode: 2018AAS...23131504H
Altcode:
  An improved understanding of the kinematic properties of CMEs and
  CME-associated phenomena has several impacts: 1) a less ambiguous
  method of mapping propagating structures into their inner coronal
  manifestations, 2) a clearer view of the relationship between the
  “main” CME and CME-associated brightenings, and 3) an improved
  identification of the heliospheric sources of shocks, Type II
  bursts, and SEPs. We present the results of a mapping technique that
  facilitates the separation of CMEs and CME-associated brightenings
  (such as shocks) from background corona. The Time Convolution Mapping
  Method (TCMM) segments coronagraph data to identify the time history
  of coronal evolution, the advantage being that the spatiotemporal
  evolution profiles allow users to separate features with different
  propagation characteristics. For example, separating “main”
  CME mass from CME-associated brightenings or shocks is a well-known
  obstacle, which the TCMM aids in differentiating. A TCMM CME map is
  made by first recording the maximum value each individual pixel in
  the image reaches during the traversal of the CME. Then the maximum
  value is convolved with an index to indicate the time that the pixel
  reached that value. The TCMM user is then able to identify continuous
  “kinematic profiles,” indicating related kinematic behavior, and
  also identify breaks in the profiles that indicate a discontinuity in
  kinematic history (i.e. different structures or different propagation
  characteristics). The maps obtained from multiple spacecraft viewpoints
  (i.e., STEREO and SOHO) can then be fit with advanced structural models
  to obtain the 3D properties of the evolving phenomena. We will also
  comment on the TCMM's further applicability toward the tracking of
  prominences, coronal hole boundaries and coronal cavities.

Title: Tracking Photospheric Energy Transport in Active Regions
    with SDO
Authors: Attié, R.; Thompson, B. J.
Bibcode: 2017AGUFMSH13A2470A
Altcode:
  The solar photosphere presents flow fields at all observable
  scales. Where energy-bearing magnetic active regions break through
  the photosphere these flows are particularly strong, as sheared and
  twisted magnetic fields come into equilibrium with their surroundings
  while transporting magnetic energy into the corona. A part of this
  magnetic energy - the so-called `free energy' stored in the magnetic
  field in the form of "twisted" and shear of the field - is released in
  flares and eruptions. We can quantify the energy arrival and build-up
  in the corona by tracking flow fields and magnetic features at the
  photosphere as magnetic flux emerges and evolves before and after
  a flare or eruption.To do this reliably requires two things: a long
  series of photospheric observations at high sensitivity, spatial and
  temporal resolution, and an efficient, reliable and robust framework
  that tracks the photospheric plasma flows and magnetic evolution in both
  the quiet sun and active regions. SDO/HMI provides the observations, and
  we present here an innovative high resolution tracking framework that
  involves the `Balltracking' and `Magnetic Balltracking' algorithms. We
  show the first results of a systematic, quantitative and comprehensive
  measurements of the flows and transport of magnetic energy into the
  solar atmosphere and investigate whether this dynamic view can improve
  predictions of flares and Coronal Mass Ejections (CMEs).

Title: Prediction of SEP Peak Proton Intensity Based on CME Speed,
    Direction and Observations of Associated Solar Phenomena
Authors: Richardson, I. G.; Mays, M. L.; Thompson, B. J.; Kwon, R.;
   Frechette, B. P.
Bibcode: 2017AGUFMSH31B2735R
Altcode:
  We assess whether a formula obtained by Richardson et al. (Solar
  Phys., 289, 3059, 2014; DOI 10.1007/s11207-014-0524-8) relating the
  intensity of 14-24 MeV protons in a solar energetic particle event
  at 1 AU to the solar event location and the speed of the associated
  coronal mass ejection (CME), may be used to "predict" the intensity
  of a solar energetic particle event. Starting with a subset of
  several hundred CMEs in the CCMC/SWRC DONKI real-time database
  (http://kauai.ccmc.gsfc.nasa.gov/DONKI/) selected without consideration
  of whether they were associated with SEP events, we first use the CME
  speed and direction to predict the proton intensity at Earth or the
  STEREO spacecraft using this formula. Since most of these CMEs were
  not in fact associated with SEP events, many "false alarms" result. We
  then examine whether considering other phenomena which may accompany
  the CMEs, such as the X-ray flare intensity and the properties of type
  II and type III radio emissions, may help to reduce the false alarm
  rate. We also use CME parameters calculated from an ellipsoidal shell
  fit to multi-spacecraft CME shock observations for a smaller number
  of events to predict the SEP intensity. We calculate skill scores for
  each case and assess whether the Richardson et al. (2014) formula,
  using additional observations to reduce the false alarm rate, has
  any potential as a SEP prediction tool, assuming that the required
  observations could be acquired sufficiently rapidly following the
  onset of the related solar event/CME.

Title: Deriving and Constraining 3D CME Kinematic Parameters from
    Multi-Viewpoint Coronagraph Images
Authors: Thompson, B. J.; Mei, H. F.; Barnes, D.; Colaninno, R. C.;
   Kwon, R.; Mays, M. L.; Mierla, M.; Moestl, C.; Richardson, I. G.;
   Verbeke, C.
Bibcode: 2017AGUFMSH31A2714T
Altcode:
  Determining the 3D properties of a coronal mass ejection using
  multi-viewpoint coronagraph observations can be a tremendously
  complicated process. There are many factors that inhibit the
  ability to unambiguously identify the speed, direction and shape
  of a CME. These factors include the need to separate the "true"
  CME mass from shock-associated brightenings, distinguish between
  non-radial or deflected trajectories, and identify asymmetric CME
  structures. Additionally, different measurement methods can produce
  different results, sometimes with great variations. Part of the reason
  for the wide range of values that can be reported for a single CME
  is due to the difficulty in determining the CME's longitude since
  uncertainty in the angle of the CME relative to the observing image
  planes results in errors in the speed and topology of the CME. Often
  the errors quoted in an individual study are remarkably small when
  compared to the range of values that are reported by different authors
  for the same CME. For example, two authors may report speeds of 700
  +- 50 km/sec and 500+-50 km/sec for the same CME. Clearly a better
  understanding of the accuracy of CME measurements, and an improved
  assessment of the limitations of the different methods, would be
  of benefit. We report on a survey of CME measurements, wherein we
  compare the values reported by different authors and catalogs. The
  survey will allow us to establish typical errors for the parameters
  that are commonly used as inputs for CME propagation models such
  as ENLIL and EUHFORIA. One way modelers handle inaccuracies in CME
  parameters is to use an ensemble of CMEs, sampled across ranges of
  latitude, longitude, speed and width. The CMEs simulated in order to
  determine the probability of a "direct hit" and, for the cases with a
  "hit," derive a range of possible arrival times. Our study will provide
  improved guidelines for generating CME ensembles that more accurately
  sample across the range of plausible values.

Title: CCMC: bringing space weather awareness to the next generation
Authors: Chulaki, A.; Muglach, K.; Zheng, Y.; Mays, M. L.; Kuznetsova,
   M. M.; Taktakishvili, A.; Collado-Vega, Y. M.; Rastaetter, L.; Mendoza,
   A. M. M.; Thompson, B. J.; Pulkkinen, A. A.; Pembroke, A. D.
Bibcode: 2017AGUFMSH21A2635C
Altcode:
  Making space weather an element of core education is critical for
  the future of the young field of space weather. Community Coordinated
  Modeling Center (CCMC) is an interagency partnership established to
  aid the transition of modern space science models into space weather
  forecasting while supporting space science research. Additionally, over
  the past ten years it has established itself as a global space science
  education resource supporting undergraduate and graduate education and
  research, and spreading space weather awareness worldwide. A unique
  combination of assets, capabilities and close ties to the scientific
  and educational communities enable our small group to serve as a hub
  for rising generations of young space scientists and engineers. CCMC
  offers a variety of educational tools and resources publicly available
  online and providing access to the largest collection of modern space
  science models developed by the international research community. CCMC
  has revolutionized the way these simulations are utilized in
  classrooms settings, student projects, and scientific labs. Every
  year, this online system serves hundreds of students, educators and
  researchers worldwide. Another major CCMC asset is an expert space
  weather prototyping team primarily serving NASA's interplanetary space
  weather needs. Capitalizing on its unique capabilities and experiences,
  the team also provides in-depth space weather training to hundreds of
  students and professionals. One training module offers undergraduates an
  opportunity to actively engage in real-time space weather monitoring,
  analysis, forecasting, tools development and research, eventually
  serving remotely as NASA space weather forecasters. In yet another
  project, CCMC is collaborating with Hayden Planetarium and Linkoping
  University on creating a visualization platform for planetariums (and
  classrooms) to provide simulations of dynamic processes in the large
  domain stretching from the solar corona to the Earth's upper atmosphere,
  for near real-time and historical space weather events.

Title: Assessing and Adapting Scientific Results for Space Weather
    Research to Operations (R2O)
Authors: Thompson, B. J.; Friedl, L.; Halford, A. J.; Mays, M. L.;
   Pulkkinen, A. A.; Singer, H. J.; Stehr, J. W.
Bibcode: 2017AGUFMSM11E..04T
Altcode:
  Why doesn't a solid scientific paper necessarily result in a tangible
  improvement in space weather capability? A well-known challenge in
  space weather forecasting is investing effort to turn the results of
  basic scientific research into operational knowledge. This process
  is commonly known as "Research to Operations," abbreviated R2O. There
  are several aspects of this process: 1) How relevant is the scientific
  result to a particular space weather process? 2) If fully utilized, how
  much will that result improve the reliability of the forecast for the
  associated process? 3) How much effort will this transition require? Is
  it already in a relatively usable form, or will it require a great deal
  of adaptation? 4) How much burden will be placed on forecasters? Is
  it "plug-and-play" or will it require effort to operate? 5) How
  can robust space weather forecasting identify challenges for new
  research? This presentation will cover several approaches that have
  potential utility in assessing scientific results for use in space
  weather research. The demonstration of utility is the first step,
  relating to the establishment of metrics to ensure that there will be
  a clear benefit to the end user. The presentation will then move to
  means of determining cost vs. benefit, (where cost involves the full
  effort required to transition the science to forecasting, and benefit
  concerns the improvement of forecast reliability), and conclude with a
  discussion of the role of end users and forecasters in driving further
  innovation via "O2R."

Title: The Far Ultra-Violet Imager on the Icon Mission
Authors: Mende, S. B.; Frey, H. U.; Rider, K.; Chou, C.; Harris,
   S. E.; Siegmund, O. H. W.; England, S. L.; Wilkins, C.; Craig, W.;
   Immel, T. J.; Turin, P.; Darling, N.; Loicq, J.; Blain, P.; Syrstad,
   E.; Thompson, B.; Burt, R.; Champagne, J.; Sevilla, P.; Ellis, S.
Bibcode: 2017SSRv..212..655M
Altcode: 2017SSRv..tmp...77M
  ICON Far UltraViolet (FUV) imager contributes to the ICON science
  objectives by providing remote sensing measurements of the daytime and
  nighttime atmosphere/ionosphere. During sunlit atmospheric conditions,
  ICON FUV images the limb altitude profile in the shortwave (SW)
  band at 135.6 nm and the longwave (LW) band at 157 nm perpendicular
  to the satellite motion to retrieve the atmospheric O/N<SUB>2</SUB>
  ratio. In conditions of atmospheric darkness, ICON FUV measures the
  135.6 nm recombination emission of O<SUP>+</SUP> ions used to compute
  the nighttime ionospheric altitude distribution. ICON Far UltraViolet
  (FUV) imager is a Czerny-Turner design Spectrographic Imager with
  two exit slits and corresponding back imager cameras that produce two
  independent images in separate wavelength bands on two detectors. All
  observations will be processed as limb altitude profiles. In addition,
  the ionospheric 135.6 nm data will be processed as longitude and
  latitude spatial maps to obtain images of ion distributions around
  regions of equatorial spread F. The ICON FUV optic axis is pointed 20
  degrees below local horizontal and has a steering mirror that allows
  the field of view to be steered up to 30 degrees forward and aft, to
  keep the local magnetic meridian in the field of view. The detectors
  are micro channel plate (MCP) intensified FUV tubes with the phosphor
  fiber-optically coupled to Charge Coupled Devices (CCDs). The dual
  stack MCP-s amplify the photoelectron signals to overcome the CCD
  noise and the rapidly scanned frames are co-added to digitally create
  12-second integrated images. Digital on-board signal processing is
  used to compensate for geometric distortion and satellite motion and
  to achieve data compression. The instrument was originally aligned in
  visible light by using a special grating and visible cameras. Final
  alignment, functional and environmental testing and calibration were
  performed in a large vacuum chamber with a UV source. The test and
  calibration program showed that ICON FUV meets its design requirements
  and is ready to be launched on the ICON spacecraft.

Title: Improving Our Understanding of the 3D Coronal Evolution of
    CME Propagation
Authors: Hess Webber, Shea A.; Thompson, Barbara J.; Ireland, Jack;
   Kwon, Ryun Young
Bibcode: 2017SPD....4820603H
Altcode:
  An improved understanding of the kinematic properties of CMEs and
  CME-associated phenomena has several impacts: 1) a less ambiguous
  method of mapping propagating structures into their inner coronal
  manifestations, 2) a clearer view of the relationship between the
  “main” CME and CME-associated brightenings, and 3) an improved
  identification of the heliospheric sources of shocks, Type II
  bursts, and SEPs. We present the results of a mapping technique that
  facilitates the separation of CMEs and CME-associated brightenings
  (such as shocks) from background corona. The Time Convolution Mapping
  Method (TCMM) segments coronagraph data to identify the time history
  of coronal evolution, the advantage being that the spatiotemporal
  evolution profiles allow users to separate features with different
  propagation characteristics. For example, separating “main”
  CME mass from CME-associated brightenings or shocks is a well-known
  obstacle, which the TCMM aids in differentiating. A TCMM CME map is
  made by first recording the maximum value each individual pixel in
  the image reaches during the traversal of the CME. Then the maximum
  value is convolved with an index to indicate the time that the pixel
  reached that value. The TCMM user is then able to identify continuous
  “kinematic profiles,” indicating related kinematic behavior, and
  also identify breaks in the profiles that indicate a discontinuity in
  kinematic history (i.e. different structures or different propagation
  characteristics). The maps obtained from multiple spacecraft viewpoints
  (i.e., STEREO and SOHO) can then be fit with advanced structural models
  to obtain the 3D properties of the evolving phenomena.

Title: Observations of Magnetic Evolution and Network Flares Driven
    by Photospheric Flows in the Quiet Sun
Authors: Attie, Raphael; Thompson, Barbara J.
Bibcode: 2017SPD....4810105A
Altcode:
  The quiet Sun may be the biggest laboratory to study physical elementary
  processes of fundamental importance to space plasma. The advantage
  is the continuous availability of small-scale events, carrying the
  hidden microphysics that is responsible for larger-scale phenomena. By
  small-scale events, we mean spatial dimensions of a few Mm at most,
  and durations of less than an hour. I present here an attempt to
  describe and understand the coupling between the photospheric flows,
  the photospheric magnetic flux, and small-scale energetic transient
  events. By adapting and improving the highly efficient Balltracking
  technique for Hinode/SOT data, we relate the fine structures of the
  supergranular flow fields with the magnetic flux evolution. For
  studying the dynamics of the latter, and more precisely, the
  magnetic flux cancellation at sites of energy releases, we applied
  a new feature tracking algorithm called "Magnetic Balltracking" --
  which tracks photospheric magnetic elements -- to high-resolution
  magnetograms from Hinode/SOT.Using observations of the low corona
  in soft X-rays with Hinode/XRT, we analyse the triggering mechanism
  of small-scale network flares. By tracking both the flow fields on
  the one hand, and the magnetic motions on the other hand, we relate
  the flows with cancelling magnetic flux. We identify two patterns
  of horizontal flows that act as catalysts for efficient magnetic
  reconnection: (i) Funnel-shaped streamlines in which the magnetic
  flux is carried, and (ii) large-scale vortices (~10 Mm and above)
  at the network intersections, in which distant magnetic features of
  opposite polarities seem to be sucked in and ultimately vanish. The
  excess energy stored in the stressed magnetic field of the vortices
  is sufficient to power network flares.Prospects for determining the
  magnetic energy budget in the quiet sun are discussed.

Title: Network Flares and Magnetic Evolution Driven by Photospheric
    Flows in the Quiet Sun
Authors: Attie, Raphael; Thompson, Barbara J.
Bibcode: 2017shin.confE..58A
Altcode:
  The quiet Sun may be the biggest laboratory to study physical elementary
  processes of fundamental importance to space plasma. The advantage
  is the continuous availability of small-scale events, carrying the
  hidden microphysics that is responsible for larger-scale phenomena. By
  small-scale events, we mean spatial dimensions of a few Mm at most,
  and durations of less than an hour. I present here an attempt to
  describe and understand the coupling between the photospheric flows,
  the photospheric magnetic flux, and small-scale energetic transient
  events. By adapting and improving the highly efficient Balltracking
  technique for Hinode/SOT data, we relate the fine structures of
  the supergranular flow fields with the magnetic flux evolution. For
  studying the magnetic flux cancellation at sites of energy releases,
  we applied a new feature tracking algorithm called

Title: The Solar Energetic Particle Event of 2010 August 14:
    Connectivity with the Solar Source Inferred from Multiple Spacecraft
    Observations and Modeling
Authors: Lario, D.; Kwon, R. -Y.; Richardson, I. G.; Raouafi, N. E.;
   Thompson, B. J.; von Rosenvinge, T. T.; Mays, M. L.; Mäkelä, P. A.;
   Xie, H.; Bain, H. M.; Zhang, M.; Zhao, L.; Cane, H. V.; Papaioannou,
   A.; Thakur, N.; Riley, P.
Bibcode: 2017ApJ...838...51L
Altcode:
  We analyze one of the first solar energetic particle (SEP) events
  of solar cycle 24 observed at widely separated spacecraft in order
  to assess the reliability of models currently used to determine the
  connectivity between the sources of SEPs at the Sun and spacecraft in
  the inner heliosphere. This SEP event was observed on 2010 August 14 by
  near-Earth spacecraft, STEREO-A (∼80° west of Earth) and STEREO-B
  (∼72° east of Earth). In contrast to near-Earth spacecraft, the
  footpoints of the nominal magnetic field lines connecting STEREO-A
  and STEREO-B with the Sun were separated from the region where the
  parent fast halo coronal mass ejection (CME) originated by ∼88° and
  ∼47° in longitude, respectively. We discuss the properties of the
  phenomena associated with this solar eruption. Extreme ultraviolet and
  white-light images are used to specify the extent of the associated
  CME-driven coronal shock. We then assess whether the SEPs observed
  at the three heliospheric locations were accelerated by this shock or
  whether transport mechanisms in the corona and/or interplanetary space
  provide an alternative explanation for the arrival of particles at the
  poorly connected spacecraft. A possible scenario consistent with the
  observations indicates that the observation of SEPs at STEREO-B and near
  Earth resulted from particle injection by the CME shock onto the field
  lines connecting to these spacecraft, whereas SEPs reached STEREO-A
  mostly via cross-field diffusive transport processes. The successes,
  limitations, and uncertainties of the methods used to resolve the
  connection between the acceleration sites of SEPs and the spacecraft
  are evaluated.

Title: Geosynchronous Patrol Orbit for Space Situational Awareness
Authors: Thompson, B.; Kelecy, T.; Kubancik, T.; Flora, T.; Chylla,
   M.; Rose, D.
Bibcode: 2017amos.confE..96T
Altcode:
  Applying eccentricity to a geosynchronous orbit produces
  both longitudinal and radial motion when viewed in Earth-fixed
  coordinates. An interesting family of orbits emerges, useful for
  “neighborhood patrol” space situational awareness and other
  missions. The basic result is a periodic (daily), quasielliptical,
  closed path around a fixed region of the geosynchronous (geo) orbit
  belt, keeping a sensor spacecraft in relatively close vicinity to
  designated geo objects. The motion is similar, in some regards, to the
  relative motion that may be encountered during spacecraft proximity
  operations, but on a much larger scale. The patrol orbit does not
  occupy a fixed slot in the geo belt, and the east-west motion can be
  combined with north-south motion caused by orbital inclination, leading
  to even greater versatility. Some practical uses of the geo patrol
  orbit include space surveillance (including catalog maintenance), and
  general space situational awareness. The patrol orbit offers improved,
  diverse observation geometry for angles-only sensors, resulting in
  faster, more accurate orbit determination compared to simple inclined
  geo orbits. In this paper, we analyze the requirements for putting a
  spacecraft in a patrol orbit, the unique station keeping requirements
  to compensate for perturbations, repositioning the patrol orbit to
  a different location along the geo belt, maneuvering into, around,
  and out of the volume for proximity operations with objects within
  the volume, and safe end-of-life disposal requirements.

Title: Connectivity Between Solar Energetic Particle Observations
and Their Solar Sources: The Event on 14 August 2010
Authors: Kwon, R. Y.; Makela, P. A.; Lario, D.; Raouafi, N. E.;
   Thompson, B. J.; Richardson, I. G.; von Rosenvinge, T. T.; Xie, H.;
   Mays, M. L.; Thakur, N.; Bain, H. M.; Zhang, M.; Zhao, L.; Matthaeus,
   W. H.; Papaioannou, A.; Riley, P.
Bibcode: 2016AGUFMSH41B2530K
Altcode:
  We analyze one of the first multi-spacecraft solar energetic particle
  (SEP) events of solar cycle 24 to assess the reliability of models
  currently used to determine the connectivity between the sources of SEPs
  at the Sun and spacecraft located in the inner heliosphere. This SEP
  event was observed on 14 August 2010 by near-Earth spacecraft, STEREO-A
  (at 0.96 AU from the Sun and 80° west of Earth) and STEREO-B (at 1.07
  AU and 72° east of Earth). The SEP event occurred in association with
  a C4.4 flare at N13W54 (as seen from Earth) and a fast ( 1200 km s-1)
  halo coronal mass ejection (CME). Whereas near-Earth observers were
  magnetically connected to the site of the active region, the other
  spacecraft observing SEPs remained poorly connected to the active
  region. We discuss the properties of the phenomena associated with the
  solar eruption as seen in extreme ultraviolet and white-light images
  collected by SOHO, SDO and STEREO that allow us to specify the extent of
  the coronal shock associated with the CME and whether the SEPs observed
  at the three heliospheric locations were accelerated and injected by the
  shock. Alternatively, we study whether transport mechanisms in the solar
  corona and/or interplanetary space explain the arrival of particles
  to those spacecraft poorly connected to the particle sources. Finally,
  we discuss whether the large-scale physics-based prediction models of
  the heliosphere, currently used by the Space Weather Forecast Offices
  at NOAA and NASA/GSFC, provide a good description for the connectivity
  of each spacecraft with the particle sources in interplanetary space.

Title: Dynamic Mapping of Coronal Activity
Authors: Thompson, B. J.; Uritsky, V. M.; Ireland, J.; Young, C. A.;
   Kirk, M. S.
Bibcode: 2016AGUFMSH11A2224T
Altcode:
  There is a great deal of variation in how CMEs are manifested in
  EUV and coronagraph images. Complicating the issue is the range
  of CME-associated phenomena: shocks, waves, prominences, flares,
  dimmings, to name a few. None of these phenomena are a necessary
  or sufficient condition for a CME. However, each can provide clues
  as to CME origin, topology, and kinematics. New analysis strategies
  have been devised specifically to extract key properties of CMEs and
  CME-associated phenomena, with results that are converging towards
  a more consistent model of solar eruptive menagerie. We will discuss
  techniques such as Persistence Mapping and Time Convolution mapping,
  and how they are used to extract the dynamics of eruptive phenomena.

Title: Asymmetries in Solar Particle Events: Are They Related to
    Dimming Region Asymmetries Relative to Flares?
Authors: Richardson, I. G.; Thompson, B. J.; von Rosenvinge, T. T.
Bibcode: 2016AGUFMSH32A..03R
Altcode:
  Studies of the longitudinal distribution of solar energetic particles
  generally use the location of the related solar flare as a reference
  longitude. In particular, particle intensities are typically found
  to fall off with increasing "connection angle" - the longitudinal
  separation between the flare and the footpoint of the field line
  passing the observing spacecraft - and are often fitted by Gaussians
  in connection angle. Although the peak of the Gaussian is often close
  to zero connection angle, i.e., on field lines connecting close to
  the flare longitude, some 25 MeV proton events observed by both STEREO
  spacecraft and at the Earth show clear asymmetries, either to the east
  or west relative to the flare longitude, in their early stages. There
  are various possible reasons for such asymmetries, one being that
  the flare longitude may not represent the expansion direction of the
  coronal mass ejection and associated shock, which may accelerate the
  particles. Since coronal dimming regions lie below CMEs, and dimmings
  may form asymmetrically relative to flares, we use the centroid of a
  dimming region as a proxy for CME direction and examine whether there is
  any relationship between the east-west asymmetry in the dimming relative
  to the flare and the longitudinal asymmetry in the related SEP event.

Title: Dynamic Mapping of Prominence Activity
Authors: Thompson, Barbara J.; Gilbert, Holly R.; Kirk, Michael
   S.; Mays, M. Leila.; Ofman, Leon; Uritsky, Vadim; Wyper, Peter;
   Hovis-Afflerbach, Beryl
Bibcode: 2016usc..confE..82T
Altcode:
  We present the results of a prominence mapping effort designed to
  extract the dynamics of erupting prominences. The material from
  partially erupting prominences can fall back to the sun, tracing
  out the topology of the mid- and post-eruptive corona. One question
  involving the range of observed behavior is the role of magnetic
  field topology and evolution in determining the motion of the erupting
  prominence material. A variable-g ballistic approximation is applied
  to study the motion of the material, using the deviations from constant
  angular momentum as a means of quantifying the local Lorentz (and other)
  forces on each piece of material. Variations in dynamic behavior can be
  traced back to changes in the local magnetic field and the formation
  of instabilities such as Rayleigh-Taylor. We discuss the use of the
  prominence trajectories as a means of diagnosing eruptive topologies.

Title: Image-based reconstruction of the Newtonian dynamics of solar
    coronal ejecta
Authors: Uritsky, Vadim M.; Thompson, Barbara J.
Bibcode: 2016usc..confE.126U
Altcode:
  We present a new methodology for analyzing rising and falling dynamics
  of unstable coronal material as represented by high-cadence SDO AIA
  images. The technique involves an adaptive spatiotemporal tracking of
  propagating intensity gradients and their characterization in terms
  of time-evolving areas swept out by the position vector originated
  from the Sun disk center. The measured values of the areal velocity
  and acceleration are used to obtain quantitative information on
  the angular momentum and acceleration along the paths of the rising
  and falling coronal plasma. In the absence of other forces, solar
  gravitation results in purely ballistic motions consistent with the
  Kepler's second law; non-central forces such as the Lorentz force
  introduce non-zero torques resulting in more complex motions. The
  developed algorithms enable direct evaluation of the line-of-sight
  component of the net torque applied to a unit mass of the ejected
  coronal material which is proportional to the image-plane projection
  of the observed areal acceleration. The current implementation of
  the method cannot reliably distinguish torque modulations caused
  by the coronal force field from those imposed by abrupt changes
  of plasma mass density and nontrivial projection effects. However,
  it can provide valid observational constraints on the evolution of
  large-scale unstable magnetic topologies driving major solar-coronal
  eruptions as demonstrated in the related talk by B. Thompson et al.

Title: AWARE - The Automated EUV Wave Analysis and REduction algorithm
Authors: Ireland, J.; Inglis; A. R.; Shih, A. Y.; Christe, S.; Mumford,
   S.; Hayes, L. A.; Thompson, B. J.
Bibcode: 2016usc..confE..59I
Altcode:
  Extreme ultraviolet (EUV) waves are large-scale propagating disturbances
  observed in the solar corona, frequently associated with coronal
  mass ejections and flares. Since their discovery over two hundred
  papers discussing their properties, causes and physics have been
  published. However, their fundamental nature and the physics of their
  interactions with other solar phenomena are still not understood. To
  further the understanding of EUV waves, and their relation to other
  solar phenomena, we have constructed the Automated Wave Analysis and
  REduction (AWARE) algorithm for the detection of EUV waves over the full
  Sun. The AWARE algorithm is based on a novel image processing approach
  to isolating the bright wavefront of the EUV as it propagates across
  the corona. AWARE detects the presence of a wavefront, and measures
  the distance, velocity and acceleration of that wavefront across the
  Sun. Results from AWARE are compared to results from other algorithms
  for some well known EUV wave events. Suggestions are also give for
  further refinements to the basic algorithm presented here.

Title: Relationship of EUV Irradiance Coronal Dimming Slope and
    Depth to Coronal Mass Ejection Speed and Mass
Authors: Mason, James Paul; Woods, Thomas N.; Webb, David F.; Thompson,
   Barbara J.; Colaninno, Robin C.; Vourlidas, Angelos
Bibcode: 2016ApJ...830...20M
Altcode: 2016arXiv160705284M
  Extreme ultraviolet (EUV) coronal dimmings are often observed in
  response to solar eruptive events. These phenomena can be generated
  via several different physical processes. For space weather, the most
  important of these is the temporary void left behind by a coronal mass
  ejection (CME). Massive, fast CMEs tend to leave behind a darker void
  that also usually corresponds to minimum irradiance for the cooler
  coronal emissions. If the dimming is associated with a solar flare,
  as is often the case, the flare component of the irradiance light
  curve in the cooler coronal emission can be isolated and removed
  using simultaneous measurements of warmer coronal lines. We apply
  this technique to 37 dimming events identified during two separate
  two-week periods in 2011 plus an event on 2010 August 7, analyzed in a
  previous paper to parameterize dimming in terms of depth and slope. We
  provide statistics on which combination of wavelengths worked best
  for the flare-removal method, describe the fitting methods applied
  to the dimming light curves, and compare the dimming parameters
  with corresponding CME parameters of mass and speed. The best linear
  relationships found are v CME km s ≈ 2.36 × 10 6 km % × s dim % s
  m CME [ g ] ≈ 2.59 × 10 15 g % × d dim [ % ] . These relationships
  could be used for space weather operations of estimating CME mass and
  speed using near-real-time irradiance dimming measurements.

Title: SDO 2016: Unraveling the Suns Complexity
Authors: Pesnell, W. Dean; Thompson, Barbara
Bibcode: 2016usc..conf.....P
Altcode:
  Living With a Star Solar Dynamics Observatory research connects to many
  areas of solar physics and many other solar missions. Tracing these
  connections allows us to build a more accurate understanding of the Sun
  and solar activity. The workshop will focus on our improved knowledge
  and understanding of the Suns magnetic field that have come from the
  SDO data, and what will come in the future. Scientific sessions will
  feature a broad spectrum of science topics fundamental to SDO science
  investigations: Atmospheric Imaging Assembly (AIA), EUV Variability
  Experiment (EVE), and Helioseismic and Magnetic Imager (HMI), as
  well as the overlap between SDO and other scientific missions and
  activities. We invite you to celebrate the breadth of research topics
  enabled by SDO during its Prime Mission and the First Extended Mission.

Title: Chemical abundance gradients from open clusters in the Milky
Way disk: Results from the APOGEE survey
Authors: Cunha, K.; Frinchaboy, P. M.; Souto, D.; Thompson, B.;
   Zasowski, G.; Allende Prieto, C.; Carrera, R.; Chiappini, C.; Donor,
   J.; García-Hernández, D. A.; García Pérez, A. E.; Hayden, M. R.;
   Holtzman, J.; Jackson, K. M.; Johnson, J. A.; Majewski, S. R.;
   Mészáros, S.; Meyer, B.; Nidever, D. L.; O'Connell, J.; Schiavon,
   R. P.; Schultheis, M.; Shetrone, M.; Simmons, A.; Smith, V. V.; et al.
Bibcode: 2016AN....337..922C
Altcode: 2016arXiv160103099C
  Metallicity gradients provide strong constraints for understanding
  the chemical evolution of the Galaxy. We report on radial abundance
  gradients of Fe, Ni, Ca, Si, and Mg obtained from a sample of 304
  red-giant members of 29 disk open clusters, mostly concentrated
  at galactocentric distances between ∼ 8-15 kpc, but including
  two open clusters in the outer disk. The observations are from the
  APOGEE survey. The chemical abundances were derived automatically by
  the ASPCAP pipeline and these are part of the SDSS III Data Release
  12. The gradients, obtained from least squares fits to the data,
  are relatively flat, with slopes ranging from -0.026 to -0.033 dex
  kpc<SUP>-1</SUP> for the α-elements [O/H], [Ca/H], [Si/H], and [Mg/H],
  and -0.035 dex kpc<SUP>-1</SUP> and -0.040 dex kpc<SUP>-1</SUP> for
  [Fe/H] and [Ni/H], respectively. Our results are not at odds with
  the possibility that metallicity ([Fe/H]) gradients are steeper in
  the inner disk ({R_GC∼ 7}-12 kpc) and flatter towards the outer
  disk. The open cluster sample studied spans a significant range in
  age. When breaking the sample into age bins, there is some indication
  that the younger open cluster population in our sample (log age &lt;
  8.7) has a flatter metallicity gradient when compared with the gradients
  obtained from older open clusters.

Title: Asymmetries in Solar Particle Events: Are They Related to
    Dimming Region Asymmetries Relative to Flares?
Authors: Richardson, Ian; Thompson, Barbara J.; von Rosenvinge,
   Tycho T.
Bibcode: 2016shin.confE..22R
Altcode:
  Studies of the longitudinal distribution of solar energetic particles
  have typically assumed the location of the related solar flare as a
  reference longitude. For example, intensities observed at spacecraft are
  typically mapped back to the Sun along Parker spiral field lines (often
  with some modification near the Sun given by a coronal field model) and
  the resulting 'connection angle' between the flare location and field
  line foot point is then obtained. Particle intensities typically fall
  off with increasing connection angle, and are often fitted by Gaussians
  in connection angle. Frequently, the peak of the Gaussian is close to
  zero connection angle, i.e., the largest particle intensities occur on
  field lines connecting close to the flare longitude. However, we find
  that some 25 MeV proton events observed by the two STEREO spacecraft
  and at the Earth show significant asymmetries either to the east or
  west relative to the flare longitude. One possible contributor is that
  the flare longitude may not represent the expansion direction of the
  CME. Recent results indicate that coronal dimming regions lie below
  CMEs, and dimmings may form asymmetrically relative to flares. Using the
  centroid of a dimming region as a proxy for CME direction, we examine
  whether there is any relationship between the east-west asymmetry in
  the dimming relative to the flare and the longitudinal asymmetry in
  the related SEP event.

Title: Dimmings as a footprint of coronal mass ejections
Authors: Thompson, Barbara J.; Allred, Joel C.; Kay, Christina;
   Nieves-Chinchilla, Teresa
Bibcode: 2016shin.confE..55T
Altcode:
  Large regions of coronal dimming often accompany coronal mass ejections
  (CMEs). Of all of the EUV signatures of CMEs, dimmings (when present)
  are the best match to the location and extent of the coronagraph
  CME observations. They last on timescales from minutes to hours, are
  sometimes patchy in appearance, and can extend far (&gt;1 RSun) from
  the flaring region. They are known to be good indicators of the site
  of evacuated material, and have been extensively studied as a CME mass
  source. We investigate the possibility that dimmings also serve as a
  magnetic footprint of CMEs. Dimmings develop during or soon after the
  eruption, and may trace field lines locally opened during the CME. These
  dimming regions can be extensive, representing at least part of the
  'base' of a CME and the mass and magnetic flux transported outward by
  it. We report on three-dimensional observations of the co- development
  of dimmings in EUV and coronagraph images, magnetic field topologies
  represented by the dimmings, and (when available) in situ observations
  that can be used as a diagnostic of the erupting field topology.

Title: Dynamic Mapping of Prominence Activity
Authors: Thompson, Barbara J.; Uritsky, Vadim; Ofman, Leon
Bibcode: 2016shin.confE.141T
Altcode:
  We present the results of a prominence mapping effort designed to
  extract the dynamics of both erupting and quiescent prominences. The
  material from partially erupting prominences can fall back to the sun,
  tracing out the topology of the post-eruptive corona. A variable-g
  ballistic approximation is applied to study the motion of the material,
  using the deviations from constant angular momentum as a means of
  quantifying the local Lorentz (and other) forces on each piece of
  material. Variations in dynamic behavior can be traced back to changes
  in the local magnetic field and the formation of instabilities such
  as Rayleigh-Taylor.

Title: Persistence Mapping Using EUV Solar Imager Data
Authors: Thompson, B. J.; Young, C. A.
Bibcode: 2016ApJ...825...27T
Altcode:
  We describe a simple image processing technique that is useful for
  the visualization and depiction of gradually evolving or intermittent
  structures in solar physics extreme-ultraviolet imagery. The technique
  is an application of image segmentation, which we call “Persistence
  Mapping,” to isolate extreme values in a data set, and is particularly
  useful for the problem of capturing phenomena that are evolving in both
  space and time. While integration or “time-lapse” imaging uses the
  full sample (of size N ), Persistence Mapping rejects (N - 1)/N of the
  data set and identifies the most relevant 1/N values using the following
  rule: if a pixel reaches an extreme value, it retains that value until
  that value is exceeded. The simplest examples isolate minima and maxima,
  but any quantile or statistic can be used. This paper demonstrates
  how the technique has been used to extract the dynamics in long-term
  evolution of comet tails, erupting material, and EUV dimming regions.

Title: About Steady and Transient States During Two Long Intervals
    of Extremely Low Speed Solar Wind Speed Observed by STEREO and Wind
Authors: Berdichevsky, Daniel Benjamin; Galvin, A. B.; Farrugia,
   C. J.; Thompson, B. J.; Vasquez, B.; Simunac, K. D. C.
Bibcode: 2016shin.confE..76B
Altcode:
  The passage of a solar wind stream extending from October 24 to 30,
  2010, was well monitored, ahead of arrival at Earth's location of a
  possible corotating stream, with the help of the STEREO-A instruments
  IMPACT and PLASTIC. This was an extremely slow flow which exhibited the
  following features <P />a. An interval of over 2 days of speeds below
  250 km/s <P />b. At the start, an expanding magnetic cloud interval
  lasting about 14 hrs. <P />c. The presence of distinct ratios in charge
  states suggesting presence of transient material in and outside the
  magnetic cloud. <P />d. The presence in the plasma of a sizeable amount
  of He++ which we compare with the predictions made at the observed
  SW speed. <P />We check with Lopez (1987) the observed and predicted
  estimates of the thermal velocity of the protons observed for the
  interval. In addition, we present the implication on the Parker model
  for the possible temperature of the corona assuming the dominant aspects
  of the outflow correspond to the case of an steady solar wind. The
  lack of passage of the event near Earth location is discussed, and its
  implications regarding the spatial extent of the solar outflow and the
  nature of its overall origin is assessed. Although not on year 2010,
  at the Lagrangian point L1, we observe with Wind the occurrence in
  years 2007 to 2009 of several intervals of low speed solar wind, of
  which for a comparison we select the low solar wind interval starting
  Dec 8, 2009 and which continued for more than 5 days. The interval at
  Wind has a similar extension as the one at STEREO-A. This includes the
  presence of a MC. Charge states are compared as well as the presence
  of the alpha-to-proton number density ratio

Title: Dimmings as a footprint of coronal mass ejections
Authors: Thompson, Barbara J.; Allred, Joel C.; Kay, Christina;
   Krista, Larisza Diana; Mason, James; Nieves-Chinchilla, Teresa;
   Reinard, Alysha; Webb, David F.
Bibcode: 2016SPD....4710601T
Altcode:
  Large regions of coronal dimming often accompany coronal mass ejections
  (CMEs). Of all of the EUV signatures of CMEs, dimmings (when present)
  are the best match to the location and extent of the coronagraph
  CME observations. They last on timescales from minutes to hours, are
  sometimes patchy in appearance, and can extend far (&gt;1 RSun) from
  the flaring region. They are known to be good indicators of the site
  of evacuated material, and have been extensively studied as a CME mass
  source. We investigate the possibility that dimmings also serve as a
  magnetic footprint of CMEs. Dimmings develop during or soon after the
  eruption, and may trace field lines locally opened during the CME. These
  dimming regions can be extensive, representing at least part of the
  “base” of a CME and the mass and magnetic flux transported outward
  by it. We report on three-dimensional observations of the co-development
  of dimmings in EUV and coronagraph images, magnetic field topologies
  represented by the dimmings, and (when available) in situ observations
  that can be used as a diagnostic of the erupting field topology.

Title: ENLIL Global Heliospheric Modeling as a Context For Multipoint
    Observations
Authors: Mays, M. Leila; Odstrcil, Dusan; Luhmann, Janet; Bain, Hazel;
   Li, Yan; Schwadron, Nathan; Gorby, Matt; Thompson, Barbara; Jian,
   Lan; Möstl, Christian; Rouillard, Alexis; Davies, Jackie; Temmer,
   Manuela; Rastaetter, Lutz; Taktakishvili, Aleksandre; MacNeice, Peter;
   Kuznetsova, Maria
Bibcode: 2016EGUGA..1811638M
Altcode:
  We present heliospheric simulation case studies using recent
  enhancements to WSA--ENLIL+Cone (version 2.8) at the Community
  Coordinated Modeling Center (CCMC). The global 3D MHD ENLIL model
  provides a time-dependent description of the background solar wind
  plasma and magnetic field using a sequence of WSA coronal model
  maps as input at the inner boundary of 21.5 Rs. A homogeneous,
  over-pressured hydrodynamic plasma cloud is launched through the
  inner boundary of the heliospheric computational domain and into
  the background solar wind. Multipoint observations help constrain
  simulations and this modeling system provides global context and
  arrival times of the solar wind streams and CMEs at Earth, planets,
  and spacecraft. Additionally, one can extract the magnetic topologies
  of observer-connected magnetic field lines and all plasma and shock
  properties along those field lines. ENLIL "likelihood/all-clear"
  forecasting maps provide expected intensity, timing/duration of events
  at locations throughout the heliosphere with "possible SEP affected
  areas" color-coded based on shock strength. ENLIL simulations are also
  useful to drive SEP models such as the Solar Energetic Particle Model
  (SEPMOD) (Luhmann et al. 2007, 2010) and Energetic Particle Radiation
  Environment Module (EPREM) (Schwadron et al., 2010). SEPMOD injects
  protons onto a sequence observer field lines at intensities dependent
  on the connected shock source strength which are then integrated at
  the observer to approximate the proton flux. EPREM couples with MHD
  models such as ENLIL and computes energetic particle distributions
  based on the focused transport equation along a Lagrangian grid of
  nodes that propagate out with the solar wind. Studies have shown
  that accurate descriptions of the heliosphere, and hence modeled CME
  arrival times and SEPs, are achieved by ENLIL only when the background
  solar wind is well-reproduced and CME parameters are accurate. It is
  essential to include all of the relevant CMEs and allow enough time
  for the events to propagate and interact. In this presentation we
  demonstrate several event case studies of ENLIL simulations compared
  with multipoint observations, exploring the background solar wind and
  CME pre-conditioning, and including comparisons between ENLIL synthetic
  j-maps with observed STEREO/HI j-maps using catalogues from the HELCATS
  FP7 project.

Title: Deriving Kinematic Properties of Non-Radial, Asymmetric and
Deflecting CMEs: Methods and Implications
Authors: Thompson, B. J.; Liewer, P. C.; Mays, M. L.; Richardson,
   I. G.; Kwon, R.; Ofman, L.; Makela, P. A.; Ireland, J.; Hess, P.;
   Waldron, Z.
Bibcode: 2015AGUFMSH33B2467T
Altcode:
  An improved understanding of the kinematic properties of CMEs and
  CME-associated phenomena has several impacts: 1) a less ambiguous
  method of mapping propagating structures into their inner coronal
  manifestations, 2) a clearer view of the relationship between the
  "main" CME and CME-associated brightenings, and 3) an improved
  identification of the heliospheric sources of shocks, Type II bursts,
  and SEPs. However, there are several challenges in characterizing
  the kinematic properties of CMEs. Most rapidly-evolving eruptions are
  accompanied by changes in the surrounding corona. The larger the impact
  on the surrounding corona, the more difficult it is to separate the
  "main" CME from the CME-associated brightenings. Complicating the
  issue is the range of observed propagation properties: super-radial
  expansion, asymmetric expansion, non-radial propagation, and alterations
  in the direction of propagation. These properties can be a function
  of both the internal magnetic structure of the CME and the structure
  of the corona through which the CME is propagating. While the relative
  contribution of internal/external factors can be difficult to assess,
  it is of fundamental importance because it not only reveals the nature
  of CMEs but also CME-associated phenomena such as EUV waves, Type
  II radio bursts, shocks, and SEPs. Most halo CMEs are a combination
  of both the "main" CME and the CME-associated brightenings, but
  new diagnostic methods such as time convolution mapping can help
  separate the CME mass from the impacted corona. Additionally, while
  most CME-fitting methods assume symmetry about the radial direction,
  adaptive methods allow us to study highly asymmetric CME expansion
  and take into account the fundamentally different natures of the CME
  and the shocked/deflected corona. Several methods will be examined,
  and each has their respective strengths and weaknesses; for example,
  the difference between the direction of a highly non-radial CME and a
  sun-centered model's orientation can exceed 45 degrees, which impacts
  our ability to correctly assess changes in propagation direction and
  the causes of these changes. We examine the assumptions inherent in
  these methods and how they may produce artifacts that can influence
  conclusions about CME kinematics.

Title: On the Structure of a Long Interval of Extremely Low Speed
    Solar Wind Observed by STEREO, and Comparison to Similar Events in
    the Same Solar Cycle
Authors: Berdichevsky, D. B.; Galvin, A. B.; Farrugia, C. J.; Thompson,
   B. J.
Bibcode: 2015AGUFMSH23A2430B
Altcode:
  The passage of a solar wind stream extending from October 24 to 30,
  2010, with its magnetized plasma was well monitored, ahead of Earth's
  location arrival of a possible corotating stream, with the help of the
  STEREO-A instruments IMPACT and PLASTIC. This was an extremely slow
  flow which exhibited the following features a. An interval of over
  2 days showing a solar wind speed below 250 km/s b. At the start,
  an expanding magnetic cloud interval lasting about 14 hrs. c. The
  presence of distinct ratios in charge states suggesting presence
  of transient at material in and outside the magnetic cloud. d. The
  presence in the plasma of a sizeable amount of He++ which we compare
  with the predictions made at the observed SW speed. We check with Lopez
  (1987) the observed and predicted estimates of the thermal velocity
  of the protons observed for the interval. In addition we present the
  implication on the parker model for the possible temperature of the
  corona assuming the dominant aspects of the outflow correspond to
  the case of an steady solar wind. The lack of passage of the event
  near Earth location is discussed, and its implications regarding
  its extension in space of the solar outflow and the nature of its
  overall origin is assessed. Although not on the same year 2010, at the
  Lagrangian point L1, we observe with Wind the occurrence in 2007 to 2009
  of several intervals of low speed solar wind, of which for a comparison
  we select the two low solar wind intervals starting Nov 29, and Dec 8,
  2009 which extended over more than 5 days each. These intervals at
  Wind have a similar extension as the one at STEREO-A. However, the
  presence of a MC or not are less clear for these cases. Also charge
  states are compared as well as the presence of the alpha--to--proton
  number density ratio.

Title: Survey of high-altitude partially erupting prominences
Authors: Gilbert, H. R.; St Cyr, O. C.; Thompson, B. J.; Inglis,
   A. R.; Xie, H.
Bibcode: 2015AGUFMSH53B2490G
Altcode:
  Solar prominences exhibit a range of eruptive-like dynamic activity,
  including in some cases the confined or 'failed' ejection of prominence
  material from the solar atmosphere. Many prominences exhibit a partial
  eruption in which some mass escapes while the remaining mass drains
  back to the photosphere. This process may involve the formation of an
  X-type neutral line in this region, which allows disconnection of part
  of the prominence material. In a previous study (Gilbert et al. 2000)
  it was found that this separation tends to occur in the height range
  from 1.20 to 1.35 Rsun. More recently, the separation point in these
  types of partial eruptions has been observed to occur at much larger
  heights. We investigate a selection of these higher partial eruptions,
  exploring the characteristics of the prominences and their associated
  CMEs to better understand the dynamical processes in the solar
  atmosphere associated with eruption.

Title: Propagation of the 7 January 2014 CME and Resulting Geomagnetic
    Non-event
Authors: Mays, M. L.; Thompson, B. J.; Jian, L. K.; Colaninno, R. C.;
   Odstrcil, D.; Möstl, C.; Temmer, M.; Savani, N. P.; Collinson, G.;
   Taktakishvili, A.; MacNeice, P. J.; Zheng, Y.
Bibcode: 2015ApJ...812..145M
Altcode: 2015arXiv150906477M
  On 2014 January 7 an X1.2 flare and coronal mass ejection (CME) with a
  radial speed ≈2500 km s<SUP>-1</SUP> was observed from near an active
  region close to disk center. This led many forecasters to estimate a
  rapid arrival at Earth (≈36 hr) and predict a strong geomagnetic
  storm. However, only a glancing CME arrival was observed at Earth
  with a transit time of ≈49 hr and a K <SUB>P</SUB> geomagnetic
  index of only 3-. We study the interplanetary propagation of this
  CME using the ensemble Wang-Sheeley-Arge (WSA)-ENLIL+Cone model,
  that allows a sampling of CME parameter uncertainties. We explore a
  series of simulations to isolate the effects of the background solar
  wind solution, CME shape, tilt, location, size, and speed, and the
  results are compared with observed in situ arrivals at Venus, Earth,
  and Mars. Our results show that a tilted ellipsoid CME shape improves
  the initial real-time prediction to better reflect the observed in situ
  signatures and the geomagnetic storm strength. CME parameters from the
  Graduated Cylindrical Shell model used as input to WSA-ENLIL+Cone, along
  with a tilted ellipsoid cloud shape, improve the arrival-time error
  by 14.5, 18.7, 23.4 hr for Venus, Earth, and Mars respectively. These
  results highlight that CME orientation and directionality with respect
  to observatories play an important role in understanding the propagation
  of this CME, and for forecasting other glancing CME arrivals. This study
  also demonstrates the importance of three-dimensional CME fitting made
  possible by multiple viewpoint imaging.

Title: False Alarm Rate in Predicting the Longitudinal Dependence
    of SEP Intensity
Authors: Mays, M. Leila; Richardson, I. G.; Thompson, B. J.
Bibcode: 2015shin.confE.165M
Altcode:
  Richardson et al. (Solar Physics, 2014, 289:8) studied the longitudinal
  dependence of &gt;25 MeV solar proton events observed by multiple
  spacecraft from December 2009 -December 2012, together with their solar
  sources. Gaussian fits to the peak SEP intensity observed by multiple
  spacecraft versus the connection angle (phi) were combined together
  with the correlation of the peak intensity with the associated CME
  speed V, leading to an equation for the 14 - 24 MeV proton intensity: I
  (phi) (MeV s cm2 sr)?1 = 0.013 exp(0.0036V ?phi^2/2Ïƒ^2). In this
  work we apply this equation to approximately 100 CMEs which have
  been associated with flares from 2010-2015 in the DONKI database
  which consists of CME measurements performed real-time by CCMC/SWRC
  (http://kauai.ccmc.gsfc.nasa.gov/DONKI/). We compare the predicted SEP
  intensities with those observed and examine the false alarm rate and
  whether radio bursts are a useful discriminator to reduce false alarms.

Title: The Space Weather Research Laboratory 'Research To Operations'
    (R2O) Mini-Workshop Program
Authors: Thompson, Barbara J.; Friedl, L. A.; Kuznetsova, M.; Mays,
   M. L.; Nieves-Chinchilla, T.; Pulkkinen, A. A.; Richardson, I. G.;
   Stehr, J. W.; Zesta, E.; Zheng, Y.
Bibcode: 2015shin.confE.169T
Altcode:
  The Space Weather Research to Operations (R2O) Working Group is hosted
  by NASA GSFC's Heliophysics Science Division (HSD), but participants
  from outside organizations and institutions also play important
  roles. The focus of the R2O Working Group is to capitalize on the
  research and knowledge of scientists who are not forecasters, and
  improve their awareness of forecasting and research needs. Although
  there are many research results that are directly related to space
  weather, there is a need to help non-forecasters communicate new results
  to forecasters and turn scientific advances into ingestible products
  by forecasting operations. <P />The R2O program organizes a series
  of theme-focused workshops in order to quickly advance communication
  in each themed topic. Each R2O mini-workshop is an open forum where
  operations experts, forecasters and researchers discuss the state of the
  knowledge of a chosen space weather research topic. The discussion then
  moves to which aspects of current research activities have potential
  to be used in space weather forecasting. The goal is to be broad yet
  comprehensive, with the aim of determining which items have the greatest
  potential for space weather development. <P />The ultimate goal is
  to produce tools and products that can easily be added to operations
  and improve forecasts. Team members are able to identify topics that
  require further collaboration and research, but have great potential
  in the long-term to provide useful tools. Many continue the effort by
  publishing research papers on the topic or choosing to seek support
  through a proposal. A useful tool to guide the discussions is the
  concept of 'Application Readiness Levels' (ARLs) developed by the NASA
  Earth Science Applications Office. ARLs parallel Technology Readiness
  Levels (TRLs), and allow us to assess different areas of knowledge
  and research and keep track of how close to 'full implementation'
  a given model or data analysis effort is. <P />A final aspect of this
  discussion is the reverse stream of information, namely Operations to
  Research (O2R). O2R includes the feedback of operational environment to
  guide research goals, the use of operational assets to enable research,
  and the use of an operational environment to validate, question, and
  refine research efforts. A healthy circle based on R2O-O2R activities
  means that the operational and research communities have formed a
  successful, close-looped partnership, are aware of the other's needs,
  and are making steps towards improvement. In the O2R environment,
  forecasters are not passive recipients of scientific knowledge;
  they actively work with the research community to refine and develop
  new research goals. A major driver of the popularity of the annual
  'Space Weather Workshops' hosted by the Space Weather Research Center
  in Boulder, CO is due to this beneficial relationship.

Title: Predicting the magnetic vectors within coronal mass ejections
arriving at Earth: 1. Initial architecture
Authors: Savani, N. P.; Vourlidas, A.; Szabo, A.; Mays, M. L.;
   Richardson, I. G.; Thompson, B. J.; Pulkkinen, A.; Evans, R.;
   Nieves-Chinchilla, T.
Bibcode: 2015SpWea..13..374S
Altcode: 2015arXiv150202067S
  The process by which the Sun affects the terrestrial environment
  on short timescales is predominately driven by the amount
  of magnetic reconnection between the solar wind and Earth's
  magnetosphere. Reconnection occurs most efficiently when the solar
  wind magnetic field has a southward component. The most severe impacts
  are during the arrival of a coronal mass ejection (CME) when the
  magnetosphere is both compressed and magnetically connected to the
  heliospheric environment. Unfortunately, forecasting magnetic vectors
  within coronal mass ejections remain elusive. Here we report how,
  by combining a statistically robust helicity rule for a CME's solar
  origin with a simplified flux rope topology, the magnetic vectors
  within the Earth-directed segment of a CME can be predicted. In
  order to test the validity of this proof-of-concept architecture for
  estimating the magnetic vectors within CMEs, a total of eight CME
  events (between 2010 and 2014) have been investigated. With a focus
  on the large false alarm of January 2014, this work highlights the
  importance of including the early evolutionary effects of a CME for
  forecasting purposes. The angular rotation in the predicted magnetic
  field closely follows the broad rotational structure seen within the
  in situ data. This time-varying field estimate is implemented into
  a process to quantitatively predict a time-varying Kp index that is
  described in detail in paper II. Future statistical work, quantifying
  the uncertainties in this process, may improve the more heuristic
  approach used by early forecasting systems.

Title: What Do EUV Dimmings Tell Us About CME Topology
Authors: Thompson, Barbara J.; DeRosa, Marc L.; Fisher, Richard R.;
   Krista, Larisza D.; Kwon, Ryun Young; Mason, James P.; Mays, Mona L.;
   Nitta, Nariaki V.; Webb, David F.; West, Matthew J.
Bibcode: 2015TESS....121201T
Altcode:
  Large-scale coronal EUV dimmings develop on timescales of hours in
  association with a flare or filament eruption, and are known to be
  well correlated with coronal mass ejections (CMEs). However, it is not
  clear why some CMEs have dimmings and some do not, nor is it clear how
  these dimmings relate to CME topology. The inner coronal coverage of
  SDO AIA and STEREO EUVI, combined with the extended field of view of
  PROBA2's SWAP imager, allow us the opportunity to map the topology of
  a dimming region in three dimensions into an erupting CME. Although
  the location and extent of a dimming region appears to be the best
  indicator of the inner "footprint" of a CME, the correlation is far
  from perfect. However, dimmings can provide vital clues about the
  development and 3D kinematics of CMEs. This is particularly important
  as we are currently in an extended period where the STEREO coronagraph
  images are not always available and are increasingly "mirroring" LASCO
  images, and therefore the 3D properties of a CME will be difficult
  to deduce. Thus, understanding the inner coronal manifestations of
  a CME can provide clues to its structure and dynamics, even without
  multi-viewpoint coronagraph observations. We present the results of
  this combined analysis effort, along with a discussion of how dimmings
  can be used to forecast CME trajectories.

Title: Survey of high-altitude partially erupting prominences
Authors: Gilbert, Holly; St Cyr, O. C.; Inglis, Andrew; Xie, Hong;
   Thompson, Barbara J.
Bibcode: 2015TESS....120316G
Altcode:
  Solar prominences exhibit a range of eruptive-like dynamic activity,
  including in some cases the confined or 'failed' ejection of prominence
  material from the solar atmosphere. Many prominences exhibit a partial
  eruption in which some mass escapes while the remaining mass drains
  back to the photosphere. This process may involve the formation of an
  X-type neutral line in this region, which allows disconnection of part
  of the prominence material. In a previous study (Gilbert et al. 2000)
  it was found that this separation tends to occur in the height range
  from 1.20 to 1.35 R<SUB>sun</SUB>. More recently, the separation point
  in these types of partial eruptions has been observed to occur at much
  larger heights. We investigate a selection of these higher partial
  eruptions, exploring the characteristics of the prominences and their
  associated CMEs to better understand the dynamical processes in the
  solar atmosphere associated with eruption.

Title: STEREO as a 'Planetary Hazards' Mission
Authors: Guhathakurta, M.; Thompson, B. J.
Bibcode: 2015hchp.book..197G
Altcode:
  No abstract at ADS

Title: NASA Space Weather Research Center: Addressing the Unique
    Space Weather Needs of NASA Robotic Missions
Authors: Zheng, Y.; Pulkkinen, A. A.; Kuznetsova, M. M.; Maddox,
   M. M.; Mays, M. L.; Taktakishvili, A.; Chulaki, A.; Thompson, B. J.;
   Collado-Vega, Y. M.; Muglach, K.; Evans, R. M.; Wiegand, C.; MacNeice,
   P. J.; Rastaetter, L.
Bibcode: 2014AGUFMSM31A4151Z
Altcode:
  The Space Weather Research Center (SWRC) has been providing space
  weather monitoring and forecasting services to NASA's robotic
  missions since its establishment in 2010. Embedded within the Community
  Coordinated Modeling Center (CCMC) (see Maddox et al. in Session IN026)
  and located at NASA Goddard Space Flight Center, SWRC has easy access
  to state-of-the-art modeling capabilities and proximity to space science
  and research expertise. By bridging space weather users and the research
  community, SWRC has been a catalyst for the efficient transition from
  research to operations and operations to research. In this presentation,
  we highlight a few unique aspects of SWRC's space weather services,
  such as addressing space weather throughout the solar system, pushing
  the frontier of space weather forecasting via the ensemble approach,
  providing direct personnel and tool support for spacecraft anomaly
  resolution, prompting development of multi-purpose tools and knowledge
  bases (see Wiegand et al. in the same session SM004), and educating
  and engaging the next generation of space weather scientists.

Title: The Great "Non-Event" of 7 January 2014: Challenges in CME
    Arrival Time and Geomagnetic Storm Strength Prediction
Authors: Mays, M. L.; Thompson, B. J.; Jian, L.; Evans, R. M.; Savani,
   N.; Odstrcil, D.; Nieves-Chinchilla, T.; Richardson, I. G.
Bibcode: 2014AGUFMSH51E..04M
Altcode:
  We present a case study of the 7 January 2014 event in order to
  highlight current challenges in space weather forecasting of CME
  arrival time and geomagnetic storm strength. On 7 January 2014 an X1.2
  flare and CME with a radial speed ~2400 km/s was observed from active
  region 11943. The flaring region was only ten degrees southwest of disk
  center with extensive dimming south of the active region and preliminary
  analysis indicated a fairly rapid arrival at Earth (~36 hours). Of the
  eleven forecasting groups world-wide who participated in CCMC's Space
  Weather Scoreboard (http://kauai.ccmc.gsfc.nasa.gov/SWScoreBoard),
  nine predicted early arrivals and six predicted dramatic geomagnetic
  storm impacts (Kp predictions ranged from 6 to 9). However, the CME
  only had a glancing blow arrival at Earth - Kp did not rise above 3
  and there was no geomagnetic storm. What happened? One idea is that
  the large coronal hole to the northeast of the active region could
  have deflected the CME. This coronal hole produced a high speed
  stream near Earth reaching an uncommon speed of 900 km/s four days
  after the observed CME arrival. However, no clear CME deflection was
  observed in the outer coronagraph fields of view (~5-20Rs) where CME
  measurements are derived to initiate models, therefore deflection seems
  unlikely. Another idea is the effect of the CME flux rope orientation
  with respect to Earth orbit. We show that using elliptical major and
  minor axis widths obtained by GCS fitting for the initial CME parameters
  in ENLIL would have improved the forecast to better reflect the observed
  glancing blow in-situ signature. We also explore the WSA-ENLIL+Cone
  simulations, the background solar wind solution, and compare with the
  observed CME arrival at Venus (from Venus Express) and Earth.

Title: Brightenings Associated with Falling Filament Material
Authors: Gilbert, H. R.; Inglis, A. R.; Mays, M. L.; Ofman, L.;
   Provornikova, E.; Thompson, B. J.; Young, C. A.
Bibcode: 2014AGUFMSH13B4101G
Altcode:
  Solar filaments exhibit a range of eruptive-like dynamic activity,
  including in some cases the confined or 'failed' ejection of prominence
  material from the solar atmosphere. In rare cases material that
  fails to erupt exhibits a strong interaction with the lower corona as
  the material returns to the solar surface, observed as substantial
  broadband brightening of EUV emission. We investigate a selection
  of recent partial prominence eruptions in order to understand the
  apparent rarity of the brightening phenomenon. Using combined data
  from SDO/AIA and STEREO, we explore the energetics and kinematics of
  these events, assessing the likely conditions of both the corona and
  the prominence material that are required in order to explain these EUV
  brightenings. We further demonstrate the potential of this phenomenon
  as diagnostic tool for both prominence material conditions and the
  coronal magnetic field.

Title: Forecasting the magnetic vectors within a CME at L1 by using
    solar observations.
Authors: Savani, N.; Vourlidas, A.; Szabo, A.; Mays, M. L.; Evans,
   R. M.; Thompson, B. J.; Richardson, I. G.; Pulkkinen, A. A.;
   Nieves-Chinchilla, T.
Bibcode: 2014AGUFMSH43B4213S
Altcode:
  The direction of magnetic vectors within coronal mass ejections has
  important consequences to forecasting terrestrial behaviour, however
  forecasting these vectors remains predominately elusive. Here,
  we report that a simplified system is capable of replicating the
  broad field rotations seen within flux rope CMEs at L1 monitors. The
  predictions are performed under three main themes: 1) The majority of
  the field rotations can be simplified to the constant-alpha force-free
  (CAFF) flux model first implemented circa 1990. 2) The helicity will
  follow the Bothmer &amp; Schwenn system that relies on a reliable
  helicity prediction of active regions during solar cycle. Which has
  been recently confirmed by Wang [2013 ApJ]. 3) The majority of the
  distortions, deflections and rotations will have already occurred
  within coronagraphic field of view, thereby allowing the creation
  of a projected "volume-of-influence" on the Sun, from which Earth's
  position relative to the CME can be estimated. This presentation will
  compare predicted results to the observations from 7 CME events and then
  estimate the sources of uncertainty. As an example, the difference in
  robust statistics from 2 solar cycles of CAFF model fittings for the
  field magnitude will be compared to estimates generated from simulated
  CME-sheaths within forecasting Enlil runs. The figure displays an
  example field vector forecast from the techniques employed above.

Title: What Do EUV Dimmings Tell Us About CME Topology?
Authors: Thompson, B. J.; DeRosa, M. L.; Fisher, R. R.; Krista, L. D.;
   Kwon, R. Y.; Mason, J. P.; Mays, M. L.; Nitta, N.; Savani, N.; West,
   M. J.
Bibcode: 2014AGUFMSH43B4202T
Altcode:
  Large-scale coronal EUV dimmings, developing on timescales of minutes
  to hours in association with a flare or filament eruption, are known to
  exhibit a high correlation with coronal mass ejections. However, it is
  not clear why some CMEs have dimmings and some do not, nor is it clear
  how these dimmings relate to CME topology. The inner coronal coverage
  of SDO AIA and STEREO EUVI, combined with the extended field of view
  of PROBA2's SWAP imager, allow us the opportunity to map the topology
  of a dimming region in three dimensions into an erupting CME. Although
  the location and extent of a dimming region appears to be the best
  indicator of the inner "footprint" of a CME, the correlation is far
  from perfect. However, dimmings can provide vital clues about the
  development and 3D kinematics of a CME. This is particularly important
  as we are entering an extended period of time where STEREO coronagraph
  images will not always be available, and therefore the 3D properties of
  a CME will be difficult to deduce. Therefore, understanding the inner
  coronal manifestations of a CME can provide clues to its structure and
  dynamics, even without multi-viewpoint coronagraph observations. We
  present the results of this combined analysis effort, along with a
  discussion of how dimmings can be used in forecasting CME directions.

Title: VizieR Online Data Catalog: WIYN open cluster
    study. LXII. Photometry of M35 (Thompson+, 2014)
Authors: Thompson, B.; Frinchaboy, P.; Kinemuchi, K.; Sarajedini,
   A.; Cohen, R.
Bibcode: 2014yCat..51480085T
Altcode:
  Using the Kitt Peak National Observatory (KPNO) 0.9m MOSAIC camera,
  a 59'*59' field of view has been observed in UBVRI. M35 images,
  observed over two nights in 2000 February, were taken in two sequences:
  short and long, allowing for the photometry of both the brightest
  and faintest stars in the cluster. <P />JHKs observations of M35 were
  taken using the NEWFIRM instrument on the Kitt Peak 4m Telescope in
  2008 February. The NEWFIRM camera is a grid of four 2k*2k IR detectors,
  creating a 4k*4k image. <P />(1 data file).

Title: WIYN Open Cluster Study. LXII. Comparison of Isochrone Systems
    using Deep Multi-band Photometry of M35
Authors: Thompson, B.; Frinchaboy, P.; Kinemuchi, K.; Sarajedini,
   A.; Cohen, R.
Bibcode: 2014AJ....148...85T
Altcode: 2014arXiv1408.1684T
  The current generation of stellar isochrone models exhibits
  non-negligible discrepancies due to variations in the input
  physics. The success of each model is determined by how well it fits the
  observations, and this paper aims to disentangle contributions from the
  various physical inputs. New deep, wide-field optical and near-infrared
  photometry (UBVRIJHK<SUB>S</SUB> ) of the cluster M35 is presented,
  against which several isochrone systems are compared: Padova, PARSEC,
  Dartmouth, and Y <SUP>2</SUP>. Two different atmosphere models are
  applied to each isochrone: ATLAS9 and BT-Settl. For any isochrone set
  and atmosphere model, observed data are accurately reproduced for all
  stars more massive than 0.7 M <SUB>⊙</SUB>. For stars less massive
  than 0.7 M <SUB>⊙</SUB>, Padova and PARSEC isochrones consistently
  produce higher temperatures than observed. Dartmouth and Y<SUP>2</SUP>
  isochrones with BT-Settl atmospheres reproduce optical data accurately;
  however, they appear too blue in IR colors. It is speculated that
  molecular contributions to stellar spectra in the near-infrared may
  not be fully explored, and that future study may reconcile these
  differences.

Title: Evolving Solar Activity and Its Influence on Space and Earth
Authors: Pesnell, W. Dean; Thompson, Barbara
Bibcode: 2014esai.conf.....P
Altcode:
  The 2014 Living with a Star (LWS) Science Meeting will focus on
  advancing the understanding of the integral system coupling the Sun
  to the Earth. An important part of this meeting is the inclusion of
  the Hinode-8 and IRIS-2 meetings with complementary objectives towards
  improved understanding of the evolving solar activity.

Title: Mechanisms and Observations of Coronal Dimming for the 2010
    August 7 Event
Authors: Mason, James Paul; Woods, T. N.; Caspi, A.; Thompson, B. J.;
   Hock, R. A.
Bibcode: 2014ApJ...789...61M
Altcode: 2014arXiv1404.1364M
  Coronal dimming of extreme ultraviolet (EUV) emission has the
  potential to be a useful forecaster of coronal mass ejections
  (CMEs). As emitting material leaves the corona, a temporary void is
  left behind which can be observed in spectral images and irradiance
  measurements. The velocity and mass of the CMEs should impact the
  character of those observations. However, other physical processes
  can confuse the observations. We describe these processes and the
  expected observational signature, with special emphasis placed on the
  differences. We then apply this understanding to a coronal dimming
  event with an associated CME that occurred on 2010 August 7. Data
  from the Solar Dynamics Observatory's Atmospheric Imaging Assembly
  and EUV Variability Experiment (EVE) are used for observations of the
  dimming, while the Solar and Heliospheric Observatory's Large Angle
  and Spectrometric Coronagraph and the Solar Terrestrial Relations
  Observatory's COR1 and COR2 are used to obtain velocity and mass
  estimates for the associated CME. We develop a technique for mitigating
  temperature effects in coronal dimming from full-disk irradiance
  measurements taken by EVE. We find that for this event, nearly 100%
  of the dimming is due to mass loss in the corona.

Title: Predicting the magnetic vectors within coronal mass ejections
    arriving at Earth
Authors: Savani, Neel P.; Vourlidas, Angelos; Szabo, Adam; Mays,
   M. Leila; Thompson, Barbara; Richardson, Ian; Evans, Rebekah;
   Pulkkinen, Antti; Nieves-Chinchilla, Teresa
Bibcode: 2014shin.confE.164S
Altcode:
  The process by which the Sun affects the terrestrial environment
  on short timescales is predominately driven by the amount
  of magnetic reconnection between the solar wind and Earth's
  magnetosphere. Reconnection occurs most efficiently when the solar
  wind magnetic field has a southward component. The most severe impacts
  are during the arrival of a coronal mass ejection (CME) when the
  magnetosphere is both compressed and magnetically connected to the
  heliospheric environment, leading to disruptions to, for example, power
  grids and satellite navigation. Unfortunately, forecasting magnetic
  vectors within coronal mass ejections remains elusive. Here we report
  how, by combining a statistically robust helicity rule for a CME's solar
  origin with a simplified flux rope topology the magnetic vectors within
  the Earth-directed segment of a CME can be predicted. These magnetic
  vectors can be incorporated into forecasting procedures to predict the
  global response measured by the Kp index more reliably. In particular,
  false predictions of strong geomagnetic events made without magnetic
  field information are considerably reduced. As an example, the forecast
  strength of a geomagnetic storm following a CME on 7 January 2014, is
  reduced from G3 (strong) to G1 (minor) on the NOAA scale when magnetic
  vectors are taken into account.

Title: What are the 'Correct' Parameters (Speed, Width, Direction)
    of Coronal Mass Ejections Associated With 25 MeV Proton Events?
Authors: Richardson, Ian; Thompson, B. J.; von Rosenvinge, T. T.;
   Cane, H. V.
Bibcode: 2014shin.confE.161R
Altcode:
  A correlation between the intensity of solar energetic particle (SEP)
  events and the speed of the associated coronal mass ejection (CME)
  has been reported for over 35 years and is generally interpreted as
  evidence for particle acceleration by CME-driven shocks. However,
  the wide (orders of magnitude) spread in SEP intensity for events
  related to CMEs with similar speeds has led to a number of efforts
  to identify other influences on the size of SEP events. We suggest,
  from comparing values from independent CME catalogs (e.g., CDAW,
  CACTUS, DONKI, SEEDS) and from observations in quadrature for the
  CMEs associated with 200 25 MeV proton events (Richardson et al.,
  DOI 10.1007/s11207-014-0524-8), that uncertainties in CME speed also
  contribute to this scatter. While CME speeds tend to be correlated in
  different catalogs for the group of events, for individual events there
  is no consistent relationship in the CME speeds. We point out several
  ways this may occur, for example by different ways of defining CME speed
  (e.g., the fastest feature or average over the CME front) and whether
  CME identification and measurement is manual or automated. CME widths
  vary even more widely between catalogs and are influenced by plane
  of the sky projection and how the width is estimated from coronagraph
  images. In particular, the high degree of association ( 50%) between
  the SEP events and 'full halo' CMEs in the CDAW catalog is removed
  when other catalogs or quadrature observations are considered. We
  suggest that CME parameters should be carefully determined, and the
  most reliable values used, when studying the relationship between SEP
  intensity and CME parameters. We illustrate how a recently-developed
  CME detection algorithm ('Time Convolution Mapping Method', TCMM,
  Thompson and Young, 2014; http://sipwork.org/TCMM/) can provide improved
  estimates of parameters of the CMEs associated with SEP events.

Title: Results from Persistence Mapping of Solar EUV Data
Authors: Thompson, Barbara J.; Young, C. Alex
Bibcode: 2014AAS...22421838T
Altcode:
  Persistence Mapping is a simple image processing technique that is
  useful for the visualization and depiction of gradually evolving
  or intermittent structures. Persistence Mapping allows the user to
  isolate extreme values in a data set, and is particularly useful for
  the problem of capturing phenomena that are evolving in both space and
  time. While integration or "time lapse" imaging uses the full sample
  (of size N), Persistence Mapping rejects (N-1)/N of the data set and
  identifies the most relevant 1/N values using the following rule:
  if a pixel reaches an extreme value, it retains that value until
  that value is exceeded. The simplest examples isolate minima and
  maxima, and the technique has been used to extract the dynamics in
  long-term evolution of comet tails, erupting material, spicules, and
  EUV dimming regions. The presentation will review the technique and
  discuss scientific results obtained through Persistence Mapping. For
  more information, please see http://sipwork.org/persistence-mapping

Title: The Perihelion Passage of Comet ISON as seen by SDO
Authors: Pesnell, W. D.; Schrijver, C. J.; Boerner, P.; DeRosa, M. L.;
   Liu, W.; Thompson, B. J.
Bibcode: 2013AGUFM.P24A..10P
Altcode:
  Comet ISON will fly through perihelion on November 28, 2013. It is one
  of the largest sungrazing comets to be seen in the Space Age. The Solar
  Dynamics Observatory (SDO) has seen two previous sungrazing comets in
  the extreme ultraviolet channels of the Atmospheric Imaging Assembly
  (AIA). Comet ISON will fly farther from the Sun (perihelion distance
  of 2.7 Rsun compared to 1.15 for Comet Lovejoy), meaning it probes
  a different part of the solar corona, but its larger size should
  provide enough mass to illuminate the path of the nucleus. Based on
  the latest ephemeris, SDO will be able to track Comet ISON through
  the entire perihelion passage by a series of off-point maneuvers. We
  will present the AIA data obtained from the Comet ISON perihelion,
  discussing the differences between Comets ISON and Lovejoy. We will
  then summarize what we have learned from the observations and offer
  some thoughts on what sungrazing comets may reveal about comets,
  the Sun, and their interaction.

Title: Energy Release from Impacting Prominence Material Following
    the 2011 June 7 Eruption
Authors: Gilbert, H. R.; Inglis, A. R.; Mays, M. L.; Ofman, L.;
   Thompson, B. J.; Young, C. A.
Bibcode: 2013ApJ...776L..12G
Altcode: 2013arXiv1309.1769G
  Solar filaments exhibit a range of eruptive-like dynamic activity,
  ranging from the full or partial eruption of the filament mass
  and surrounding magnetic structure as a coronal mass ejection to
  a fully confined or failed eruption. On 2011 June 7, a dramatic
  partial eruption of a filament was observed by multiple instruments
  on board the Solar Dynamics Observatory (SDO) and Solar-Terrestrial
  Relations Observatory. One of the interesting aspects of this event
  is the response of the solar atmosphere as non-escaping material
  falls inward under the influence of gravity. The impact sites show
  clear evidence of brightening in the observed extreme ultraviolet
  wavelengths due to energy release. Two plausible physical mechanisms
  for explaining the brightening are considered: heating of the plasma due
  to the kinetic energy of impacting material compressing the plasma, or
  reconnection between the magnetic field of low-lying loops and the field
  carried by the impacting material. By analyzing the emission of the
  brightenings in several SDO/Atmospheric Imaging Assembly wavelengths,
  and comparing the kinetic energy of the impacting material (7.6 ×
  10<SUP>26</SUP>-5.8 × 10<SUP>27</SUP> erg) to the radiative energy
  (≈1.9 × 10<SUP>25</SUP>-2.5 × 10<SUP>26</SUP> erg), we find
  the dominant mechanism of energy release involved in the observed
  brightening is plasma compression.

Title: Brightenings Caused by Falling Filament Material in the 2011
    June 7 Event
Authors: Gilbert, Holly; Inglis, A.; Ofman, L.; Mays, L. M.; Thompson,
   B. J.; Young, A.
Bibcode: 2013SPD....44...30G
Altcode:
  Solar filaments exhibit a range of eruptive-like dynamic activity from
  the full, or partial, eruption of the filament mass and surrounding
  magnetic structure, as a CME, to a fully confined dynamic evolution or
  ‘failed’ eruption. On 2011 June 7, a dramatic partial eruption of a
  filament was observed by multiple instruments and SDO and STEREO. One
  of the interesting aspects of this partial eruption was the response
  of the surface as non-erupting material fell back under the influence
  of gravity. The impact sites show clear evidence of brightening in the
  observed EUV wavelengths due to energy release by the impact. There
  are two plausible physical mechanisms of the brightening: heating
  of the plasma due to the kinetic energy of the impacting material -
  compression of the plasma, or reconnection between the magnetic field of
  the low-laying loops with the field carried by the impacting material,
  or combination thereof. By analyzing the emission of the brightenings
  in several SDO/AIA wavelength, and comparing the kinetic energy of the
  impacting material (with true velocity determined from triangulation
  of the two STEREO spacecraft) to the radiative energy we provide clues
  for the dominant mechanism of energy release involved in the observed
  brightenings.

Title: The ISS Space Plasma Laboratory: A Proposed Orbital Solar
    Physics Simulation Lab
Authors: Antiochos, Spiro K.; DeVore, C. R.; Thompson, B. J.; Bering,
   E. A., III; Edeen, G.; Carter, M.; Giambusso, M.; Olsen, C. S.;
   Squire, J.; Larson, D.; McFadden, J. P.; Longmier, B.
Bibcode: 2013shin.confE.162A
Altcode:
  We describe a proposed laboratory-experiment research program that will
  answer several fundamental questions concerning the dynamical opening
  and closing of the Sun's magnetic field - the defining property of
  CMEs and eruptive flares. Our experiment is specifically designed to
  address the key questions of the rate of reconnection in the topology of
  a flare or heliospheric current sheet, its burstiness, and the energy
  partition between thermal, kinetic, and particle. Of course, it seems
  completely contradictory to use a laboratory experiment to study an open
  magnetic system, because so far all laboratory plasmas have very solid
  walls. The pioneering feature of our program is that the experiments
  will be performed on the International Space Station (ISS). Only by
  going into space can we obtain the open domain that is absolutely
  essential for studying the opening and closing of coronal flux. Our
  research program will provide the instrumentation infrastructure,
  modeling and solar data expertise and initial scientific understanding
  required to develop the VASIMR® VF-200 high powered plasma source
  into a wall-less, orbiting ISS Space Plasma Laboratory (ISPL) national
  facility. For example, the VF-200 exhaust will simulate conditions
  in the solar corona during CMEs/eruptive flares by creating plasma
  jets in open magnetic field geometries. Such a facility would measure
  quantities in the plasma flow with the goal of measuring magnetic
  reconnection and transport phenomena that should be similar in nature
  to those occurring in the corona and solar wind. Our experiment will
  capture all the effects inherent in a fully 3D magnetic system and
  reproduce some of the physics occurring in the post initiation phase
  of CMEs/eruptive flares. The Aurora Plasma Diagnostics Package (APDP)
  will carry Langmuir probes, a retarding potential analyzer (RPA),
  dc magnetometer, plasma wave detectors, Faraday cups, electrostatic
  analyzers, solid state energetic particle telescope and Ar II and
  broadband imagers.

Title: Brightenings Caused by Falling Filament Material in the 2011
    June 7 Event
Authors: Gilbert, Holly; Inglis, Andrew; Mays, Leila; Ofman, Leon;
   Thompson, Barbara; Young, Alex
Bibcode: 2013shin.confE..74G
Altcode:
  Solar filaments exhibit a range of eruptive-like dynamic activity,
  ranging from the full or partial eruption of the filament mass and
  surrounding magnetic structure as a coronal mass ejection (CME), to
  a fully confined dynamic evolution or 'failed' eruption. On 2011 June
  7, a dramatic partial eruption of a filament was observed by multiple
  instruments on SDO and STEREO. One of the interesting aspects of this
  partial eruption is the response of the solar atmosphere as non-escaping
  material falls inward under the influence of gravity. The impact sites
  show clear evidence of brightening in the observed EUV wavelengths due
  to energy release. Two plausible physical mechanisms explaining the
  brightening are considered: heating of the plasma due to the kinetic
  energy of impacting material compressing the plasma, or reconnection
  between the magnetic field of the low-lying loops and the field carried
  by the impacting material. By analyzing the emission of the brightenings
  in several SDO/AIA wavelengths, and comparing the kinetic energy of the
  impacting material ((2.12-60.4) - 10^26 ergs) to the radiative energy
  ( 10^25 ergs) we find the dominant mechanism of energy release involved
  in the observed brightening is plasma compression.

Title: Exploring the Network of SDO Science
Authors: Pesnell, W. Dean; Thompson, Barbara
Bibcode: 2013enss.conf.....P
Altcode:
  Living With a Star's Solar Dynamics Observatory invites you to its
  2013 Science Workshop to be held March 3-8, 2013 at the Hyatt Regency
  Chesapeake Bay in Cambridge, MD (http://chesapeakebay.hyatt.com/). The
  workshop is a follow-on to the "Many Spectra of Solar Activity" workshop
  held May 1-5, 2011 in Squaw Valley, CA. <P />Scientific sessions will
  feature a broad spectrum of science topics fundamental to SDO's science
  investigations: Atmospheric Imaging Assembly (AIA), EUV Variability
  Experiment (EVE), and Helioseismic and Magnetic Imager (HMI), as well
  as the overlap between SDO and other scientific missions and activities.

Title: Understanding Solar Eruptive Events
Authors: Mason, James P.; Hock, Rachel A.; Woods, Thomas N.; Thompson,
   Barbara J.; Webb, David F.; Caspi, Amir
Bibcode: 2013enss.confE.138M
Altcode:
  Coronal dimming is studied using data from the EUV Variability
  Experiment (EVE) and the Atmospheric Imaging Assembly (AIA), both
  onboard the Solar Dynamics Observatory (SDO). Dimming can be caused
  by a number of physical processes, including mass loss (e.g. coronal
  mass ejections), obscuration of bright features (e.g. flaring loops)
  by dark features (e.g. filament eruptions), global scale waves, and
  changes of temperature in the emitting plasma. Each of these processes
  have unique spectral signatures, which EVE and AIA are well suited
  to observe. We are building a method for isolating the signature
  indicative of mass loss, which is thought to be correlated with the
  kinetics of coronal mass ejections. Our analysis of the M9 flare on
  August 4, 2011 are shown as an example of all four of these physical
  processes and their spectral signatures.

Title: STEREO Observations of Fast Magnetosonic Waves in the Extended
    Solar Corona Associated with EIT/EUV Waves
Authors: Kwon, Ryun-Young; Ofman, Leon; Olmedo, Oscar; Kramar, Maxim;
   Davila, Joseph M.; Thompson, Barbara J.; Cho, Kyung-Suk
Bibcode: 2013ApJ...766...55K
Altcode:
  We report white-light observations of a fast magnetosonic wave
  associated with a coronal mass ejection observed by STEREO/SECCHI/COR1
  inner coronagraphs on 2011 August 4. The wave front is observed in the
  form of density compression passing through various coronal regions such
  as quiet/active corona, coronal holes, and streamers. Together with
  measured electron densities determined with STEREO COR1 and Extreme
  UltraViolet Imager (EUVI) data, we use our kinematic measurements of
  the wave front to calculate coronal magnetic fields and find that the
  measured speeds are consistent with characteristic fast magnetosonic
  speeds in the corona. In addition, the wave front turns out to be
  the upper coronal counterpart of the EIT wave observed by STEREO
  EUVI traveling against the solar coronal disk; moreover, stationary
  fronts of the EIT wave are found to be located at the footpoints of
  deflected streamers and boundaries of coronal holes, after the wave
  front in the upper solar corona passes through open magnetic field
  lines in the streamers. Our findings suggest that the observed EIT
  wave should be in fact a fast magnetosonic shock/wave traveling in
  the inhomogeneous solar corona, as part of the fast magnetosonic wave
  propagating in the extended solar corona.

Title: Investigating Coronal Activity by Release Using Sublimation
Authors: Moore, T. E.; Bryans, P.; Pesnell, W. D.; Thompson, B. J.
Bibcode: 2012AGUFMSH21D..05M
Altcode:
  Plasma tails left by sun-grazing comets are visible in EUV, expanding
  their traditional role as "windsocks" into the low corona and serving
  as natural "chemical release" experiments. SDO obtained spectrally
  resolved video imagery of passages as close as 0.15 Rs to the solar
  photosphere at 12 sec frame cadence. Vaporized cometary materials
  form sublimation trails or "subtrails" that persist as long as 20
  min. in 13.1 and 17.1 nm channels. Striation along local magnetic flux
  tubes implies filamentation of the visible plasma, and the subtrails
  exhibit substantial deviations from the comet orbital track. These
  reveal coronal winds and shears with velocities that are comparable to
  the comet velocity of up to 600 km/s. We analyze the likely origins
  and directionality of these winds and their implications for coronal
  heating in the altitude range where ion-neutral collision mean free
  paths are longer than the gyro radius but shorter than the atmospheric
  scale height, that is, the solar transition region. With active impact
  or photo-ionization, and charge exchange, the inferred super-thermal,
  sub-Alfvenic ion-neutral relative velocities will lead to ion pick-up
  distributions that decay or relax into "kappa" distributions with
  super-thermal power law tails that are relevant to the formation of
  the corona.

Title: EUV Dimmings: Formation Mechanisms and Associated Phenomena
Authors: Thompson, B. J.; Mays, M. L.; West, M. J.
Bibcode: 2012AGUFMSH44A..03T
Altcode:
  Large-scale coronal EUV dimmings, developing on timescales of minutes
  to hours in association with a flare or filament eruption, are known
  to exhibit a high correlation with coronal mass ejections. While most
  observations indicate that the decrease in emission in a dimming is due,
  at least in part, to a density decrease, a complete understanding
  requires us to examine at least four mechanisms that have been
  observed to cause darkened regions in the corona: 1) mass loss, 2)
  cooling, 3) heating, and 4) absorption/obscuration. Recent advances in
  automatic detection, observations with improved cadence and resolution,
  multi-viewpoint imaging, and spectroscopic studies have continued to
  shed light on dimming formation, evolution, and recovery. However,
  there are still some outstanding questions, including 1) Why do some
  CMEs show dimming and some do not? 2) What determines the location of
  a dimming? 3) What determines the temporal evolution of a dimming? 4)
  How does the post-eruption dimming connect to the ICME? 5) What is the
  relationship between dimmings and other CME-associated phenomena? The
  talk will emphasize the different formation mechanisms of dimmings
  and their relationship to CMEs and CME-associated phenomena.

Title: Erratum: "SDO/AIA Observation of Kelvin-Helmholtz Instability
    in the Solar Corona" <A href="/abs/2011ApJ...734L..11O">(2011, ApJ,
    734, L11)</A>
Authors: Ofman, L.; Thompson, B. J.
Bibcode: 2012ApJ...760L..19O
Altcode:
  No abstract at ADS

Title: Vibrational Shift of Adsorbed Carbon Dioxide Within a
    Metal-Organic Framework
Authors: Fitzgerald, S.; Pierce, C.; Schloss, J.; Thompson, B.;
   Rowsell, J.
Bibcode: 2012mss..confEMJ11F
Altcode:
  There is much interest in a class of materials known as Metal-Organic
  Frameworks (MOFs). While practical applications center on hydrogen
  storage and carbon sequestration, these highly porous, crystalline
  materials also provide an excellent opportunity for performing matrix
  isolation experiments. In this talk we will present data on MOF-74,
  a honey-comb structure consisting of metal-oxide units linked by
  aromatic rings. Infrared spectra show that for a series of different
  metal cations, Mn<SUP>2+</SUP>, Fe<SUP>2+</SUP>, Co<SUP>2+</SUP>,
  Ni<SUP>2+</SUP>, and Zn<SUP>2+</SUP> the vibrational modes of adsorbed
  CO<SUB>2</SUB> are all red shifted relative to the gas phase values. In
  contrast the ν<SUB>3</SUB> mode of CO<SUB>2</SUB> adsorbed within
  the Mg version of MOF-74 is unique in showing a blue shift. It is
  accompanied by broader sidebands associated with librational or center
  of mass motion of the adsorbed CO<SUB>2</SUB>. Spectra obtained below
  100 K show the emergence of a second ν<SUB>3</SUB> band indicating a
  further distortion of the CO<SUB>2</SUB> molecule. These results will
  be discussed in terms of the interaction mechanisms of the different
  metal cations and in particular the fact that the Mg version of MOF-74
  has a very strong affinity for CO<SUB>2</SUB> with a binding enenergy
  of 47 kJ/mol, more than 5 kJ/mol greater than any other MOF.

Title: Comparison of Prominence Structures with Instances of Flux
    Rope CMEs in STEREO Data
Authors: Rager, Amy; Thompson, B. J.; Antiochos, S. K.; Thernisien,
   A.; Thompson, W. T.
Bibcode: 2012AAS...22020004R
Altcode:
  STEREO A and B CME data have been visually searched for instances
  of flux ropes, signified by a concave outward cavity feature in
  the COR1 coronagraph. The flux rope events selected were observed
  by both spacecraft, and also had visible prominences in both EUVI-A
  and EUVI-B. The appearance of a flux rope was compared to the angle
  of the inferred magnetic neutral line of the CME to discover if a
  relationship existed. The GCS CME flux rope model was fit to the COR1
  data, allowing for a clearer representation of the flux rope structure
  to compare with the magnetic neutral line.

Title: Modeling waves, flows, and instabilities produced by impulsive
    events in coronal active regions
Authors: Ofman, L.; Liu, W.; Wang, T. J.; Davila, J. M.; Thompson,
   B. J.
Bibcode: 2012decs.confE..73O
Altcode:
  Recent high-resolution observations by SDO/AIA combined with spectral
  data from Hinode provide insights into the properties of MHD waves,
  flows, and instabilities in coronal active region plasma and
  their connection with impulsive energy release. Shear flow driven
  instabilities, such as the Kelvin-Helmholtz (KH) instability were
  only recently detected in detail in the corona. I will present recent
  results of 3D MHD models of slow and fast magnetosonic waves in active
  regions excited by jets and quasi-periodic flows driven by micro-flares
  at loops' footpoints. I will discuss models of super-fast magnetosonic
  waves detected recently by SDO/AIA. I will also discuss models of global
  (EIT) waves, and KH instabilities driven by CMEs. The relations between
  waves, flows, instabilities, and impulsive events such as flares and
  CMEs are becoming apparent thanks to the combination of observational
  data analysis and the 3D MHD modeling. Understanding these relations
  is useful for coronal seismology and for tracing the flow of energy
  from the transition region to the corona.

Title: The Solar Dynamics Observatory (SDO)
Authors: Pesnell, W. Dean; Thompson, B. J.; Chamberlin, P. C.
Bibcode: 2012SoPh..275....3P
Altcode:
  The Solar Dynamics Observatory (SDO) was launched on 11 February 2010 at
  15:23 UT from Kennedy Space Center aboard an Atlas V 401 (AV-021) launch
  vehicle. A series of apogee-motor firings lifted SDO from an initial
  geosynchronous transfer orbit into a circular geosynchronous orbit
  inclined by 28° about the longitude of the SDO-dedicated ground station
  in New Mexico. SDO began returning science data on 1 May 2010. SDO
  is the first space-weather mission in NASA's Living With a Star (LWS)
  Program. SDO's main goal is to understand, driving toward a predictive
  capability, those solar variations that influence life on Earth and
  humanity's technological systems. The SDO science investigations will
  determine how the Sun's magnetic field is generated and structured,
  how this stored magnetic energy is released into the heliosphere and
  geospace as the solar wind, energetic particles, and variations in the
  solar irradiance. Insights gained from SDO investigations will also
  lead to an increased understanding of the role that solar variability
  plays in changes in Earth's atmospheric chemistry and climate. The
  SDO mission includes three scientific investigations (the Atmospheric
  Imaging Assembly (AIA), Extreme Ultraviolet Variability Experiment
  (EVE), and Helioseismic and Magnetic Imager (HMI)), a spacecraft bus,
  and a dedicated ground station to handle the telemetry. The Goddard
  Space Flight Center built and will operate the spacecraft during
  its planned five-year mission life; this includes: commanding the
  spacecraft, receiving the science data, and forwarding that data to the
  science teams. The science investigations teams at Stanford University,
  Lockheed Martin Solar Astrophysics Laboratory (LMSAL), and University
  of Colorado Laboratory for Atmospheric and Space Physics (LASP) will
  process, analyze, distribute, and archive the science data. We will
  describe the building of SDO and the science that it will provide
  to NASA.

Title: The Sun-Earth Connection near Solar Minimum: Placing it
    into Context
Authors: Bisi, Mario M.; Thompson, Barbara J.; Emery, Barbara A.;
   Gibson, Sarah E.; Leibacher, John; van Driel-Gesztelyi, Lidia
Bibcode: 2011SoPh..274....1B
Altcode:
  No abstract at ADS

Title: A Snapshot of the Sun Near Solar Minimum: The Whole Heliosphere
    Interval
Authors: Thompson, Barbara J.; Gibson, Sarah E.; Schroeder, Peter C.;
   Webb, David F.; Arge, Charles N.; Bisi, Mario M.; de Toma, Giuliana;
   Emery, Barbara A.; Galvin, Antoinette B.; Haber, Deborah A.; Jackson,
   Bernard V.; Jensen, Elizabeth A.; Leamon, Robert J.; Lei, Jiuhou;
   Manoharan, Periasamy K.; Mays, M. Leila; McIntosh, Patrick S.; Petrie,
   Gordon J. D.; Plunkett, Simon P.; Qian, Liying; Riley, Peter; Suess,
   Steven T.; Tokumaru, Munetoshi; Welsch, Brian T.; Woods, Thomas N.
Bibcode: 2011SoPh..274...29T
Altcode: 2011SoPh..tmp..413T
  We present an overview of the data and models collected for the
  Whole Heliosphere Interval, an international campaign to study the
  three-dimensional solar-heliospheric-planetary connected system near
  solar minimum. The data and models correspond to solar Carrington
  Rotation 2068 (20 March - 16 April 2008) extending from below the
  solar photosphere, through interplanetary space, and down to Earth's
  mesosphere. Nearly 200 people participated in aspects of WHI studies,
  analyzing and interpreting data from nearly 100 instruments and
  models in order to elucidate the physics of fundamental heliophysical
  processes. The solar and inner heliospheric data showed structure
  consistent with the declining phase of the solar cycle. A closely
  spaced cluster of low-latitude active regions was responsible for an
  increased level of magnetic activity, while a highly warped current
  sheet dominated heliospheric structure. The geospace data revealed an
  unusually high level of activity, driven primarily by the periodic
  impingement of high-speed streams. The WHI studies traced the solar
  activity and structure into the heliosphere and geospace, and provided
  new insight into the nature of the interconnected heliophysical system
  near solar minimum.

Title: The Whole Heliosphere Interval in the Context of a Long and
Structured Solar Minimum: An Overview from Sun to Earth
Authors: Gibson, S. E.; de Toma, G.; Emery, B.; Riley, P.; Zhao, L.;
   Elsworth, Y.; Leamon, R. J.; Lei, J.; McIntosh, S.; Mewaldt, R. A.;
   Thompson, B. J.; Webb, D.
Bibcode: 2011SoPh..274....5G
Altcode: 2011SoPh..tmp..427G
  Throughout months of extremely low solar activity during the recent
  extended solar-cycle minimum, structural evolution continued to be
  observed from the Sun through the solar wind and to the Earth. In
  2008, the presence of long-lived and large low-latitude coronal holes
  meant that geospace was periodically impacted by high-speed streams,
  even though solar irradiance, activity, and interplanetary magnetic
  fields had reached levels as low as, or lower than, observed in past
  minima. This time period, which includes the first Whole Heliosphere
  Interval (WHI 1: Carrington Rotation (CR) 2068), illustrates the
  effects of fast solar-wind streams on the Earth in an otherwise quiet
  heliosphere. By the end of 2008, sunspots and solar irradiance had
  reached their lowest levels for this minimum (e.g., WHI 2: CR 2078),
  and continued solar magnetic-flux evolution had led to a flattening
  of the heliospheric current sheet and the decay of the low-latitude
  coronal holes and associated Earth-intersecting high-speed solar-wind
  streams. As the new solar cycle slowly began, solar-wind and geospace
  observables stayed low or continued to decline, reaching very low
  levels by June - July 2009. At this point (e.g., WHI 3: CR 2085) the
  Sun-Earth system, taken as a whole, was at its quietest. In this article
  we present an overview of observations that span the period 2008 -
  2009, with highlighted discussion of CRs 2068, 2078, and 2085. We show
  side-by-side observables from the Sun's interior through its surface and
  atmosphere, through the solar wind and heliosphere and to the Earth's
  space environment and upper atmosphere, and reference detailed studies
  of these various regimes within this topical issue and elsewhere.

Title: Solar Dynamics and Magnetism from the Interior to the
    Atmosphere
Authors: Pesnell, W. Dean; Thompson, Barbara
Bibcode: 2011sdmi.conf.....P
Altcode:
  The goal of the workshop is to discuss recent advances and new problems
  in the exploration of the Sun's interior structure, solar dynamics and
  dynamo, mechanisms of sunspot and active regions formation, sources of
  solar irradiance variations, and links between the subsurface dynamics,
  flaring and CME activity. <P />NASA's Solar Dynamics Observatory (SDO)
  mission is providing a large amount of new data on solar dynamics and
  magnetic activities during the rising phase of the current and highly
  unusual solar cycle. These data are complemented by the continuing
  SOHO mission, and by ground-based observatories that include the GONG
  helioseismology network and the New Solar Telescope. This unprecedented
  amount of data provides a unique opportunity for multi-instrument
  investigations that address fundamental problems of the origin of
  solar magnetic activity at various spatial and temporal scales. <P
  />The data is being used to develop new methods for forecasting
  solar cycles, emergence and evolution of active regions and their
  flaring and CME activity. <P />The scientific program will begin
  on Monday, October 31 at 9 AM, and conclude on Friday, November
  4 at 1PM. Abstracts are solicited on the following topics: <P />-
  "Local and Global Helioseismology" - "Large-Scale Dynamics, Magnetism
  and Dynamo" - "Emerging Magnetic Flux and Subsurface Dynamics" -
  "Formation, Structure and Evolution of Sunspots and Active Regions" -
  "Numerical Simulations and Laboratory Experiments" - "Observations of
  the Solar Dynamics and Magnetism" - "Links between the Solar Interior
  and Atmosphere" - "Sources of Spectral and Total Irradiance Variations"
  - "Dynamics and Magnetic Topology of Flares and CMEs" <P />The workshop
  program will include invited and contributed talks, as well as poster
  sessions. On the last day, 4 splinter working group meetings will be
  organized: <P />1. Helioseismology (organizers R. Bogart, R. Komm,
  A. Kosovichev) 2. Vector Magnetometry (organizer T. Hoeksema and
  A. Pevtsov) 3. Feature Recognition, and Data Distribution and Access
  (organizers P. Martens and N. Hurlburt) 4. Numerical Simulations and
  Modeling (organizers N. Mansour and I. Kitiashvili)

Title: SDO/AIA Observation of Kelvin-Helmholtz Instability in the
    Solar Corona
Authors: Ofman, L.; Thompson, B. J.
Bibcode: 2011ApJ...734L..11O
Altcode: 2011arXiv1101.4249O
  We present observations of the formation, propagation, and decay of
  vortex-shaped features in coronal images from the Solar Dynamics
  Observatory associated with an eruption starting at about 2:30
  UT on 2010 April 8. The series of vortices were formed along the
  interface between an erupting (dimming) region and the surrounding
  corona. They ranged in size from several to 10 arcsec and traveled
  along the interface at 6-14 km s<SUP>-1</SUP>. The features were
  clearly visible in six out of the seven different EUV wave bands of
  the Atmospheric Imaging Assembly. Based on the structure, formation,
  propagation, and decay of these features, we identified the event as
  the first observation of the Kelvin-Helmholtz instability (KHI) in the
  corona in EUV. The interpretation is supported by linear analysis and
  by a nonlinear 2.5-dimensional magnetohydrodynamic model of KHI. We
  conclude that the instability is driven by the velocity shear between
  the erupting and closed magnetic field of the coronal mass ejection. The
  shear-flow-driven instability can play an important role in energy
  transfer processes in coronal plasma.

Title: Molecular Hydrogen Interactions Within Metal-Organic Frameworks
Authors: Fitzgerald, S.; Pierce, C.; Schloss, J.; Thompson, B.;
   Rowsell, J.
Bibcode: 2011mss..confEMJ10F
Altcode:
  There is much interest in understanding the details of molecular
  hydrogen physisorption within highly porous materials that could be
  used for hydrogen storage applications. Unfortunately, the structures of
  the most promising materials are too complex for ab inito calculations
  and DFT models are notoriously unreliable for weak interactions. A new
  approach based on so-called van der Waals DFT has been proposed for
  explaining the behavior of molecular hydrogen within metal-organic
  frameworks.<SUP>1</SUP> In this talk we will present IR spectra of
  adsorbed hydrogen within a series of isostructural MOFs containing
  Mg<SUP>2+</SUP> and various first-row transition metal cations. The
  data clearly show that H<SUB>2</SUB> binds first at an open metal
  site, with a large vibrational redshift that correlates with the
  magnitude of the site binding energy. These spectra show minimal
  effects due to H<SUB>2</SUB>\cdot\cdotCdotH<SUB>2</SUB> interactions
  and are significantly different from the recent findings of the Chabal
  group.<SUP>1</SUP> After collecting spectra over a wide range of
  temperature and H<SUB>2</SUB> pressure, we could only reproduce their
  experimental observations by exposing samples to moist air, which is
  well-known to cause occupation of the open metal sites by water. This
  calls into question the appropriateness of the van der Waals DFT
  models that were used to support their interpretations.<SUP>1</SUP>
  We are hopeful that the spectra we present will inspire improved
  parametrization of such advanced computational models, or prompt the
  development of superior ones. 1. Nijjem et al., J. Am. Chem. Soc. 132,
  14834 (2010).

Title: Pulsed Flows Along a Cusp Structure Observed with SDO/AIA
Authors: Thompson, Barbara; Démoulin, P.; Mandrini, C.; Mays, M.;
   Ofman, L.; Van Driel-Gesztelyi, L.; Viall, N.
Bibcode: 2011SPD....42.2117T
Altcode: 2011BAAS..43S.2117T
  We present observations of a cusp-shaped structure that formed after
  a flare and coronal mass ejection on 14 February 2011. Throughout
  the evolution of the cusp structure, blob features up to a few Mm in
  size were observed flowing along the legs and stalk of the cusp at
  projected speeds ranging from 50 to 150 km/sec. Around two dozen blob
  features, on order of 1 - 3 minutes apart, were tracked in multiple
  AIA EUV wavelengths. The blobs flowed outward (away from the Sun)
  along the cusp stalk, and most of the observed speeds were either
  constant or decelerating. We attempt to reconstruct the 3-D magnetic
  field of the evolving structure, discuss the possible drivers of the
  flows (including pulsed reconnection and tearing mode instability),
  and compare the observations to studies of pulsed reconnection and
  blob flows in the solar wind and the Earth's magnetosphere.

Title: Accessing SDO Data : The Poster
Authors: Hourcle, Joseph; Addison, K.; Bogart, R.; Chamberlin, P.;
   Freeland, S.; Hughitt, V. K.; Ireland, J.; Maddox, M.; Mueller, D.;
   Somani, A.; Sommers, J.; Thompson, B.; solar physics data community,
   The
Bibcode: 2011SPD....42.2130H
Altcode: 2011BAAS..43S.2130H
  As the data from SDO are useful for a variety of purposes, including
  solar physics, helioseismology, atmospheric science, space weather
  forecasting, education and public outreach, a wide variety of tools
  have been development to cater to the different needs of the various
  groups. Systems have been developed for pipeline processing, searching,
  browsing, subsetting, or simply just moving around large volumes
  of data. <P />We present a quick overview of the different systems
  that can be used to access SDO data including (J)Helioviewer, the
  Heliophysics Event Knowledgebase (HEK), the Virtual Solar Observatory
  (VSO), the Integrated Space Weather Analysis System (iSWA), the
  Data Record Management System (DRMS), and various websites. We cover
  web-based applications, application programming interfaces (APIs),
  and IDL command line tools. <P />This poster serves as a supplement
  to the oral presentation as a place to distribute information about
  the various interfaces and to collect feedback about any unmet needs
  for data access.

Title: The International Space Weather Initiative (ISWI)
Authors: Davila, Joseph M.; Gopalswamy, Nat; Thompson, Barbara J.;
   Bogdan, Tom; Hapgood, Mike
Bibcode: 2011sswh.book..375D
Altcode:
  No abstract at ADS

Title: SDO/AIA Observation of Kelvin-Helmholtz Instability in the
    Solar Corona associated with CME
Authors: Ofman, L.; Thompson, B. J.
Bibcode: 2010AGUFMSH14A..02O
Altcode:
  We present observations of the formation, propagation and decay
  of vortex-shaped features in coronal images from the Solar Dynamics
  Observatory (SDO) associated with Coronal Mass Ejection (CME) at about
  2:34UT on Apr 8, 2010. The series of vortices are seen at 3:20UT
  to 3:37UT formed along the interface between erupting (dimming)
  region and the surrounding corona and ranged in size from several
  to ten arcseconds, traveling along the interface at approximately
  5 km/sec. The features are clearly visible in five out of the six
  different EUV wavebands of the Atmospheric Imaging Assembly (AIA). Based
  on the structure, formation, propagation and decay of these features, we
  conclude that these are the first observations of the Kelvin-Helmholtz
  (KH) instability in the corona. The KH instability is likely driven
  by the velocity shear between the erupting and closed magnetic field
  regions. We compare the dynamics and structure of SDO/AIA observation
  to an MHD model of KH instability in the nonlinear stage in magnetized
  plasma, and find good agreement.

Title: The Many Ways to Access SDO Data
Authors: Thompson, B. J.; Hourcle, J. A.; Addison, K.; Bogart, R. S.;
   Chamberlin, P. C.; Dietert, H.; Freeland, S. L.; Hughitt, V. K.;
   Ireland, J.; Mueller, D.; Somani, A.; Sommers, J.
Bibcode: 2010AGUFMSH23C1865T
Altcode:
  To solve the issue of dealing with the large volume of data available
  from AIA, there are a number of ways to get access to SDO data. With
  Helioviewer, the Heliophysics Event Knowledgebase, the Virtual Solar
  Observatory, and the PI-provided tools, scientists and other interested
  parties have a number of ways to find and obtain data of interest. We
  present an overview of the differences between the various systems,
  and a flow chart to help determine which one might be of the most
  benefit for a given situation.

Title: Observed Core of a Gradual Solar Energetic Particle Event
Authors: Kocharov, L.; Reiner, M. J.; Klassen, A.; Thompson, B. J.;
   Valtonen, E.
Bibcode: 2010ApJ...725.2262K
Altcode:
  Using space-borne particle and EUV detection and radio spectrograms
  from both ground-based and space-borne instruments, we study the first
  phase of the major solar energetic particle (SEP) event associated with
  the western solar flare and fast and wide coronal mass ejection (CME) on
  2000 April 4. The SEP event being observed at the magnetic connection to
  the eruption's center starts with deka-MeV nucl<SUP>-1</SUP> helium- and
  relativistic electron-rich production from coronal sources identified
  with the electromagnetic diagnostics and the SEP event modeling. The
  broadband observations and modeling of the initial phase of the
  "well-connected" major SEP event support the idea that acceleration
  of SEPs starts in the helium-rich plasma of the eruption's core in
  association with coronal shocks and magnetic reconnections caused by the
  CME liftoff, and that the coronal component dominates during the first
  hour of the SEP event considered, not yet being shielded by the CME bow
  shock in the solar wind. The first phase of the SEP event is followed
  by a second phase of SEP production associated with a decelerating
  CME-driven shock wave in the solar wind, which accelerates ions from
  a distinct, helium-poor seed particle population that may originate
  from the CME interaction with a coronal streamer.

Title: a Three-Dimensional View of Major Solar Energetic Particle
    Events
Authors: Kocharov, L. G.; Valtonen, E.; Thompson, B. J.; Reiner,
   M. J.; Klassen, A.
Bibcode: 2010AGUFMSH42B..04K
Altcode:
  Using SOHO particle and EUV detection and radio spectrograms from both
  ground-based and spaceborne instruments, we study the first phase
  of two major solar energetic particle (SEP) events associated with
  solar eruptions centered at different solar longitudes. A major solar
  energetic particle (SEP) event observed on 4 April 2000 was associated
  with western solar flare and fast and wide coronal mass ejection
  (CME). The SEP event near the eruption's center starts with deka-MeV/n
  helium- and relativistic electron- rich production from coronal sources
  identified with the electromagnetic diagnostics. Observations of the
  initial phase of the "well-connected" major SEP event support the
  idea that acceleration of SEPs starts in the helium-rich plasma of
  the eruption's core well behind the CME leading edge, in association
  with coronal shocks and/or magnetic reconnection caused by the CME
  liftoff; and those "coronal" components dominate during the first ~1.5
  hour of the SEP event, not yet being hidden by the CME-bow shock in
  solar wind. The 12 September 2000 eruption's center was angle-distant
  with respect to the SOHO-connected heliolongitude. The event began
  with a first-phase, hard-spectrum SEP production that was extremely
  poor in helium, and onset of the first stage of the SEP event as
  observed on SOHO was delayed by an extra half hour, compared to the
  "well-connected" event of 4 April 2000. At magnetic connection to
  the eruption's periphery, onset of SEP emission is delayed for a
  time of the lateral expansion that is visualized by global coronal
  (EIT) waves. In both cases, the initial, coronal phase of SEP event
  is followed by the second-phase SEP production associated with a
  decelerating CME-driven shock wave in solar wind, which accelerates
  deka-MeV/n ions from a helium-poor particle population for ~6--12 hours,
  until the interplanetary shock slows down to below 1000 km/s. Based
  on these and other SOHO observations, we discuss what findings we can
  expect from STEREO in the SOHO era perspective.

Title: Escape of O<SUP>+</SUP> through the distant tail plasma sheet
Authors: Kistler, L. M.; Galvin, A. B.; Popecki, M. A.; Simunac,
   K. D. C.; Farrugia, C.; Moebius, E.; Lee, M. A.; Blush, L. M.;
   Bochsler, P.; Wurz, P.; Klecker, B.; Wimmer-Schweingruber, R. F.;
   Opitz, A.; Sauvaud, J. -A.; Thompson, B.; Russell, C. T.
Bibcode: 2010GeoRL..3721101K
Altcode:
  In February 2007, the STEREO-B spacecraft encountered the
  magnetosheath, plasma sheet and plasma sheet boundary layer from
  about 200 R<SUB>E</SUB> to 300 R<SUB>E</SUB> downtail. This time
  period was during solar minimum, and there was no storm activity
  during this month. Using data from the PLASTIC instrument, we find
  that even during quiet times, O<SUP>+</SUP> is a constant feature of
  the deep magnetotail, with an O<SUP>+</SUP> density of about 15% of
  the O<SUP>+</SUP> density in the near-earth plasma sheet for similar
  conditions. The tailward flux of the O<SUP>+</SUP> is similar to the
  flux of O<SUP>+</SUP> beams that have been observed in the lobe/mantle
  region of the deep tail. The total outflow rate of the O<SUP>+</SUP>
  down the plasma sheet is 1.1 × 10<SUP>24</SUP> ions/s, which is 10%
  of the total outflow rate of 1 × 10<SUP>25</SUP> ions/s, and of the
  same order as the estimated loss from dayside transport.

Title: Whole Heliosphere Interval: Overview of JD16
Authors: Webb, David F.; Gibson, Sarah E.; Thompson, Barbara J.
Bibcode: 2010HiA....15..471W
Altcode:
  The Whole Heliosphere Interval is an international observing and
  modeling effort to characterize the three-dimensional interconnected
  solar-heliospheric-planetary system, i.e., the “heliophysical”
  system. WHI was part of the International Heliophysical Year, on the
  50th anniversary of the International Geophysical Year, and benefited
  from hundreds of observatories and instruments participating in IHY
  activities. WHI describes the 3-D heliosphere originating from solar
  Carrington Rotation 2068, March 20-April 16, 2008. The focus of IAU JD16
  was on analyses of observations obtained during WHI, and simulations
  and modeling involving those data and that period. Consideration of
  the WHI interval in the context of surrounding solar rotations and/or
  compared to last solar minimum was also encouraged. Our goal was to
  identify connections and commonalities between the various regions of
  the heliosphere.

Title: The Whole Heliosphere Interval in the Context of the Current
    Solar Minimum
Authors: Gibson, S. E.; Webb, D. F.; Thompson, B. J.
Bibcode: 2010ASPC..428..223G
Altcode:
  The current solar minimum may not be "peculiar" when considered on
  scales of a century or more. However, the opportunity for discovery
  yielded by its extended nature, in combination with the abundance of
  modern observations, cannot be overstated. In this paper, we describe
  the Whole Heliosphere Interval (WHI), an in-depth study of the Sun-Earth
  system for a solar rotation in March/April 2008. We discuss how WHI
  fits within the broader context of the current deep, long, and complex
  solar minimum.

Title: Molecular Hydrogen Adsorption in Metal-Organic Frameworks
Authors: Fitzgerald, S.; Friedman, M.; Gotdank, J.; Thompson, B.;
   Rowsell, J.
Bibcode: 2010mss..confEFB01F
Altcode:
  There is presently much interest in studying hydrogen storage materials
  for fuel cell applications. A promising class of physisorbents for
  this purpose is metal-organic frameworks, which consist of metal ions
  bridged by rigid organic molecules that assemble as highly porous
  molecular "scaffolds". We will report on a novel application of
  diffuse reflectance IR spectroscopy to probe the ro-vibrational modes
  of molecular hydrogen adsorbed within these materials. Experiments
  with H<SUB>2</SUB>, HD, and D<SUB>2</SUB> illustrate the importance
  of quantum mechanical considerations and the necessity for rotational
  translational coupling models. Data reveal the propensity of exposed
  metals sites to produce some of the largest recorded interaction
  energies with adsorbed hydrogen. This leads to large frequency redshifts
  in the H<SUB>2</SUB> vibrational mode (65 - 130 cm<SUP>-1</SUP>) along
  with a dramatic increase in the overtone intensity. The magnitude of
  the effect is shown to follow the Irving-Williams sequence in which
  the frequency shift for H<SUB>2</SUB> bound to Ni<SUP>2+</SUP> &gt;
  Co<SUP>2+</SUP> &gt; Zn<SUP>2+</SUP>.

Title: What Do High-resolution EIT Waves Tell Us About CMEs?
Authors: Thompson, Barbara; Biesecker, D. A.; Nitta, N.; Ofman, L.;
   West, M. J.
Bibcode: 2010AAS...21640229T
Altcode:
  Although many studies have demonstrated that some coronal waves are
  not generated by coronal mass ejections, we have learned a great
  deal about the ability of coronal mass ejections to drive large-scale
  coronal waves, also called "EIT waves." We present new results based
  on EIT wave amplitude, timing, speed, and direction of propagation,
  with respect to their correlation with CME-related dimmings, speeds,
  locations and widths. Furthermore, we demonstrate the ability to
  correlate different aspects of EIT waves with some of the observed
  structure of CMEs observed in coronagraph data. Finally, we expand
  on the discussion of the types of wave modes that can be generated
  by a coronal mass ejection, and how these observations can serve as a
  diagnostic of the type of impulse a CME can deliver to the surrounding
  corona. These diagnostics are obtained by examining the motion of
  individual field lines, requiring high-resolution observations like
  those provided by TRACE and SDO/AIA.

Title: Kinetic temperatures of iron ions in the solar wind observed
    with STEREO/PLASTIC
Authors: Bochsler, Peter; Lee, Martin A.; Karrer, Reto; Popecki,
   Mark A.; Galvin, Antoinette B.; Kistler, Lynn M.; Möbius, Eberhard;
   Farrugia, Charles J.; Kucharek, Harald; Simunac, Kristin D. C.;
   Blush, Lisa M.; Daoudi, Hagar; Wurz, Peter; Klecker, Berndt;
   Wimmer-Schweingruber, Robert F.; Thompson, Barbara; Luhmann, Janet G.;
   Jian, Lan K.; Russell, Christopher T.; Opitz, Andrea
Bibcode: 2010AIPC.1216..257B
Altcode:
  STEREO/PLASTIC provides detailed information on the three-dimensional
  velocity distributions of solar wind iron ions with a time
  resolution of 5 minutes. In general the distributions at 1 AU contain
  complicated structures showing persistence over several records,
  i.e., over intervals of up to 30 minutes, but no clear correlation
  of the properties of these distributions with the direction of the
  ambient magnetic field is evident. We have performed a statistical
  analysis using nearly 9000 observations. Iron ions follow the
  same trends as protons, alpha particles, and electrons: The ratio
  T<SUB>⊥</SUB>/T<SUB>||</SUB> seems to be limited by the ion cyclotron
  instability, whereas T<SUB>||</SUB>/T<SUB>⊥</SUB> is bounded by the
  firehose instability.

Title: Mini-RF Observations of a Sample of Large Lunar Pyroclastic
    Deposits
Authors: Carter, L. M.; Gillis-Davis, J. J.; Bussey, D. B. J.; Spudis,
   P. D.; Neish, C. D.; Thompson, B. J.; Patterson, G. W.; Raney, R. K.;
   Mini-Rf Science Team
Bibcode: 2010LPI....41.1563C
Altcode:
  We present new radar data of large lunar pyroclastic deposits obtained
  using the Mini-RF instruments on Chandrayaan-1 and Lunar Reconnaissance
  Orbiter, including the Orientale pyroclastic.

Title: Using Mini-RF to Investigate the Anomalous UVVIS Spectrum in
    the Apollo and Plato Region
Authors: Trang, D.; Gillis-Davis, J. J.; Williams, K.; Bussey,
   D. B. J.; Spudis, P. D.; Carter, L. M.; Neish, C. D.; Thompson, B.;
   Patterson, W.
Bibcode: 2010LPI....41.2652T
Altcode:
  Mini-RF radar data are used to examine the chemical and physical
  properties of both Apollo and Plato regions.

Title: VizieR Online Data Catalog: A catalog of coronal "EIT wave"
    transients (Thompson+, 2009)
Authors: Thompson, B. J.; Myers, D. C.
Bibcode: 2010yCat..21830225T
Altcode:
  The catalog consists of all of the observations in the EIT 195Å images,
  from January 1996 through June 1998, in which we were able to find
  evidence of EIT wave-like phenomena. <P />(2 data files).

Title: Major solar energetic particle events: The first 100 minutes
Authors: Kocharov, Leon; Klassen, Andreas; Reiner, Mike J.; Thompson,
   Barbara; Ryan, James M.; Valtonen, Eino
Bibcode: 2010cosp...38.3002K
Altcode: 2010cosp.meet.3002K
  Using spaceborne particle, EUV and gamma-ray detection and radio
  spectrograms from both ground-based and spaceborne instruments, we
  study the first phase of two major solar energetic particle (SEP)
  events associated with solar eruptions centered at different solar
  longitudes. The well-connected SEP event, observed onboard SOHO on 4
  April 2000, starts with deka-MeV/n helium-and relativistic electron-rich
  production from coronal sources identified with the electromagnetic
  diagnostics. That production dominates during the first 100 min
  of the event, and the coronal SEP sources at that time were not
  shielded by the CME-bow shock between the Sun and the SOHO. The 12
  September 2000 solar eruption was longitude-distant, with respect to
  the Earth-connected heliolongitude, and onset of the first stage of
  the SEP event observed on SOHO was delayed by an extra half hour. In
  both cases, the first phase of the event was followed by a prolonged,
  second-phase SEP production, and both events were associated with a
  decelerating CME-driven shock in solar wind.

Title: If the Sun is so quiet, why is the Earth ringing? A comparison
    of two solar minimum intervals
Authors: Gibson, S. E.; Kozyra, J. U.; de Toma, G.; Emery, B. A.;
   Onsager, T. G.; Thompson, B. J.
Bibcode: 2009AGUFMSH11A1501G
Altcode:
  A system-oriented analysis of new observations from the recent
  international Whole Heliosphere Interval (WHI) campaign in comparison
  with the equivalent Whole Sun Month (WSM) campaign from last cycle’s
  minimum yields new insight into solar quiet intervals and the solar
  minimum Sun-Earth system. We use a side-by-side comparison of these
  two intervals to demonstrate that sunspot numbers, while providing a
  good measure of solar activity, do not provide sufficient information
  to gauge solar and heliospheric magnetic complexity and its effect
  at the Earth. The present solar minimum is exceptionally quiet, with
  sunspot numbers the lowest in 75 years, solar wind density and IMF
  strength at the lowest values ever observed, and geomagnetic indices
  and solar EUV fluxes the lowest in three solar cycles. Despite, or
  perhaps because of this global weakness in the heliospheric magnetic
  field, large near-equatorial coronal holes lingered even as the
  sunspots disappeared, indicating significant open magnetic flux at low
  latitudes. Consequently, for the months surrounding the WHI campaign,
  strong, long, and recurring high-speed streams in the solar wind
  intercepted the Earth in contrast to the weaker and more sporadic
  streams that occurred around the time of the WSM campaign. Since
  the speed, duration and southward magnetic field component in wind
  streams determine the severity of space weather effects, the geospace
  environment responded quite differently to the two solar minimum
  heliospheric morphologies. We illustrate this point with the behavior
  of relativistic electrons in the Earth’s outer radiation belt, which
  were more than three times stronger during WHI than in WSM. The cause
  is clear: it is well-known that high-speed streams drive radiation belt
  population, and indeed, for the months surrounding WHI, geospace and
  upper atmospheric parameters were ringing with the periodicities of
  the solar wind in a manner that was absent last cycle minimum. Such
  behavior could not have been predicted using sunspot numbers alone,
  indicating the importance of considering variation within and between
  solar minima in analyzing and predicting space weather responses at
  the Earth during solar quiet intervals, as well as in interpreting the
  Sun’s past behavior as preserved in geological and historical records.

Title: Recent STEREO Observations of Coronal Mass Ejections
Authors: St Cyr, O. C.; Xie, H.; Mays, M. L.; Davila, J. M.; Gilbert,
   H. R.; Jones, S. I.; Pesnell, W. D.; Gopalswamy, N.; Gurman, J. B.;
   Yashiro, S.; Wuelser, J.; Howard, R. A.; Thompson, B. J.; Thompson,
   W. T.
Bibcode: 2009AGUFMSH11A1491S
Altcode:
  Over 400 CMEs have been observed by STEREO SECCHI COR1 during
  the mission's three year duration (2006-2009). Many of the solar
  activity indicators have been at minimal values over this period,
  and the Carrington rotation-averaged CME rate has been comparable to
  that measured during the minima between Cycle 21-22 (SMM C/P) and
  Cycle 22-23 (SOHO LASCO). That rate is about 0.5 CMEs/day. During
  the current solar minimum (leading to Cycle 24), there have been
  entire Carrington rotations where no sunspots were detected and the
  daily values of the 2800 MHz solar flux remained below 70 sfu. CMEs
  continued to be detected during these exceptionally quiet periods,
  indicating that active regions are not necessary to the generation of
  at least a portion of the CME population. In the past, researchers were
  limited to a single view of the Sun and could conclude that activity
  on the unseen portion of the disk might be associated with CMEs. But
  as the STEREO mission has progressed we have been able to observe an
  increasing fraction of the Sun's corona with STEREO SECCHI EUVI and
  were able to eliminate this possibility. Here we report on the nature
  of CMEs detected during these exceptionally-quiet periods, and we
  speculate on how the corona remains dynamic during such conditions.

Title: Evolution of CMEs in the Heliosphere at Solar Minimum
Authors: Plunkett, S. P.; Wood, B. E.; Odstrcil, D.; Riley, P.;
   Thompson, B. J.; Szabo, A.
Bibcode: 2009AGUFMSH43A..06P
Altcode:
  The STEREO mission permits CMEs to be observed all the way from the Sun
  through the inner heliosphere to beyond the orbit of the Earth, from a
  vantage point away from the Sun-Earth line. We combine remotely-sensed
  imaging and in-situ observations of CMEs from STEREO and other missions
  with modeling of selected events to better understand how CMEs evolve
  as they propagate out from the Sun into the heliosphere, and to study
  the relationship between CMEs observed in imaging instruments and
  ICMEs observed in-situ. We present preliminary results from analysis
  and modeling of a small number of well-observed CME events during the
  present solar minimum period. These include the event of April 26,
  2008 and the Earth-directed event on December 12, 2008.

Title: In Situ Observations of Solar Wind Stream Interface Evolution
Authors: Simunac, K. D. C.; Kistler, L. M.; Galvin, A. B.; Lee, M. A.;
   Popecki, M. A.; Farrugia, C.; Moebius, E.; Blush, L. M.; Bochsler,
   P.; Wurz, P.; Klecker, B.; Wimmer-Schweingruber, R. F.; Thompson,
   B.; Luhmann, J. G.; Russell, C. T.; Howard, R. A.
Bibcode: 2009SoPh..259..323S
Altcode:
  The heliocentric orbits of the two STEREO satellites are similar in
  radius and ecliptic latitude, with separation in longitude increasing
  by about 45° per year. This arrangement provides a unique opportunity
  to study the evolution of stream interfaces near 1 AU over time scales
  of hours to a few days, much less than the period of a Carrington
  rotation. Assuming nonevolving solar wind sources that corotate with
  the Sun, we calculated the expected time and longitude of arrival of
  stream interfaces at the Ahead observatory based on the in situ solar
  wind speeds measured at the Behind observatory. We find agreement to
  within 5° between the expected and actual arrival longitude until the
  spacecraft are separated by more than 20° in heliocentric inertial
  longitude. This corresponds to about one day between the measurement
  times. Much larger deviations, up to 25° in longitude, are observed
  after 20° separation. Some of the deviations can be explained by a
  latitude difference between the spacecraft, but other deviations most
  likely result from evolution of the source region. Both remote and in
  situ measurements show that changes at the source boundary can occur on
  a time scale much shorter than one solar rotation. In 32 of 41 cases,
  the interface was observed earlier than expected at STEREO/Ahead.

Title: Solar wind ion trends and signatures: STEREO PLASTIC
    observations approaching solar minimum
Authors: Galvin, A. B.; Popecki, M. A.; Simunac, K. D. C.; Kistler,
   L. M.; Ellis, L.; Barry, J.; Berger, L.; Blush, L. M.; Bochsler, P.;
   Farrugia, C. J.; Jian, L. K.; Kilpua, E. K. J.; Klecker, B.; Lee,
   M.; Liu, Y. C. -M.; Luhmann, J. L.; Moebius, E.; Opitz, A.; Russell,
   C. T.; Thompson, B.; Wimmer-Schweingruber, R. F.; Wurz, P.
Bibcode: 2009AnGeo..27.3909G
Altcode:
  STEREO has now completed the first two years of its mission, moving
  from close proximity to Earth in 2006/2007 to more than 50 degrees
  longitudinal separation from Earth in 2009. During this time, several
  large-scale structures have been observed in situ. Given the prevailing
  solar minimum conditions, these structures have been predominantly
  coronal hole-associated solar wind, slow solar wind, their interfaces,
  and the occasional transient event. In this paper, we extend earlier
  solar wind composition studies into the current solar minimum using
  high-resolution (1-h) sampling times for the charge state analysis. We
  examine 2-year trends for iron charge states and solar wind proton
  speeds, and present a case study of Carrington Rotation 2064 (December
  2007) which includes minor ion (He, Fe, O) kinetic and Fe composition
  parameters in comparison with proton and magnetic field signatures at
  large-scale structures observed during this interval.

Title: If the Sun is so quiet, why is the Earth ringing? A comparison
    of two solar minimum intervals
Authors: Gibson, S. E.; Kozyra, J. U.; de Toma, G.; Emery, B. A.;
   Onsager, T.; Thompson, B. J.
Bibcode: 2009JGRA..114.9105G
Altcode: 2009JGRA..11409105G
  Observations from the recent Whole Heliosphere Interval (WHI) solar
  minimum campaign are compared to last cycle's Whole Sun Month (WSM)
  to demonstrate that sunspot numbers, while providing a good measure of
  solar activity, do not provide sufficient information to gauge solar
  and heliospheric magnetic complexity and its effect at the Earth. The
  present solar minimum is exceptionally quiet, with sunspot numbers at
  their lowest in 75 years and solar wind magnetic field strength lower
  than ever observed. Despite, or perhaps because of, a global weakness
  in the heliospheric magnetic field, large near-equatorial coronal
  holes lingered even as the sunspots disappeared. Consequently, for
  the months surrounding the WHI campaign, strong, long, and recurring
  high-speed streams in the solar wind intercepted the Earth in contrast
  to the weaker and more sporadic streams that occurred around the
  time of last cycle's WSM campaign. In response, geospace and upper
  atmospheric parameters continued to ring with the periodicities of
  the solar wind in a manner that was absent last cycle minimum, and the
  flux of relativistic electrons in the Earth's outer radiation belt was
  elevated to levels more than three times higher in WHI than in WSM. Such
  behavior could not have been predicted using sunspot numbers alone,
  indicating the importance of considering variation within and between
  solar minima in analyzing and predicting space weather responses at
  the Earth during solar quiet intervals, as well as in interpreting the
  Sun's past behavior as preserved in geological and historical records.

Title: Evolution of CMEs in the Heliosphere
Authors: Plunkett, Simon P.; Wood, Brian E.; Thompson, Barbara J.;
   Szabo, Adam; Odstrcil, Dusan; Riley, Pete
Bibcode: 2009shin.confE.117P
Altcode:
  The STEREO mission permits CMEs to be observed all the way from the Sun
  through the inner heliosphere to beyond the orbit of the Earth, from a
  vantage point away from the Sun-Earth line. We combine remotely-sensed
  imaging and in-situ observations of CMEs from STEREO and other missions
  with modeling of selected events to better understand how CMEs evolve
  as they propagate out from the Sun into the heliosphere, and to study
  the relationship between CMEs observed in imaging instruments and
  ICMEs observed in-situ. We present preliminary results from analysis
  and modeling of a small number of well-observed CME events during the
  present solar minimum period. These include the events of April 26,
  2008, May 17, 2008, and the Earth-directed event on December 12, 2008.

Title: Analysis of Suprathermal Events Observed by STEREO/PLASTIC
    with a Focus on Upstream Events
Authors: Barry, Joshua Adam; Galvin, Antoinette; Popecki, Mark; Ellis,
   Lorna; Kucharek, Harald; Lee, Marty; Simunac, Kristin; Farrugia,
   Charlie; Moebius, Eberhard; Kistler, Lynn; Klecker, Berndt; Luhmann,
   Janet; Russell, Christopher T.; Bochsler, Peter; Wurz, Peter; Wimmer,
   Robert; Thompson, Barbara
Bibcode: 2009shin.confE..94B
Altcode:
  Since the late 1960's, suprathermal and energetic ion events with
  energies ranging from just above the solar wind energies up to 2MeV
  and lasting for several minutes to hours, have been detected upstream
  of the Earth. Possible sources of these ions include magnetospheric
  ions, solar wind ions accelerated between the Earth's bow shock and
  hydromagnetic waves to energies just above the solar wind energies,
  and remnant ions from heliospheric processes (such as Solar Energetic
  Particle (SEP) events or Corotating Interaction Regions (CIRs)). The
  unique orbits of both STEREO spacecraft, STEREO-A (STA) drifting ahead
  in Earth's orbit and STEREO-B (STB) lagging behind in Earth's orbit,
  allow for analysis of upstream events in these unexamined regions. Using
  both the PLASTIC and IMPACT instruments on board STA/B we can examine
  protons in the energy range of solar wind energies up to 80keV, their
  spatial distribution, and attempt to determine if the spacecraft is
  magnetically connected to the Earth's bow shock. Suprathermal events
  observed by STEREO/PLASTIC on STA during solar minimum conditions are
  examined for possible upstream events using anisotropy measurements,
  velocity dispersion, magnetic connection to the bow shock, and frequency
  of events as a function of time and distance.

Title: A Catalog of Coronal "EIT Wave" Transients
Authors: Thompson, B. J.; Myers, D. C.
Bibcode: 2009ApJS..183..225T
Altcode:
  Solar and Heliospheric Observatory (SOHO) Extreme ultraviolet
  Imaging Telescope (EIT) data have been visually searched for coronal
  "EIT wave" transients over the period beginning from 1997 March 24
  and extending through 1998 June 24. The dates covered start at the
  beginning of regular high-cadence (more than 1 image every 20 minutes)
  observations, ending at the four-month interruption of SOHO observations
  in mid-1998. One hundred and seventy six events are included in this
  catalog. The observations range from "candidate" events, which were
  either weak or had insufficient data coverage, to events which were
  well defined and were clearly distinguishable in the data. Included
  in the catalog are times of the EIT images in which the events are
  observed, diagrams indicating the observed locations of the wave fronts
  and associated active regions, and the speeds of the wave fronts. The
  measured speeds of the wave fronts varied from less than 50 to over 700
  km s<SUP>-1</SUP> with "typical" speeds of 200-400 km s<SUP>-1</SUP>.

Title: Pickup Helium at Stream Interfaces and Corotating Interaction
    Regions.
Authors: Kucharek, Harald; Klecker, B.; Möbius, E.; Simunac, K. D. C.;
   Galvin, A. B.; Barry, J.; Bochsler, P.; Blush, L.; Ellis, L.; Farrugia,
   C.; Kistler, L. M.; Lee, M.; Luhmann, J.; Popecki, M. A.; Russell,
   C. T.; Thompson, B.; Wimmer-Schweingruber, R.
Bibcode: 2009shin.confE..34K
Altcode:
  Pickup ion measurements using AMPTE, Ulysses, SOHO, Wind and ACE
  have demonstrated that pickup ion fluxes can vary over a wide range
  and that the shape of the distributions can change substantially on
  time scales from less than one hour to many days. These variations
  have been attributed to changes in the interplanetary magnetic field
  (IMF) which may manifest themselves in incomplete pickup, density
  compressions or rarefactions, and shocks. Suprathermal tails may play a
  significant role because these energetic ions could form a seed particle
  population for further acceleration. Yet, the vast majority of the
  observed temporal variations remain unexplained and it is unknown
  at what distance of the spacecraft the acceleration occurs. High
  resolution and simultaneous observations of pickup ion distributions
  with the Plasma and Suprathermal Ion Composition (PLASTIC) instrument
  on board STEREO A and B, two spatially-separated spacecraft, provide
  an opportunity to follow the temporal and spatial structures of pickup
  ion variations. Furthermore, its Wide Angle Partition (WAP) provides
  direction information. STEREO spacecraft have encountered numerous
  large-scale interplanetary disturbances such as Stream Interfaces
  (SIs) and Corotating Interaction Regions (CIRs). In this presentation
  we will present helium pickup ion spectra and fluxes as a function of
  solar wind and IMF parameters, focusing on their spatial and temporal
  evolution. For selected events we will also determine the location of
  the acceleration region relative to the spacecraft location.

Title: Joint LROC - Mini-RF Observations: Opportunities and Benefits
Authors: Nozette, S.; Bussey, D. B. J.; Butler, B.; Carter, L.;
   Gillis-Davis, J.; Goswami, J.; Heggy, E.; Kirk, R.; Misra, T.;
   Patterson, G. W.; Robinson, M.; Raney, R. K.; Spudis, P. D.; Thompson,
   T.; Thompson, B.; Ustinov, E.
Bibcode: 2009LPICo1483...84N
Altcode:
  No abstract at ADS

Title: Temporal Evolution of the Solar Wind Bulk Velocity at Solar
    Minimum by Correlating the STEREO A and B PLASTIC Measurements
Authors: Opitz, A.; Karrer, R.; Wurz, P.; Galvin, A. B.; Bochsler,
   P.; Blush, L. M.; Daoudi, H.; Ellis, L.; Farrugia, C. J.; Giammanco,
   C.; Kistler, L. M.; Klecker, B.; Kucharek, H.; Lee, M. A.; Möbius,
   E.; Popecki, M.; Sigrist, M.; Simunac, K.; Singer, K.; Thompson, B.;
   Wimmer-Schweingruber, R. F.
Bibcode: 2009SoPh..256..365O
Altcode:
  The two STEREO spacecraft with nearly identical instrumentation were
  launched near solar activity minimum and they separate by about 45°
  per year, providing a unique tool to study the temporal evolution of the
  solar wind. We analyze the solar wind bulk velocity measured by the two
  PLASTIC plasma instruments onboard the two STEREO spacecraft. During the
  first half year of our measurements (March - August 2007) we find the
  typical alternating slow and fast solar wind stream pattern expected at
  solar minimum. To evaluate the temporal evolution of the solar wind bulk
  velocity we exclude the spatial variations and calculate the correlation
  between the solar wind bulk velocity measured by the two spacecraft. We
  account for the different spacecraft positions in radial distance and
  longitude by calculating the corresponding time lag. After adjusting
  for this time lag we compare the solar wind bulk velocity measurements
  at the two spacecraft and calculate the correlation between the two
  time-shifted datasets. We show how this correlation decreases as the
  time difference between two corresponding measurements increases. As
  a result, the characteristic temporal changes in the solar wind bulk
  velocity can be inferred. The obtained correlation is 0.95 for a time
  lag of 0.5 days and 0.85 for 2 days.

Title: Constraints on Aeolian Degradation Rates on Mars from Erasure
    of Rover Tracks
Authors: Geissler, P. E.; Arvidson, R.; Bell, J.; Bridges, N.;
   Desouza, P.; Golombek, M.; Greenberger, R.; Greeley, R.; Herkenhoff,
   K.; Lahtela, H.; Johnson, J. R.; Landis, G.; Li, R.; Moersch, J.;
   Richter, L.; Sims, M.; Soderblom, J.; Sullivan, R.; Thompson, B.;
   Verba, C. A.; Waller, D.; Wang, A.; HiRISE Team; Mer Team
Bibcode: 2009LPI....40.2257G
Altcode:
  Surface and orbital observations of the erasure of the wheel tracks
  made by the MER rovers Spirit and Opportunity provide insights into
  the mechanisms and timescales of aeolian degradation on Mars.

Title: The STEREO/PLASTIC response to solar wind ions (Flight
    measurements and models)
Authors: Daoudi, H.; Blush, L. M.; Bochsler, P.; Galvin, A. B.;
   Giammanco, C.; Karrer, R.; Opitz, A.; Wurz, P.; Farrugia, C.;
   Kistler, L. A.; Popecki, M. A.; Möbius, E.; Singer, K.; Klecker,
   B.; Wimmer-Schweingruber, R. F.; Thompson, B.
Bibcode: 2009ASTRA...5....1D
Altcode:
  The Plasma and Supra-Thermal Ion Composition (PLASTIC) instrument is
  one of four experiment packages on board of the two identical STEREO
  spacecraft A and B, which were successfully launched from Cape Canaveral
  on 26 October 2006. During the two years of the nominal STEREO mission,
  PLASTIC is providing us with the plasma characteristics of protons,
  alpha particles, and heavy ions. PLASTIC will also provide key
  diagnostic measurements in the form of the mass and charge state
  composition of heavy ions. Three measurements (E/q<SUB>k</SUB>,
  time of flight, E<SUB>SSD</SUB>) from the pulse height raw data are
  used to characterize the solar wind ions from the solar wind sector,
  and part of the suprathermal particles from the wide-angle partition
  with respect to mass, atomic number and charge state. In this paper,
  we present a new method for flight data analysis based on simulations
  of the PLASTIC response to solar wind ions. We present the response of
  the entrance system / energy analyzer in an analytical form. Based on
  stopping power theory, we use an analytical expression for the energy
  loss of the ions when they pass through a thin carbon foil. This
  allows us to model analytically the response of the time of flight
  mass spectrometer to solar wind ions. Thus we present a new version
  of the analytical response of the solid state detectors to solar wind
  ions. Various important parameters needed for our models were derived,
  based on calibration data and on the first flight measurements obtained
  from STEREO-A. We used information from each measured event that is
  registered in full resolution in the Pulse Height Analysis words and we
  derived a new algorithm for the analysis of both existing and future
  data sets of a similar nature which was tested and works well. This
  algorithm allows us to obtain, for each measured event, the mass, atomic
  number and charge state in the correct physical units. Finally, an
  important criterion was developed for filtering our Fe raw flight data
  set from the pulse height data without discriminating charge states.

Title: Universal processes in heliophysics
Authors: Davila, Joseph M.; Gopalswamy, Nat; Thompson, Barbara J.
Bibcode: 2009IAUS..257...11D
Altcode:
  The structure of the Universe is determined primarily by the interplay
  of gravity which is dominant in condensed objects, and the magnetic
  force which is dominant in the rarefied medium between condensed
  objects. Each of these forces orders the matter into a set of
  characteristic structures each with the ability to store and release
  energy in response to changes in the external environment. For the
  most part, the storage and release of energy proceeds through a number
  of Universal Processes. The coordinated study of these processes in
  different settings provides a deeper understanding of the underlying
  physics governing Universal Processes in astrophysics.

Title: Putting the "I" in IHY: The United Nations Report for the
    International Heliophysical Year 2007
Authors: Thompson, Barbara J.; Gopalswamy, Natchimuthuk; Davila,
   Joseph M.; Haubold, Hans J.
Bibcode: 2009piih.rept.....T
Altcode:
  No abstract at ADS

Title: Analysis of Suprathermal Events Observed by STEREO/PLASTIC
Authors: Barry, J. A.; Galvin, A. B.; Farrugia, C. J.; Popecki, M.;
   Klecker, B.; Ellis, L.; Lee, M. A.; Kistler, L. M.; Luhmann, J. G.;
   Russell, C. T.; Simunac, K.; Kucharek, H.; Blush, L.; Bochsler, P.;
   Möbius, E.; Thompson, B. J.; Wimmer-Schweingruber, R.; Wurz, P.
Bibcode: 2008AGUFMSH31B1671B
Altcode:
  Since the late 1960's, suprathermal and energetic ion events with
  energies ranging from just above the solar wind energies up to 2MeV
  and lasting for several minutes to hours, have been detected upstream
  of the Earth. Possible sources of these ions include magnetospheric
  ions, solar wind ions accelerated between the Earth's bow shock and
  hydromagnetic waves to energies just above the solar wind energies,
  and remnant ions from heliospheric processes (such as Solar Energetic
  Particle (SEP) events or Corotating Interaction Regions (CIRs)). The
  unique orbits of both STEREO spacecraft, STEREO-A (STA) drifting ahead
  in Earth's orbit and STEREO-B (STB) lagging behind in Earth's orbit,
  allow for analysis of upstream events in these unexamined regions. Using
  both the PLASTIC and IMPACT instruments on board STA/B we can examine
  protons in the energy range of solar wind energies up to 80keV, their
  spatial distribution, and determine if the spacecraft is magnetically
  connected to the Earth's bow shock. Suprathermal events observed by
  STEREO/PLASTIC during solar minimum conditions are examined for possible
  upstream events using anisotropy measurements, velocity dispersion,
  magnetic connection to the bow shock, and frequency of events as a
  function of time and distance.

Title: Outreach activities during the 2006 total solar eclipse
    sponsored by the International Heliophysical Year
Authors: Rabello Soares, M. C.; Rabiu, A. B.; Gopalswamy, N.; Thompson,
   B. J.; Davila, J. M.; Sobrinho, A. A.
Bibcode: 2008AdSpR..42.1792R
Altcode:
  The International Heliophysical Year (IHY) is an international program
  of scientific research to advance our understanding of the physical
  processes that govern the Sun, Earth and heliosphere. It has a strong
  educational component, linking research and education. Here, we describe
  the outreach activities during the 2006 total solar eclipse sponsored
  by IHY.

Title: Temporal and Spatial Variations of Pickup Ions seen on
    STEREO/PLASTIC
Authors: Kucharek, H.; Klecker, B.; Simunac, K.; Russell, C.; Moebius,
   E.; Popecki, M.; Galvin, A.; Kistler, L.; Ellis, L.; Gustafson, A.;
   Barry, J.; Singer, K.; Farrugia, C.; Lee, M.; Blush, L.; Karrer,
   R.; Bochsler, P.; Wurz, P.; Wimmer-Schweingruber, R.; Thompson, B.;
   Luhmann, J.
Bibcode: 2008AGUFMSH21B1605K
Altcode:
  Pickup ions seem to be a perfect tracer of interplanetary
  discontinuities in the heliosphere and they provide important
  information on acceleration processes at these structures and in the
  turbulent solar wind (i.e. suprathermal tails). Studies of pickup ions
  using AMPTE, Ulysses, SOHO, Wind and ACE demonstrated that pickup ion
  fluxes and the shape of their distributions can vary substantially on
  time scales from less than one hour to many days. These variations have
  been attributed to changes in the interplanetary magnetic field (IMF)
  direction and strength in the sense of incomplete pickup and/or density
  compressions and decompressions. For instance, at CIRs one observes
  the most intense and most prolonged enhancements of energetic helium
  pickup ions. At present, the vast majority of the observed temporal
  variations remain unexplained. Furthermore, spatial variations of
  pickup ion distributions could not be studied with single spacecraft
  observation. Simultaneous observations of pickup ion distributions with
  the PLASTIC instrument on STEREO A and B now provide the opportunity
  to follow pickup ion variations on spatial scales from a few 106 km
  to 108 km. In the early mission phase STEREO A and B were often along
  the same magnetic field flux tubes. This allows us to study temporal
  effects. With increasing spacecraft separation spatial effects can
  be studied. In this presentation we will show STEREO observations of
  helium pickup ion spectra and fluxes for 2007/8 in their dependence
  on solar wind density, speed and flux as well IMF direction and
  strength on both spacecraft. We then determined whether the observed
  variations are mainly correlated features that are associated with
  spatial structures passing the STEREO spacecraft at different times
  (such as CIRs or the focusing cone), or whether they have a substantial
  uncorrelated component indicative of temporal variations.

Title: Oxygen Observations by STEREO/PLASTIC in the Slow Solar Wind
Authors: Liu, Y. C.; Galvin, A. B.; Simunac, K. D.; Kistler, L. M.;
   Popecki, M. A.; Farrugia, C. F.; Ellis, L.; Mobius, E.; Lee, M. A.;
   Zurbuchen, T. H.; Lepri, S.; Blush, L. M.; Bochsler, P.; Daoudi, H.;
   Wurz, P.; Wimmer-Schweingruber, R. F.; Klecker, B.; Thompson, B.
Bibcode: 2008AGUFMSH51B1604L
Altcode:
  We have analyzed solar wind oxygen in the data from the STEREO Plasma
  and Supra-thermal Ion Composition Experiment (PLASTIC). For this initial
  study we concentrate on the slow solar wind where the ion composition
  is stable, different ion species have nearly the same bulk speed,
  and the kinetic temperature is usually low. The mass of the detected
  ions is determined when the ions have both a valid time-of-flight
  and a residual energy measured by a Solid State Detector (SSD). The
  bulk speed, thermal speed and flow angles of O6+ are then calculated
  using the electrostatic analyzer and position data. The STEREO data
  are compared to similar measurement on ACE/SWICS.

Title: The Whole Heliosphere Interval: Campaign Summaries and
    Early Results
Authors: Thompson, B.; Gibson, S. E.; McIntosh, S.; Fuller-Rowell,
   T.; Galvin, A. B.; Kozyra, J. U.; Petrie, G.; Schroeder, P.; Strachan,
   L.; Webb, D. F.; Woods, T.
Bibcode: 2008AGUFMSH21C..01T
Altcode:
  The Whole Heliosphere Interval (WHI) is an internationally coordinated
  observing and modeling effort to characterize the 3-dimensional
  interconnected solar-heliospheric-planetary system - a.k.a. the
  "heliophysical" system. The heart of the WHI campaign is the study
  of the interconnected 3-D heliophysical domain, from the interior
  of the Sun, to the Earth, outer planets, and into interstellar
  space. WHI observing campaigns began with the 3-D solar structure from
  solar Carrington Rotation 2068, which ran from March 20 - April 16,
  2008. Observations and models of the outer heliosphere and planetary
  impacts extend beyond those dates as necessary; for example, the
  solar wind transit time to outer planets can take months. WHI occurred
  during solar minimum, which optimizes our ability to characterize the
  3-D heliosphere and trace the structure to the outer limits of the
  heliosphere. Highlights include the 3-D reconstruction of the solar
  wind and complex geospace response during this solar minimum, contrasts
  with the past solar minimum, and the effect of transient activity on the
  "quiet" heliosphere. Nearly 200 scientists are participated in WHI data
  and modeling efforts, ensuring that the WHI integrated observations
  and models will give us a "new view" of the heliophysical system. A
  summary of some of the key results from the WHI first workshop in
  August 2008 will be given.

Title: Constructing a Data System to Support Analysis of the Whole
    Heliosphere Interval
Authors: Thompson, B. J.; Schroeder, P. C.; Gibson, S. E.
Bibcode: 2008AGUFMSH23A1632T
Altcode:
  The Whole Heliosphere Interval is an internationally coordinated
  observing and modeling effort to characterize the 3-dimensional
  interconnected solar-heliospheric-planetary system. The WHI observing
  campaigns began with the 3-D solar structure from solar Carrington
  Rotation 2068, which ran from March 20 to April 16, 2008, and traced
  these structures through the heliosphere and into geospace. The WHI
  team has developed a data and modeling clearinghouse to create a
  unified point of entry into the disparate data sets spanning across
  the traditional disciplinary boundaries. Linkages are provided to data
  from the special observing programs conducted by many observatories
  for the WHI effort, models that looked in detail at the WHI and the
  many other data sets and models from the interval. We also explore
  the Virtual Observatory landscape and highlight their contributions
  to the development of a more complete understanding of the entire
  heliophysical system.

Title: Constraints on Aeolian Degradation Rates on Mars from Erasure
    of Rover Tracks
Authors: Geissler, P. E.; Arvidson, R.; Bell, J.; Bridges, N.; de
   Souza, P.; Golombek, M.; Greenberger, R.; Greeley, R.; Herkenhoff,
   K.; Lahtela, H.; Landis, G.; Li, R.; Moersch, J.; Richter, L.; Sims,
   M.; Soderblom, J.; Sullivan, R.; Thompson, B.; Verba, C.; Waller,
   D.; Wang, A.; Team, H.; Team, M.
Bibcode: 2008AGUFM.P53A1434G
Altcode:
  The wheel tracks left by the MER rovers Spirit and Opportunity are
  unique artificial markings on the surface of Mars. The tracks stretch
  several kilometers across diverse terrain in two widely separated
  regions of the planet. The initial appearance and characteristics of the
  tracks were well documented by the science and navigation cameras aboard
  the vehicles at the time the tracks were formed. Orbital observations
  by Mars Global Surveyor and now Mars Reconnaissance Orbiter document the
  erasure of the tracks over a period of more than two Mars years. We are
  studying the erasure of the rover tracks as a means to better understand
  the mechanisms and time-scales of aeolian degradation on Mars. Spirit's
  wheels left conspicuous dark tracks in the dust-mantled soil of Gusev
  crater. Low albedo sand and gravel were exposed from beneath the bright
  dust mantle along Spirit's traverse from its landing site across the
  Columbia Hills. High albedo, silica-rich soils were ploughed up near
  Home Plate by the rover's stuck right front wheel. MOC images show
  that the tracks near the landing site began to fade gradually in the
  weeks after they were made. Atmospheric dust fallout and summertime
  dust-devils rendered Spirit's tracks invisible before the arrival of
  MRO. Only two small sections of tracks from Spirit's traverse to Home
  Plate can still be seen in recent HiRISE images, on the southern flanks
  of Husband Hill and in the corridor west of Mitcheltree Ridge. Spirit
  witnessed the episodic erasure of its tracks at the height of the
  global dust storm of 2007, when strong surface winds blew away the
  tracks and shifted the soil surrounding the rover over a period of
  just days. Opportunity's tracks across Meridiani Planum to Victoria
  crater were barely visible at the time that they were made, and had
  largely disappeared before the arrival of MRO. Opportunity's tracks
  are slightly brighter than the undisturbed surface because the wheels
  press the darker hematite spherules into the soft soil. Only two short
  sections of pre-2006 tracks remain visible in recent HiRISE images,
  near the craters Fram and Erebus. However, the rover left conspicuous
  bright tracks in the smooth annulus surrounding Victoria crater as she
  traversed the crater's northern rim. Surprisingly, these tracks were
  scarcely altered by the 2007 dust storm, despite clear changes in the
  pattern of wind streaks emanating from the crater. Understanding the
  time-scales and mechanisms of erasure of the rover tracks is important
  for constraining the age of the many pristine impact craters that have
  been discovered by MRO. In turn, this knowledge lets us place bounds
  on the present day bombardment rate of Mars.

Title: International Heliophysical Year 2007: A Report from the
    UN/NASA Workshop Bangalore, India, 27 November 1 December 2006
Authors: Davila, Joe; Gopalswamy, Nat; Thompson, Barbara; Haubold,
   Hans J.
Bibcode: 2008EM&P..103....9D
Altcode: 2008EM&P..tmp...19D
  The IHY Secretariat and the United Nations Basic Space Science
  Initiative (UNBSSI) assist scientists and engineers from all over the
  world in participating in the International Heliophysical Year (IHY)
  2007. A major thrust of IHY/UNBSSI is to deploy arrays of small,
  inexpensive instruments such as magnetometers, radio telescopes,
  GPS receivers, all-sky cameras, etc. around the world to allow
  global measurements of ionospheric and heliospheric phenomena. The
  small instrument programme is envisioned as a partnership between
  instrument providers and instrument hosts in developing nations. The
  IHY/UNBSSI can facilitate the deployment of several of these networks
  world-wide. Existing data bases and relevant software tools will
  be identified to promote space science activities in developing
  nations. Extensive data on space science have been accumulated by a
  number of space missions. Similarly, long-term data bases are available
  from ground-based observations. These data can be utilized in ways
  different from originally intended for understanding the heliophysical
  processes. This paper provides a comprehensive overview of IHY/UNBSSI,
  its achievements, future plans, and outreach to the 192 Member States
  of the United Nations as recorded in the UN/NASA workshop in India.

Title: Polar Gateways Arctic Circle Sunrise Conference 2008, Barrow,
Alaska: IHY-IPY Outreach on Exploration of Polar and Icy Worlds in
    The Solar System
Authors: Cooper, John F.; Kauristie, K.; Weatherwax, A. T.; Sheehan,
   G. W.; Smith, R. W.; Sandahl, I.; Østgaard, N.; Chernouss, S.; Moore,
   M. H.; Peticolas, L. M.; Senske, D. A.; Thompson, B. J.; Tamppari,
   L. K.; Lewis, E. M.
Bibcode: 2008DPS....40.1813C
Altcode: 2008BAAS...40..420C
  Polar, heliophysical, and planetary science topics related to the
  International Heliophysical and Polar Years 2007-2009 were addressed
  during this circumpolar video conference hosted January 23-29,
  2008 at the new Barrow Arctic Research Center of the Barrow Arctic
  Science Consortium in Barrow, Alaska. This conference was planned as
  an IHY-IPY event science outreach event bringing together scientists
  and educational specialists for the first week of sunrise at subzero
  Arctic temperatures in Barrow. Science presentations spanned the
  solar system from the polar Sun to Earth, Moon, Mars, Jupiter, Saturn,
  and the Kuiper Belt. On-site participants experienced look and feel
  of icy worlds like Europa and Titan by being in the Barrow tundra
  and sea ice environment and by going "on the ice" during snowmobile
  expeditions to the near-shore sea ice environment and to Point Barrow,
  closest geographic point in the U.S. to the North Pole. Many science
  presentations were made remotely via video conference or teleconference
  from Sweden, Norway, Russia, Canada, Antarctica, and the United States,
  spanning up to thirteen time zones (Alaska to Russia) at various
  times. Extensive educational outreach activities were conducted with
  the local Barrow and Alaska North Slope communities and through the NASA
  Digital Learning Network live from the "top of the world" at Barrow. The
  Sun-Earth Day team from Goddard, and a videographer from the Passport
  to Knowledge project, carried out extensive educational interviews with
  many participants and native Inupiaq Eskimo residents of Barrow. Video
  and podcast recordings of selected interviews are available at
  http://sunearthday.nasa.gov/2008/multimedia/podcasts.php. Excerpts from
  these and other interviews will be included in a new high definition
  video documentary called "From the Sun to the Stars: The New Science
  of Heliophysics" from Passport to Knowledge that will later broadcast
  on NASA TV and other educational networks. Full conference proceedings
  are accessible at http://polargateways2008.org/.

Title: Whole Heliosphere Interval: Introduction
Authors: Gibson, S. E.; Thompson, B. J.; Webb, D.
Bibcode: 2008AGUSMSH53A..01G
Altcode:
  The Whole Heliosphere Interval (WHI) is an international coordinated
  observing and modeling effort to characterize the three-dimensional
  interconnected solar-heliospheric-planetary system at solar minimum,
  using observations originating at the Sun during Carrington Rotation
  2067: March 20 - April 16, 2008. WHI's science begins with the solar
  interior and extends through the heliosphere and interplanetary
  space out to the heliopause. WHI is a special campaign period of the
  International Heliophysical Year, and involves the participation of
  many observatories and researchers around the world. A "synoptic" set
  of observations provides baseline measurements of the heliophysical
  system, while "targeted" observing campaigns during the WHI interval
  focuses on particular sub-regions of the coupled heliospheric system
  and address specific scientific questions via day-to-day coordinated
  observations. This introductory talk will begin this special session
  dedicated to providing a broad description of the heliosphere at solar
  minimum by showcasing early results of the WHI campaign.

Title: Geospace, Heliospheric and Solar Data collected during the
    Whole Heliosphere Interval
Authors: Thompson, B. J.; Gibson, S. E.; Webb, D. F.
Bibcode: 2008AGUSMSH51A..01T
Altcode:
  The Whole Heliosphere Interval is a comprehensive observing and
  modeling campaign that seeks to connect variations in the Earth's
  ionosphere and magnetosphere with structure and energy variations in
  the heliosphere and solar corona. Hundreds of researchers from around
  the world participated by performing observations and contributing
  data from an extensive array of sources. This poster will summarize
  the observations taking during WHI, including special observations
  performed under the targeted observing campaigns.

Title: The Plasma and Suprathermal Ion Composition (PLASTIC)
    Investigation on the STEREO Observatories
Authors: Galvin, A. B.; Kistler, L. M.; Popecki, M. A.; Farrugia,
   C. J.; Simunac, K. D. C.; Ellis, L.; Möbius, E.; Lee, M. A.; Boehm,
   M.; Carroll, J.; Crawshaw, A.; Conti, M.; Demaine, P.; Ellis, S.;
   Gaidos, J. A.; Googins, J.; Granoff, M.; Gustafson, A.; Heirtzler,
   D.; King, B.; Knauss, U.; Levasseur, J.; Longworth, S.; Singer, K.;
   Turco, S.; Vachon, P.; Vosbury, M.; Widholm, M.; Blush, L. M.; Karrer,
   R.; Bochsler, P.; Daoudi, H.; Etter, A.; Fischer, J.; Jost, J.; Opitz,
   A.; Sigrist, M.; Wurz, P.; Klecker, B.; Ertl, M.; Seidenschwang, E.;
   Wimmer-Schweingruber, R. F.; Koeten, M.; Thompson, B.; Steinfeld, D.
Bibcode: 2008SSRv..136..437G
Altcode: 2008SSRv..tmp....5G
  The Plasma and Suprathermal Ion Composition (PLASTIC) investigation
  provides the in situ solar wind and low energy heliospheric
  ion measurements for the NASA Solar Terrestrial Relations
  Observatory Mission, which consists of two spacecraft (STEREO-A,
  STEREO-B). PLASTIC-A and PLASTIC-B are identical. Each PLASTIC is
  a time-of-flight/energy mass spectrometer designed to determine the
  elemental composition, ionic charge states, and bulk flow parameters of
  major solar wind ions in the mass range from hydrogen to iron. PLASTIC
  has nearly complete angular coverage in the ecliptic plane and an energy
  range from ∼0.3 to 80 keV/e, from which the distribution functions
  of suprathermal ions, including those ions created in pick-up and
  local shock acceleration processes, are also provided.

Title: Whole Heliosphere Interval: Early Science Results
Authors: Gibson, Sarah; Webb, David; Thompson, Barbara
Bibcode: 2008cosp...37.1011G
Altcode: 2008cosp.meet.1011G
  The Whole Heliosphere Interval (WHI) is an international coordinated
  observing and modeling effort to characterize the three-dimensional
  interconnected solar-heliospheric-planetary system at solar minimum,
  using observations originating at the Sun during Carrington Rotation
  2067: March 20 - April 16, 2008. WHI's science begins with the solar
  interior and extends through the heliosphere and interplanetary
  space out to the heliopause. WHI is a special campaign period of the
  International Heliophysical Year, and involves the participation of
  many observatories and researchers around the world. A "synoptic" set
  of observations provides baseline measurements of the heliophysical
  system, while "targeted" observing campaigns during the WHI interval
  focuses on particular sub-regions of the coupled heliospheric system
  and address specific scientific questions via day-to-day coordinated
  observations. This talk will showcase early results of the WHI
  campaign, and thus provide a broad description of the heliosphere at
  solar minimum.

Title: Multi-Spacecraft Observations of Recurring Proton Entropy
    Enhancements Near Solar Minimum
Authors: Simunac, Kristin; Galvin, Antoinette; Kistler, Lynn;
   Popecki, Mark; Moebius, Eberhard; Farrugia, Charles; Luhmann, Janet
   G.; Russell, Christopher; Klecker, Berndt; Wimmer-Schweingruber,
   Robert F.; Thompson, Barbara
Bibcode: 2008cosp...37.2908S
Altcode: 2008cosp.meet.2908S
  The approach to solar minimum in 2007 was an exceptionally quiet time
  in terms of solar activity. Recurring patterns of fast and slow solar
  wind dominated the in situ observations, making it an ideal time to
  study large-scale structures such as recurring high-speed streams
  and co-rotating interaction regions. The leading and trailing edges
  of high-speed streams can be identified in part through changes in
  proton entropy. We have combined in situ data from STEREO-A, STEREO-B,
  and WIND to study the geometry and evolution of recurring highspeed
  streams that have enhanced entropy compared to slow, ambient solar
  wind. Parkerspiral-like geometry is observed for both the leading and
  trailing edges. The trailing edges are observed to have effective
  speeds which are sometimes less than the solar wind bulk speed. We
  will discuss the implications of these findings.

Title: Education and public outreach program for IHY   A global
    approach
Authors: Rabello-Soares, M. C.; Thompson, B. J.; Scherrer, D.;
   Morrow, C.
Bibcode: 2008AdSpR..41.1206R
Altcode:
  Education and public outreach (EPO) is one of the four components
  of the International Heliophysical Year (IHY). It is fundamental in
  achieving one of IHY’s primary objectives which is to “demonstrate
  the beauty, relevance and significance of Space and Earth science
  to the world.” In this paper we give an overview of the IHY EPO
  Program. We describe its goals, structure, elements, plans and what
  have already been achieved.

Title: IHY-IPY conference report from Polar Gateways Arctic Circle
    Sunrise 2008
Authors: Cooper, John; Kauristie, Kirsti; Weatherwax, Allan; Thompson,
   Barbara; Sheehan, Glenn; Smith, Roger; Sandahl, Ingrid
Bibcode: 2008cosp...37..581C
Altcode: 2008cosp.meet..581C
  Polar, heliophysical, and planetary science topics related to the
  International Heliophysical and Polar Years 2007-2009 were addressed
  during this unique circumpolar conference hosted January 23-29,
  2008 at the new Barrow Arctic Research Center of the Barrow Arctic
  Science Consortium in Barrow, Alaska. Science presentations spanned
  the solar system from the polar Sun and heliospheric environment to
  Earth, Moon, Mars, Jupiter, Saturn, the Kuiper Belt, and the solar
  wind termination shock now crossed by both Voyager spacecraft. Many of
  the science presentations were made remotely via video conference or
  teleconference from Sweden, Norway, Russia, Canada, Antarctica, and the
  United States, spanning up to thirteen time zones (Alaska to Russia)
  at various times during the conference. U.S. remote contributions came
  from the University of Alaska at Fairbanks, the University of California
  at Berkeley, the University of Arizona, NASA Jet Propulsion Laboratory,
  and NASA Goddard Space Flight Center. Convening during the first week
  of 2008 Arctic sunrise at Barrow, this conference served as a prelude
  that year to international Sun-Earth Day celebrations for IHY, while
  also commemorating Barrow scientific and native cultural support for the
  first International Polar Year 1882-1883. Extensive educational outreach
  activities were conducted with the local Barrow and Alaska North Slope
  communities and through the NASA Digital Learning Network live from the
  "top of the world" at Barrow. The conference proceedings are Internet
  accessible via the home page at http://polargateways2008.org/.

Title: Solar Wind and Suprathermal Ion Populations at the STEREO
    Spacecraft Approaching Solar Minimum
Authors: Galvin, A. B.; Popecki, M.; Kistler, L.; Simunac, K.;
   Farrugia, C.; Gustafson, A.; Barry, J.; Ellis, L.; Moebius, E.; Blush,
   L.; Klecker, B.; Bochsler, P.; Wurz, P.; Wimmer-Schweingruber, R.;
   Thompson, B.; Luhmann, J.; Russell, C.
Bibcode: 2007AGUFMSH33A1083G
Altcode:
  The two STEREO spacecraft, which were launched in October 2006, have
  been gradually separating in longitude at a rate of about 22 degrees
  per year. During this past year, the dominant heliospheric features
  have been a series of recurrent high and slow speed solar wind and
  their interaction regions, an occasional transient event (e.g., May
  22), and "background" suprathermal populations such as interstellar
  pick up ions. In this poster we present an overview of the plasma
  and suprathermal signatures observed by the STEREO spacecraft using
  data from the Plasma and Suprathermal Ion Composition (PLASTIC)
  and Magnetometer (IMPACT/MAG) investigations. Complementary STEREO
  PLASTIC related presentations in this session are by Popecki et al.,
  Klecker et al. (invited), and Simunac et al.

Title: Correction to ``Major geomagnetic storms (Dst &lt;= -100 nT)
    generated by corotating interaction regions''
Authors: Richardson, I. G.; Webb, D. F.; Zhang, J.; Berdichevsky,
   D. B.; Biesecker, D. A.; Kasper, J. C.; Kataoka, R.; Steinberg, J. T.;
   Thompson, B. J.; Wu, C. -C.; Zhukov, A. N.
Bibcode: 2007JGRA..11212105R
Altcode:
  <A href="/journals/ja/ja0712/2007JA012332/">Abstract Available</A>
  from <A href="http://www.agu.org">http://www.agu.org</A>

Title: Pickup Helium in the Inner Heliosphere: an Overview
Authors: Klecker, B.; Galvin, A. B.; Kucharek, H.; Kistler, L. M.;
   Popecki, M. A.; Mouikis, C.; Farrugia, C.; Möbius, E.; Lee,
   M. A.; Ellis, L.; Simunac, K.; Singer, K.; Blush, L. M.; Bochsler,
   P.; Wurz, P.; Daoudi, H.; Giammanco, C.; Karrer, R.; Opitz, A.;
   Wimmer-Schweingruber, R. F.; Koeten, M.; Hilchenbach, M.; Thompson,
   B.; Acuna, M.; Luhman, J.
Bibcode: 2007AGUFMSH51B..01K
Altcode:
  The CELIAS experiment onboard SOHO and the two Plasma and Suprathermal
  Ion Composition (PLASTIC) experiments onboard STEREO-A/B provide
  measurements of velocity, mass and ionic charge of solar wind ions
  and of suprathermal particles up to energies of 80 keV/e (PLASTIC)
  and 600 keV/e (CELIAS), respectively. Thus both the SOHO and STEREO
  instrumentation covers the energy range of the pickup He particle
  population of interstellar origin that is accelerated to suprathermal
  energies at interplanetary shocks and corotating interaction regions
  (CIRs). ACE and SOHO observations showed a large variability of both
  the pickup He source and the flux of suprathermal particles that so
  far could not be satisfactorily explained. In this overview we will
  summarize recent pickup He observations with ACE and SOHO at 1 AU,
  present first results of pickup He in CIRs obtained with STEREO, and
  discuss open questions that can be tackled in the near future with
  the new constellation of several spacecraft in the inner heliosphere.

Title: Probing the 2-D Geometry of CIRs at Solar Minimum: Observations
    From STEREO
Authors: Simunac, K. D.; Galvin, A. B.; Kistler, L. M.; Popecki,
   M. A.; Farrugia, C.; Moebius, E.; Ellis, L.; Blush, L. M.; Bochsler,
   P.; Wurz, P.; Klecker, B.; Wimmer-Schweingruber, R. F.; Thompson,
   B. J.; Luhmann, J. G.; Russell, C. T.; Jian, L. K.
Bibcode: 2007AGUFMSH33A1084S
Altcode:
  The twin STEREO observatories provide a unique opportunity to study
  the two-dimensional in-ecliptic geometry of structures in the solar
  wind. At the start of 2007 the AHEAD (A) and BEHIND (B) satellites
  were near Earth. By the end of the year they will each be separated
  from Earth by about 20 degrees longitudinally, and from each other
  by about 40 degrees. This arrangement is well suited to test the
  conceptual picture of CIRs in the ecliptic plane. The orbital radius
  of STEREO A is about 0.98 AU, while STEREO B is at about 1.03 AU. If
  A and B were at the same line of longitude they would be less than
  2000 Earth radii apart. Observations show this small radial separation
  becomes important when predicting the arrival time at Earth of streams
  observed with STEREO B; stream fronts were seen to arrive at A and B
  almost simultaneously in mid 2007 when the spacecraft were separated
  by about 7 degrees. This suggests the leading edge of the stream is
  roughly aligned with the solar wind garden hose angle. We report on
  observations of the leading edges of co-rotating high-speed streams,
  and discuss the implications for space weather forecasting.

Title: Correction to ``Solar and interplanetary sources of major
    geomagnetic storms (Dst &lt;= -100 nT) during 1996-2005''
Authors: Zhang, J.; Richardson, I. G.; Webb, D. F.; Gopalswamy, N.;
   Huttunen, E.; Kasper, J.; Nitta, N. V.; Poomvises, W.; Thompson,
   B. J.; Wu, C. -C.; Yashiro, S.; Zhukov, A. N.
Bibcode: 2007JGRA..11212103Z
Altcode:
  <A href="/journals/ja/ja0712/2007JA012891/">Abstract Available</A>
  from <A href="http://www.agu.org">http://www.agu.org</A>

Title: Solar and interplanetary sources of major geomagnetic storms
    (Dst &lt;= -100 nT) during 1996-2005
Authors: Zhang, J.; Richardson, I. G.; Webb, D. F.; Gopalswamy, N.;
   Huttunen, E.; Kasper, J. C.; Nitta, N. V.; Poomvises, W.; Thompson,
   B. J.; Wu, C. -C.; Yashiro, S.; Zhukov, A. N.
Bibcode: 2007JGRA..11210102Z
Altcode:
  We present the results of an investigation of the sequence of
  events from the Sun to the Earth that ultimately led to the 88 major
  geomagnetic storms (defined by minimum Dst ≤ -100 nT) that occurred
  during 1996-2005. The results are achieved through cooperative
  efforts that originated at the Living with a Star (LWS) Coordinated
  Data-Analysis Workshop (CDAW) held at George Mason University in
  March 2005. On the basis of careful examination of the complete array
  of solar and in situ solar wind observations, we have identified
  and characterized, for each major geomagnetic storm, the overall
  solar-interplanetary (solar-IP) source type, the time, velocity, and
  angular width of the source coronal mass ejection (CME), the type and
  heliographic location of the solar source region, the structure of the
  transient solar wind flow with the storm-driving component specified,
  the arrival time of shock/disturbance, and the start and ending times
  of the corresponding IP CME (ICME). The storm-driving component,
  which possesses a prolonged and enhanced southward magnetic field
  (B<SUB>s</SUB>), may be an ICME, the sheath of shocked plasma (SH)
  upstream of an ICME, a corotating interaction region (CIR), or a
  combination of these structures. We classify the Solar-IP sources
  into three broad types: (1) S-type, in which the storm is associated
  with a single ICME and a single CME at the Sun; (2) M-type, in which
  the storm is associated with a complex solar wind flow produced by
  multiple interacting ICMEs arising from multiple halo CMEs launched
  from the Sun in a short period; (3) C-type, in which the storm is
  associated with a CIR formed at the leading edge of a high-speed stream
  originating from a solar coronal hole (CH). For the 88 major storms,
  the S-type, M-type, and C-type events number 53 (60%), 24 (27%), and 11
  (13%), respectively. For the 85 events for which the surface source
  regions could be investigated, 54 (63%) of the storms originated in
  solar active regions, 11 (13%) in quiet Sun regions associated with
  quiescent filaments or filament channels, and 11 (13%) were associated
  with coronal holes. Remarkably, nine (11%) CME-driven events showed no
  sign of eruptive features on the surface or in the low corona (e.g.,
  no flare, no coronal dimming, and no loop arcade, etc.), even though
  all the available solar observations in a suitable time period were
  carefully examined. Thus while it is generally true that a major
  geomagnetic storm is more likely to be driven by a frontside fast
  halo CME associated with a major flare, our study indicates a broad
  distribution of source properties. The implications of the results
  for space weather forecasting are briefly discussed.

Title: HiRISE Observations of Valles Marineris Layering
Authors: Beyer, R. A.; Weitz, C. M.; Thompson, B. J.; Moore, J. M.;
   McEwen, A. S.; HiRISE Team
Bibcode: 2007LPICo1353.3310B
Altcode:
  We used HiRISE to examine layering in the chasma slopes, the interior
  mesas, the chasma floors, and layers observed on the surrounding
  plains. Images show extensive layering with variable lithologies,
  and stunning new views of familiar landscapes.

Title: Bulk Properties of Solar Wind Protons: Inter-comparison of
    Observations From STEREO, SOHO, ACE, and WIND
Authors: Simunac, K. D.; Galvin, A. B.; Kistler, L. A.; Popecki, M. A.;
   Farrugia, C.; Moebius, E.; Lee, M.; Ellis, L.; Singer, K.; Walker,
   C.; Blush, L. M.; Bochsler, P.; Wurz, P.; Daoudi, H.; Giammanco,
   C.; Karrer, R.; Opitz, A.; Klecker, B.; Wimmer-Schweingruber, R. F.;
   Koeten, M.; Thompson, B.
Bibcode: 2007AGUSMSH41A..10S
Altcode:
  The twin STEREO observatories were launched in October 2006. The PLASTIC
  experiment onboard both spacecraft analyzes ions with energies between
  0.25 and 80 keV/charge, including solar wind protons. Information on
  bulk properties such as density, speed, and temperature are obtained. In
  early 2007 STEREO A was separated from SOHO, ACE, WIND, and STEREO
  B by hundreds of earth radii within the ecliptic plane, and by tens
  of earth radii out of the ecliptic plane. We report on comparisons of
  bulk parameters between these spacecraft, and what they show us about
  small-scale temporal and spatial variations in the solar wind.

Title: Early Results from STEREO SECCHI COR1
Authors: St. Cyr, Orville C.; Davila, J. M.; Thompson, W.; Thompson,
   B. J.; Gurman, J. B.; Burkepile, J. T.; de Toma, G.
Bibcode: 2007AAS...21011903S
Altcode: 2007BAAS...39..243S
  With the successful launch and commissioning of STEREO, routine
  observations of the Sun's corona by the payload began in early 2007. The
  COR1 internally-occulted coronagraphs, which are classically-designed
  Lyot instruments covering 1.4-4.0 Rsun, are performing extremely
  well. More than two dozen coronal mass ejections (CMEs) were detected
  by COR1 in the first month of observations. As the STEREO spacecraft
  separate away from Earth, the MK4 coronameter at MLSO will provide
  a third vantage point for observations of the low corona. In this
  presentation we will show CME observations from COR1 and MK4, and we
  will describe the context of these new observations.

Title: IHY - An International Cooperative Program
Authors: Rabello-Soares, M. Cristina; Davila, J.; Gopalswamy, N.;
   Thompson, B.
Bibcode: 2007AAS...210.5701R
Altcode: 2007BAAS...39..167R
  The International Heliophysical Year (IHY) in 2007/2008 involves
  thousands of scientists representing over 70 nations. It consists
  of four distinct elements that will be described here. <P />Taking
  advantage of the large amount of heliophysical data acquired routinely
  by a vast number of sophisticated instruments aboard space missions and
  at ground-based observatories, IHY aims to develop the basic science of
  heliophysics through cross-disciplinary studies of universal processes
  by means of Coordinated Investigation Programs (CIPs). <P />The second
  component is in collaboration with the United Nations Basic Space
  Science Initiative (UNBSSI) and consists of the deployment of arrays of
  small, inexpensive instruments such as magnetometers, radio antennas,
  GPS receivers, etc. around the world to provide global measurements. An
  important aspect of this partnership is to foster the participation
  of developing nations in heliophysics research. <P />IHY coincides
  with the commemoration of 50 years of the space age that started with
  launch of Sputnik on October 4, 1957 and it is on the brink of a new
  age of space exploration where the Moon, Mars and the outer planets
  will be the focus of the space programs in the next years. As a result,
  it presents an excellent opportunity to create interest for science
  among young people with the excitement of discovery of space. The
  education and outreach program forms another cornerstone of IHY. <P
  />Last but not least, an important part of the IHY activities, its
  forth component, is to preserve the history and memory of IGY 1957.

Title: Observations of Energetic O+ in the Distant Tail Magnetosheath:
    Results from STEREO/PLASTIC
Authors: Kistler, L. M.; Galvin, A. B.; Popecki, M. A.; Mouikis,
   C.; Farrugia, C.; Moebius, E.; Lee, M. A.; Ellis, L.; Simunac, K.;
   Singer, K.; Blush, L. M.; Klecker, B.; Wimmer-Schweingruber, R. F.;
   Thompson, B.; Bochsler, P.; Wurz, P.; Karrer, R.; Opitz, A.; Luhmann,
   J.; Acuna, M.; Russell, C. T.
Bibcode: 2007AGUSMSH34A..03K
Altcode:
  Two identical Plasma and Suprathermal Ion Composition (PLASTIC)
  instruments are now flying on the STEREO A and B observatories, which
  launched in October 2006. PLASTIC is a solar wind and heliospheric
  ion mass spectrometer that utilizes electrostatic deflection,
  post-acceleration,time-of-flight, energy, and position measurements
  in the energy-per-charge range of 0.25-80 keV/e. During the month
  of February, 2007, as the spacecraft were approaching their final
  heliocentric orbits, STEREO B traversed the dusk-side magnetosheath and
  boundary layer from -100 Re to -300 Re down the tail. Throughout the
  month, bursts of energetic O+ were observed in the magnetosheath. The
  energy of the O+ extended to the upper range of the instrument, 80
  keV. The occurrence of O+ correlated with periods of high solar wind
  velocity. We will compare these observations with observations of O+
  in the near-earth magnetosheath, as observed by CLUSTER, and discuss
  the possible sources and transport paths for these ions.

Title: On the Variability of Suprathermal He+: new Results From
    STEREO and SOHO
Authors: Klecker, B.; Galvin, A. B.; Kistler, L. M.; Popecki, M. A.;
   Mouikis, C.; Farrugia, C.; Moebius, E.; Lee, M.; Ellis, L.; Simunac,
   K.; Singer, K.; Blush, L. M.; Bochsler, P.; Wurz, P.; Daoudi, H.;
   Giammanco, C.; Karrer, R.; Opitz, A.; Wimmer-Schweingruber, R. F.;
   Koeten, M.; Hilchenbach, M.; Thompson, B.; Acuna, M.; Luhmann, J.
Bibcode: 2007AGUSMSH34A..02K
Altcode:
  The two Plasma and Suprathermal Ion Composition (PLASTIC) experiments
  onboard STEREO-A and STEREO-B and the CELIAS experiment onboard SOHO
  provide measurements of velocity, mass and ionic charge of solar
  wind ions and of suprathermal particles up to energies of 80 keV/e
  (PLASTIC) and 600 keV/e (CELIAS), respectively. The observations with
  SOHO showed a large variability of the He+/He2+ -ratio at suprathermal
  energies, with He+/He2+ &gt; 1 in many interplanetary shock related
  solar energetic particle (SEP) events. This variability is much
  larger than the observed variations in the interstellar pickup He+
  source and suggests that the different velocity distributions of
  the two sources, i.e. solar wind and pickup ions of interstellar
  origin, play an important role for the efficiency of injection and/or
  acceleration of these ions. Thus PLASTIC onboard STEREO, covering the
  energy range from solar wind to pickup ion and suprathermal energies,
  has the potential for resolving some of the questions related to the
  large variability of the He+/He2+-ratios. In this paper we will review
  the SOHO measurements of pickup and suprathermal He+ ions at 1 AU, show
  first results from PLASTIC onboard STEREO and discuss the perspective
  to tackle some of the open questions.

Title: Early Solar Wind Observations from the Plasma and Suprathermal
    Ion Composition (PLASTIC) Experiments on STEREO
Authors: Galvin, A. B.; Kistler, L. A.; Popecki, M. A.; Farrugia, C.;
   Moebius, E.; Lee, M.; Ellis, L.; Simunac, K.; Singer, K.; Russell,
   C.; Walker, C.; Blush, L.; Klecker, B.; Wimmer-Schweingruber, R. F.;
   Thompson, B.; Bochsler, P.; Wurz, P.; Daoudi, H.; Giammanco, C.;
   Karrer, R.; Opitz, A.; Koeten, M.; Luhmann, J.; Howard, R.; Wuelser,
   J. P.; Acuna, M.
Bibcode: 2007AGUSMSH34A..01G
Altcode:
  Two identical Plasma and Suprathermal Ion Composition (PLASTIC)
  instruments are now flying on the STEREO A and B observatories, which
  launched in October 2006. The STEREO observatories are drifting away
  from the Earth and from each other, providing different longitudinal
  perspectives. PLASTIC together with the IMPACT suite provides the
  in-situ measurements for the STEREO mission, while SECCHI provides
  remote imaging of the solar corona. The PLASTIC solar wind sector
  measures solar wind proton bulk parameters and provides species
  identification and relative abundances for the more dominant solar wind
  minor (Z&gt;2) ions. During this early part of the STEREO mission,
  as we approach solar minimum conditions, there have been a series of
  coronal- hole associated high speed streams and interstream sector
  boundaries. In this talk we will provide initial observations of the
  solar wind during selected time periods.

Title: International Heliophysical Year 2007: Basic space science
    initiatives
Authors: Davila, Joe; Gopalswamy, Nat; Haubold, Hans J.; Thompson,
   Barbara
Bibcode: 2007SpPol..23..121D
Altcode:
  The UN Office for Outer Space Affairs, through the IHY Secretariat
  and the United Nations Basic Space Science Initiative (UNBSSI),
  assists scientists and engineers world-wide to participate in
  the International Heliophysical Year (IHY) 2007. A major thrust of
  IHY/UNBSSI is to deploy arrays of small, inexpensive instruments such
  as magnetometers, radio telescopes, GPS receivers, all-sky cameras,
  etc. around the world to allow global measurements of ionospheric and
  heliospheric phenomena. The small instrument program is envisioned
  as a partnership between instrument providers and instrument hosts
  in developing nations, with the former providing the instruments,
  the host nation the manpower, facilities and operational support,
  typically at a local university. Funds are not available through
  IHY/UNBSSI to build the instruments; these must be obtained through the
  normal proposal channels. All instrument operational support for local
  scientists, facilities, data acquisition, etc. will be provided by the
  host nation. The IHY/UNBSSI can facilitate the deployment of several
  of these networks and existing databases and relevant software tools
  will be identified to promote space science activities in developing
  nations. Extensive data on space science have been accumulated
  by a number of space missions. Similarly, long-term databases are
  available from ground-based observations. These data can be utilized
  in ways different from those originally intended for understanding the
  heliophysical processes. This report provides an overview of IHY/UNBSSI,
  its achievements, future plans and outreach to the 192 member states
  of the United Nations.

Title: Globalizing space and Earth science - the International
    Heliophysical Year Education and Outreach Programme
Authors: Rabello-Soares, M. Cristina; Morrow, Cherilynn; Thompson,
   Barbara; Webb, David
Bibcode: 2007IAUSS...5..289R
Altcode:
  No abstract at ADS

Title: The United Nations Basic Space Science Initiative for IHY 2007
Authors: Gopalswamy, Nat; Davila, Joseph; Thompson, Barbara; Haubold,
   Hans
Bibcode: 2007IAUSS...5..295G
Altcode:
  No abstract at ADS

Title: The United Nations Basic Space Science Initiative: the
    TRIPOD concept
Authors: Kitamura, Masatoshi; Wentzel, Don; Henden, Arne; Bennett,
   Jeffrey; Al-Naimiy, H. M. K.; Mathai, A. M.; Gopalswamy, Nat; Davila,
   Joseph; Thompson, Barbara; Webb, David; Haubold, Hans
Bibcode: 2007IAUSS...5..277K
Altcode: 2006physics..10149K
  Since 1990, the United Nations is annually holding a workshop on
  basic space science for the benefit of the worldwide development of
  astronomy. Additional to the scientific benefits of the workshops and
  the strengthening of international cooperation, the workshops lead to
  the establishment of astronomical telescope facilities through the
  Official Development Assistance (ODA) of Japan. Teaching material,
  hands-on astrophysics material, and variable star observing programmes
  had been developed for the operation of such astronomical telescope
  facilities in an university environment. This approach to astronomical
  telescope facility, observing programme, and teaching astronomy has
  become known as the basic space science TRIPOD concept. Currently,
  a similar TRIPOD concept is being developed for the International
  Heliophysical Year 2007, consisting of an instrument array, data taking
  and analysis, and teaching space science.

Title: The International Heliophysical Year
Authors: Davila, Joseph M.; Gopalswamy, Nat; Thompson, Barbara J.
Bibcode: 2007RoAJ...17....3D
Altcode:
  No abstract at ADS

Title: Three-dimensional global simulation of multiple ICMEs’
    interaction and propagation from the Sun to the heliosphere following
    the 25 28 October 2003 solar events
Authors: Wu, C. -C.; Fry, C. D.; Dryer, M.; Wu, S. T.; Thompson, B.;
   Liou, Kan; Feng, X. S.
Bibcode: 2007AdSpR..40.1827W
Altcode:
  This study performs simulations of interplanetary coronal mass
  ejection (ICME) propagation in a realistic three-dimensional
  (3D) solar wind structure from the Sun to the Earth by using the
  newly developed hybrid code, HAFv.2+3DMHD. This model combines
  two simulation codes, Hakamada-Akasofu-Fry code version 2 (HAFv.2)
  and a fully 3D, time-dependent MHD simulation code. The solar wind
  structure is simulated out to 0.08 AU (18 Rs) from source surface
  maps using the HAFv.2 code. The outputs at 0.08 AU are then used to
  provide inputs for the lower boundary, at that location, of the 3D MHD
  code to calculate solar wind and its evolution to 1 AU and beyond. A
  dynamic disturbance, mimicking a particular flare's energy output,
  is delivered to this non-uniform structure to model the evolution
  and interplanetary propagation of ICMEs (including their shocks). We
  then show the interaction between two ICMEs and the dynamic process
  during the overtaking of one shock by the other. The results show that
  both CMEs and heliosphere current sheet/plasma sheet were deformed by
  interacting with each other.

Title: Duplicity in 16 Piscium Confirmed from Its Occultation by 7
    Iris on 2006 May 5
Authors: Thompson, B.; Yeelin, T.
Bibcode: 2006PASP..118.1648T
Altcode:
  The occultation of 16 Piscium by the asteroid 7 Iris on 2006 May 5 was
  observed with a mobile telescope at a site near Ithaca, New York. The
  signal from a video camera was time-stamped and recorded. Computer
  analysis of the recording shows a stepped disappearance and
  reappearance, as is expected for a double star. After correcting for
  saturated pixels in the recording, the two components of the double star
  were determined to have nearly equal magnitudes. By assuming a circular
  silhouette for the asteroid, the separation and position angle of the
  double star is constrained to two possibilities. This occultation result
  confirms a previous spectroscopic observation by G. Cayrel de Strobel.

Title: IHY-CAWSES Data base
Authors: Young, C. A.; Thompson, B. J.; Davila, J.; Gopalswamy, N.
Bibcode: 2006ihy..workE..90Y
Altcode:
  In partnership with the CAWSES (Climate And Weather of the Sun-Earth
  System) program, IHY is sponsoring a series of Virtual Workshops
  and a special IHY/CAWSES database to provide virtual access of data
  collected for IHY and CAWSES campaigns. The first of the virtual
  workshops occurred November 13-17, 2006, and had more than 200 online
  participants. Online presentation and discussion tools are being
  refined for future workshops. The IHY/CAWSES database provides a means
  of entering data into the Virtual Solar Observatory (to provide the
  maximum and easiest possible access to the data) while still maintaining
  a close connection to the other data sets used in IHY/CAWSES activities.

Title: IHY-2007: Coordinated Investigation Programs (CIPs)
Authors: Thompson, B. J.; et al.
Bibcode: 2006ihy..workE..17T
Altcode:
  The IHY has established a set of primary scientific objectives
  and goals. To accomplish these goals, a wide range of Coordinated
  Investigation Programs (CIPs) will transpire throughout the
  IHY timeframe, driving towards a more complete understanding of
  heliophysical universal processes. The CIPs are the basic "building
  block" of IHY science - they are proposed by members of the IHY
  community, and are approved and coordinated by the IHY discipline
  coordinators. The aim is that the program remains under the control
  of the proposer(s) with the IHY CIP process providing a means of
  publicising the proposed work, co-ordinating access to and use of the
  necessary resources, and a forum for discussing the results. There
  are currently over 50 CIPs in the IHY database, with many more being
  proposed.

Title: IHY/UNBSS Program: Success Stories
Authors: Gopalswamy, N.; Davila, J.; Thompson, B. J.; Haubold, H. J.
Bibcode: 2006ihy..workE..15G
Altcode:
  The United Nations Office for Outer Space Affairs, through the IHY
  secretariat and the United Nations Basic Space Science Initiative
  (UNBSSI) is assisting scientists and engineers from all over the world
  in participating in the International Heliophysical Year (IHY) 2007. A
  major thrust of the IHY/UNBSSI program is to deploy arrays of small,
  inexpensive instruments such as magnetometers, radio telescopes, GPS
  receivers, etc. around the world to provide global measurements of
  ionospheric and heliospheric phenomena. The small instrument program
  is a partnership between instrument providers, and instrument hosts in
  developing countries. The lead scientist will provide the instruments
  (or fabrication plans for instruments) in the array; the host country
  will provide manpower, facilities, and operational support to obtain
  data with the instrument typically at a local university. Existing data
  bases and relevant software tools can be identified to promote space
  science activities in developing countries. Extensive data on space
  science have been accumulated by a number of space missions. Similarly,
  long-term data bases are available from ground based observations. These
  data can be utilized in ways different from originally intended for
  understanding the heliophysical processes. This paper provides an
  overview of the IHY/UNBSS program, its achievements and future plans.

Title: Globalizing Space and Earth Science - the International
    Heliophysical Year Education and Outreach Program
Authors: Rabello-Soares, M. C.; Morrow, C.; Thompson, B. J.
Bibcode: 2006IAUSS...5E..48R
Altcode:
  The International Heliophysical Year (IHY) in 2007 &amp; 2008 will
  celebrate the 50th anniversary of the International Geophysical
  Year (IGY) and, following its tradition of international research
  collaboration, will focus on the cross-disciplinary studies of
  universal processes in the heliosphere. The main goal of IHY Education
  and Outreach Program is to create more global access to exemplary
  resources in space and earth science education and public outreach. By
  taking advantage of the IHY organization with representatives in
  every nation and in the partnership with the United Nations Basic
  Space Science Initiative (UNBSSI), we aim to promote new international
  partnerships. Our goal is to assist in increasing the visibility and
  accessibility of exemplary programs and in the identification of formal
  or informal educational products that would be beneficial to improve the
  space and earth science knowledge in a given country; leaving a legacy
  of enhanced global access to resources and of world-wide connectivity
  between those engaged in education and public outreach efforts that are
  related to IHY science. Here we describe how to participate in the IHY
  Education and Outreach Program and the benefits in doing so. Emphasis
  will be given to the role played by developing countries; not only
  in selecting useful resources and helping in their translation and
  adaptation, but also in providing different approaches and techniques
  in teaching.

Title: The United Nations Basic Space Science Initiative for IHY 2007
Authors: Gopalswamy, N.; Davila, J. M.; Thompson, B. J.; Haubold, H.
Bibcode: 2006IAUSS...5E..47G
Altcode:
  The United Nations, in cooperation with national and international
  space-related agencies and organizations, has been organizing annual
  workshops since 1990 on basic space science, particularly for the
  benefit of scientists and engineers from developing nations. The United
  Nations Office for Outer Space Affairs, through the IHY Secretariat and
  the United Nations Basic Space Science Initiative (UNBSSI) will assist
  scientists and engineers from all over the world in participating in
  the International Heliophysical Year (IHY) 2007. A major thrust of the
  IHY/UNBSSI program is to deploy arrays of small, inexpensive instruments
  such as magnetometers, radio telescopes, GPS receivers, all-sky cameras,
  etc. around the world to provide global measurements of ionospheric
  and heliospheric phenomena. The small instrument program is envisioned
  as a partnership between instrument providers, and instrument hosts in
  developing countries. The lead scientist will provide the instruments
  (or fabrication plans for instruments) in the array; the host country
  will provide manpower, facilities, and operational support to obtain
  data with the instrument typically at a local university. Funds
  are not available through the IHY to build the instruments; these
  must be obtained through the normal proposal channels. However all
  instrument operational support for local scientists, facilities, data
  acquisition, etc will be provided by the host nation. It is our hope
  that the IHY/UNBSSI program can facilitate the deployment of several of
  these networks world wide. Existing data bases and relevant software
  tools that can will be identified to promote space science activities
  in developing countries. Extensive data on space science have been
  accumulated by a number of space missions. Similarly, long-term data
  bases are available from ground based observations. These data can be
  utilized in ways different from originally intended for understanding
  the heliophysical processes. This paper provides an overview of the
  IHY/UNBSS program, its achievements and future plans.

Title: Major geomagnetic storms (Dst &lt;= -100 nT) generated by
    corotating interaction regions
Authors: Richardson, I. G.; Webb, D. F.; Zhang, J.; Berdichevsky,
   D. B.; Biesecker, D. A.; Kasper, J. C.; Kataoka, R.; Steinberg, J. T.;
   Thompson, B. J.; Wu, C. -C.; Zhukov, A. N.
Bibcode: 2006JGRA..111.7S09R
Altcode: 2006JGRA..11107S09R
  Seventy-nine major geomagnetic storms (minimum Dst ≤ -100 nT) observed
  in 1996 to 2004 were the focus of a "Living with a Star" Coordinated
  Data Analysis Workshop (CDAW) in March 2005. In nine cases, the storm
  driver appears to have been purely a corotating interaction region (CIR)
  without any contribution from coronal mass ejection-related material
  (interplanetary coronal mass ejections (ICMEs)). These storms were
  generated by structures within CIRs located both before and/or after the
  stream interface that included persistently southward magnetic fields
  for intervals of several hours. We compare their geomagnetic effects
  with those of 159 CIRs observed during 1996-2005. The major storms form
  the extreme tail of a continuous distribution of CIR geoeffectiveness
  which peaks at Dst ∼ -40 nT but is subject to a prominent seasonal
  variation of ∼40 nT which is ordered by the spring and fall equinoxes
  and the solar wind magnetic field direction toward or away from the
  Sun. The O'Brien and McPherron (2000) equations, which estimate Dst by
  integrating the incident solar wind electric field and incorporating
  a ring current loss term, largely account for the variation in storm
  size. They tend to underestimate the size of the larger CIR-associated
  storms by Dst ∼ 20 nT. This suggests that injection into the ring
  current may be more efficient than expected in such storms. Four of
  the nine major storms in 1996-2004 occurred during a period of less
  than three solar rotations in September to November 2002, also the
  time of maximum mean IMF and solar magnetic field intensity during
  the current solar cycle. The maximum CIR-storm strength found in our
  sample of events, plus additional 23 probable CIR-associated Dst ≤
  -100 nT storms in 1972-1995, is (Dst = -161 nT). This is consistent
  with the maximum storm strength (Dst ∼ -180 nT) expected from the
  O'Brien and McPherron equations for the typical range of solar wind
  electric fields associated with CIRs. This suggests that CIRs alone
  are unlikely to generate geomagnetic storms that exceed these levels.

Title: A Kopp-Pneuman-like Picture of Coronal Mass Ejections
Authors: Spicer, D. S.; Sibeck, D.; Thompson, B. J.; Davila, J. M.
Bibcode: 2006ApJ...643.1304S
Altcode:
  A new coronal mass ejection (CME) picture is described that utilizes
  a number of attributes commonly found operating during magnetotail
  reconnection events. We first present key observational constraints any
  final model of CMEs must explain. We then describe how three-dimensional
  reconnection occurs in the magnetotail and how magnetotail reconnection
  helps explain a variety of observed CME attributes. We then argue why
  reconnection, as usually described in the literature, cannot explain
  the particle acceleration process that occurs during the CME/flare
  process. Instead we argue that it is the flow fields that are driven
  by the relaxation of the magnetic stresses due to reconnection that
  are ultimately the cause of particle acceleration. In particular, it
  is the electrons that make up the discharging field-aligned currents,
  which connect flow field-driven cross field inertial currents in the
  high corona with the chromosphere, that are in fact the high-energy
  electrons needed to explain flare ribbons and other high-energy
  emissions. We compute the expected electron fluxes from these current
  systems and find that they are of order those required. In addition,
  we discuss betatron acceleration during the dipolarization process
  that occurs when the flux rope/CME is ejected and how the hot particles
  generated during the dipolarization process can lead to traps in solar
  loops, thereby helping to explain long-duration events. Further, we
  examine whether particle acceleration by shocks can contribute to the
  mix. We also note that our new picture eliminates a number of paradoxes,
  specifically elimination of magnetic flux from the Sun and how the Aly
  conjecture is not of consequence in our picture. Finally, we examine
  what will be needed to numerically simulate our picture of a CME.

Title: Major geomagnetic storms (Dst≤-100~nT) generated by
    corotating interaction regions in 1996--2004
Authors: Richardson, I. G.; Webb, D. F.; Zhang, J.; Berdichevsky,
   D. B.; Biesecker, D. A.; Kasper, J. C.; Kataoka, R.; Steinberg, J. T.;
   Thompson, B. J.; Wu, C.; Zhukov, A. N.
Bibcode: 2006AGUSMSH53A..06R
Altcode:
  Nine of the major geomagnetic storms (Dst≤-100~nT) in 1996 to 2004
  studied at the "Living with a Star" CDAW workshop in March, 2005 were
  driven purely by a corotating interaction region (CIR) without any
  contribution from coronal mass ejection-related material. These storms
  were generated by structures located both before and/or after the stream
  interface that included persistently southward magnetic fields for
  intervals of several hours. We compare the geomagnetic effects of these
  storms with those of 159 CIRs observed during 1996 -- 2005. The major
  storms form the extreme tail of a distribution of CIR geoeffectiveness
  which peaks at Dst~-40~nT but has a prominent seasonal variation of
  ~40~nT ordered by the spring and fall equinoxes and the solar wind
  magnetic field direction towards or away from the Sun. The O'Brien
  and McPherron [2000] equations for Dst prediction largely account for
  the variation in storm size but tend to underestimate the size of the
  larger CIR-associated storms by Dst~20~nT, suggesting that injection
  into the ring current may be more efficient than expected in such
  storms. The maximum storm strength in these events, plus an additional
  23 CIR-associated storms in 1972 -- 1995, is Dst=-161~nT. This is
  consistent with the maximum storm strength (Dst~-180~nT) expected
  for the range of solar wind electric fields associated with CIRs,
  suggesting that CIRs alone are unlikely to generate geomagnetic storms
  that exceed such levels.

Title: The IGY Gold History Preservation Program
Authors: Thompson, B. J.; Cliver, E. W.; Gentile, L. C.; Sigsbee,
   K. M.; Doel, R. E.
Bibcode: 2006AGUSM.U41D..08T
Altcode:
  An important part of the 2007 International Year activities will be
  preserving the history and memory of IGY 1957. The "IGY Gold" History
  initiative has several goals: 1) identifying and recognizing planners
  of and participants in the first IGY, 2) preserving memoirs, articles,
  photographs, and all items of historical significance for the IGY,
  3) making these items available to historians, researchers, etc.,
  4) serving as a contact service for these activities, 5) spreading
  awareness of the history of geophysics, and 6) planning special events
  and "reunions." The IGY "Gold" Club identifies participants from
  the first IGY (gold symbolizing the 50th anniversary). "Gold club"
  participants will be rewarded with a special "IGY Gold Anniversary"
  certificate of recognition and a special commemorative "IGY Gold"
  lapel pin. Many IGY participants from around the globe have received
  IGY Gold Club awards, and many have submitted valuable historical
  material about the IGY activities. This is a joint program of the IHY,
  eGY, IPY, IYPE and IUGG.

Title: Planning the International Heliophysical Year (IHY)
Authors: Davila, Joseph M.; Thompson, Barbara J.; Gopalswamy, Nat
Bibcode: 2006UNPSA..17...37D
Altcode:
  No abstract at ADS

Title: Preparing for the International Heliophysical Year (IHY) 2007
Authors: Davila, J. M.; Gopalswamy, N.; Thompson, B. J.
Bibcode: 2006ilws.conf..231D
Altcode:
  The International Geophysical Year (IGY) of 1957, a broad-based and
  all-encompassing effort to push the frontiers of geophysics, resulted
  in a tremendous increase of knowledge in space physics, Sun-Earth
  Connection, planetary science and the heliosphere in general. Now, 50
  years later, we have the unique opportunity to advance our knowledge of
  the global heliosphere and its interaction with planetary bodies and
  the interstellar medium through the International Heliophysical Year
  (IHY) in 2007. This will be an international effort, which will raise
  public awareness of space physics.

Title: The IHY/United Nations Distributed Observatory Development
    Program
Authors: Haubold, H.; Thompson, B. J.; Al-Naimiy, H.; Davila, J. M.;
   Gopalswamy, N.; Groves, K.; Scherrer, D.
Bibcode: 2006cosp...36.3304H
Altcode: 2006cosp.meet.3304H
  A major thrust of the International Heliophysical Year IHY is to
  deploy arrays of small inexpensive instruments such as magnetometers
  radio antennas GPS receivers all-sky cameras etc around the world
  to provide global measurements of ionospheric magnetospheric and
  heliospheric phenomena This program is a collaboration between the IHY
  and the United Nations Basic Space Science Initiative UNBSSI which has
  been dedicated to the IHY through 2009 The small instrument program
  consists of a partnership between instrument providers and instrument
  host countries The lead scientist provides the instrumentation or
  fabrication plans for instruments in the array the host country
  provides manpower facilities and operational support to obtain data
  with the instrument typically at a local university This program has
  been active in deploying instrumentation developing plans for new
  instrumentation and identifying educational opportunities for the host
  nations in association with this program We will discuss the program
  s status significant deployment activities and plans for 2007-2009

Title: Understanding the Heliospheric Environment for NASA's
    Spacefleet
Authors: St. Cyr, O. C.; Thompson, B. J.; Rowland, D. E.; Hesse, M.
Bibcode: 2006cosp...36.3297S
Altcode: 2006cosp.meet.3297S
  Presently the U S National Aeronautics and Space Administration has more
  than 50 active robotic science satellites seven active communications
  satellites and the manned International Space Station With this
  investment NASA has a responsibility to protect its space assets
  throughout the solar system For humans this function is performed by
  the Space Radiation Analysis Group at Johnson Space Center in Houston
  Texas But for robotic explorers this function is performed only on
  an ad hoc basis Space environmental awareness is missing for much of
  the existing fleet beyond Earth-orbit and it is required for anomaly
  resolution and good stewardship of our national assets Engineers
  require this information to make a complete assessment of the root
  cause of operational anomalies Threats to space assets arise from many
  sources on a wide range of timescales direct effects of radiation and
  energetic particles on robotic and human explorers indirect and delayed
  effects on the heliosphere e g MHD shocks on planetary magnetospheres e
  g transient radiation belts and on atmospheres e g aerobraking and long
  term solar cycle predictions Because environmental assessment throughout
  the heliosphere is not yet operational it requires interpretation of
  data heterogeneous in form and quality groundbased and spacebased as
  well as interaction with sophisticated numerical models A conceptual
  study of environmental conditions was done on an ad hoc basis for
  a failure at Mars in 2004 Here we will describe recent efforts and
  discuss near-term plans at

Title: Outreach and Education Program for IHY - A Global Approach
Authors: Rabello-Soares, M. C.; Thompson, B. J.
Bibcode: 2006cosp...36.2631R
Altcode: 2006cosp.meet.2631R
  The IHY Outreach and Education Program is one of the 4 main components
  of IHY Science Observatory Development Outreach and History and it is
  fundamental in achieving one of IHY s primary objectives which is to
  demonstrate the beauty relevance and significance of Space and Earth
  Science to the world The Outreach and Education Program for IHY has the
  following objectives 1 inspire the next generation of Space and Earth
  scientists and explorers and 2 spread the knowledge of our solar system
  and the exciting process of scientific exploration to the public There
  is already in place a wide variety of outreach and education activities
  related to Space and Earth Science We would like to see all of them
  come together to celebrate the International Heliophysical Year in 2007
  The IHY Outreach and Education Program will focus on a developing new
  and exciting outreach programs that provide unique opportunities for
  the global community b increasing the visibility and accessibility of
  existing outreach programs c developing partnerships between existing
  programs and activities to broaden their scope and impact d determining
  the need for

Title: International coordinated efforts for IHY 2007
Authors: Gopalswamy, N.; Davila, J.; Thompson, B.
Bibcode: 2006cosp...36.2743G
Altcode: 2006cosp.meet.2743G
  The International Heliophysical Year IHY in 2007 marks the enormous
  progress made since the International Geophysical Year IGY in 1957
  The philosophy behind IHY is similar to that of IGY in studying the
  environment of our habitat except that the scope has increased to the
  physical space extending to the interstellar medium This paper describes
  the international organization of the IHY and planning for a successful
  program in 2007 In particular we describe the national regional and
  global efforts in pooling the resources to address the universal
  processes that govern the solar system and its interaction with the
  surrounding medium The efforts include identifying science questions of
  immediate concern and the data sets needed to address these questions
  The data will be acquired using a truly distributed observatory
  consisting of all the ground and space-based instruments that exist
  today and those to be constructed before 2007 The international planning
  also involves coordinating with the United Nations which through its
  Basic Space Science Initiative is facilitating the participation of the
  developing nations in the IHY program An update of the current status
  of the planning activities at the international level will be presented

Title: The evolution and interaction of multiple coronal mass
Authors: Wu, C. C.; Fry, C.; Wu, S. T.; Dryer, M.; Thompson, B.;
   Liou, K.; Feng, X. S.
Bibcode: 2006cosp...36..407W
Altcode: 2006cosp.meet..407W
  The famous solar events of Halloween 2003 caused two of the most intense
  geomagnetic storms with Dst min -363 and -401 nT during Solar Cycle
  23 In order to understand the interplanetary causes of this famous
  event which contains multiple flares and coronal mass ejections we
  will perform MHD simulations to investigate the evolution of solar
  disturbances that caused these severe geomagnetic storms This study
  performs simulations of interplanetary coronal mass ejection ICME
  propagation in a realistic 3D solar wind structure from the Sun to the
  Earth by using the newly developed hybrid code HAFv 2 3DMHD This code
  combines two simulation codes Hakamada-Akasofu-Fry code HAF version 2
  HAFv 2 and a fully three-dimensional time-dependent MHD simulation code
  and is used for this purpose The solar wind structure is simulated out
  to 0 08 AU 18 solar radius from source surface maps 2 5 solar radii Rs
  that are derived from daily-provided solar magnetograms using the HAFv 2
  code This code is then used from 2 5 Rs to provide input for the lower
  boundary of the 3D MHD code to calculate the evolution of solar wind
  plasma and interplanetary magnetic field beyond 18 Rs 0 08 AU A dynamic
  disturbance mimicing a particular flare s energy output is delivered to
  this non-uniform structure to model the evolution and interplanetary
  propagation of coronal mass ejections ICME including their shocks We
  also integrate the line-of-sight density in the plane-of-sky to

Title: 2007: The International Heliophysical Year - a great
    opportunity for Space and Earth Science outreach
Authors: Rabello-Soares, M. C.; Thompson, B. J.; Morrow, C.
Bibcode: 2006cosp...36.2649R
Altcode: 2006cosp.meet.2649R
  Fifty years after the International Geophysical Year IGY in 1957 the
  International Heliophysical Year IHY represents a logical next-step
  extending the studies into the heliosphere and thus including
  the drivers of geophysical change The IHY fields of research are
  solar physics planetary magnetospheres heliosphere and cosmic rays
  planetary ionospheres thermospheres and mesopheres climate studies
  and heliobiology see session D1 2 The basic objectives of IHY are 1
  advancing our understanding of the physical processes that govern the
  Sun Earth and Heliosphere 2 continuing the tradition of international
  research and advancing the legacy on the 50th anniversary of the
  International Geophysical Year 3 demonstrating the Beauty Relevance
  and Significance of Space and Earth Science to the World The IHY is
  being coordinated by an international committee involving hundreds of
  observatories and institutions worldwide The central coordination is
  hosted by the American Geophysical Union Also the United Nations Basic
  Space Science Initiative UNBSSI will dedicate its activities through
  2009 to the IHY effort targeting activities in developing nations such
  as the IHY UNBSSI Small Instrument Array Deployment

Title: The International Heliophysical Year (IHY) 2007
Authors: Davila, J. M.; Thompson, B. J.; Gopalswamy, N.
Bibcode: 2006AfrSk..10....4D
Altcode:
  The International Geophysical Year (IGY) of 1957, a broad-based
  and all-encompassing effort to push the frontiers of geophysics,
  resulted in a tremendous increase of knowledge in space physics,
  the Sun-Earth connection, planetary science, and the heliosphere in
  general. Now, fifty years later, we have the unique opportunity to
  advance our knowledge of the global heliosphere and its interaction with
  planetary bodies and the interstellar medium through the International
  Heliophysical Year (IHY) in 2007. This will be an international effort
  which will raise public awareness of space physics. Because of its
  unique geographic position, Africa is well-positioned to play a
  critical role.

Title: Three-dimensional global simulation of CME/ICME/Shock
    propagation from Sun to the heliosphere
Authors: Wu, C.; Fry, C.; Thompson, B. J.; Wu, S.; Dryer, M.; Liou, K.
Bibcode: 2005AGUFMSH14A..03W
Altcode:
  This study performs simulations of the propagation of coronal mass
  ejections from the Sun to the Earth through a realistic 3D solar
  wind structure. The famous solar event of 12 May 1997, described
  observationally by Thompson et al. [1998, 1999] and theoretically
  by Wu et al. [2001], is used as motivation for this simulation. The
  newly developed code, HAF+3DMHD combines two simulation codes,
  Hakamada-Akasofu-Fry code (HAF) version 2 (HAFv.2) [Fry et al., 2001]
  and a fully three-dimensional, time-dependent MHD simulation code
  [Han et al, 1988]. The solar wind structure is simulated, using the
  HAF code, out to 0.08 AU from source surface maps derived from solar
  magnetograms. The HAF simulation is then used as input for the lower
  boundary of a 3D MHD code to calculate the evolution of solar wind
  plasma beyond 18 solar radii (0.08 AU). A dynamic disturbance is
  delivered to this non-uniform structure to model the evolution and
  interplanetary propagation of a coronal mass ejection (ICME, including
  its shock). We also integrate the changing line-of-sight heliospheric
  density to compare to data observed by the LASCO instrument on SOHO,
  and we compare the derived ICME and shock structure at 1 AU to WIND
  solar wind data for this 12 May 1997 event. This new code provides a
  tool to link the general cases of ICME at 1 AU to their solar sources,
  as well as to identify the possible origins of shock formation due to
  CMEs and CME/CIR interactions. In the case of complex or interacting
  ejecta, model interpretation is often required to accurately determine
  the solar sources of the ejecta observed at 1 AU. Because this newly
  developed model incorporates 3D MHD, its results can be extended to
  simulate coronal and heliospheric observations, including the ambient
  medium's non-uniformity provided by the HAFv.2 model, from the upcoming
  STEREO mission. Reference: Fry et al., JGR, 106, 20985-21001, 2001. Han
  et al., Comp. and Fluids, 16, 81-103, 1988. Thompson et al., GRL,
  25, 2465-2468, 1998. Thompson et al., AP. J. Lett., 517, L151-L155,
  1999. Wu et al., JGR, 106, 25089-25102, 2001.

Title: Distributed Instrumentation Deployment During the IHY
Authors: Davila, J. M.; Thompson, B. J.; Gopalswamy, N.
Bibcode: 2005AGUFMSM21A0347D
Altcode:
  A major thrust of the International Heliophysical Year (IHY) is to
  deploy arrays of small, inexpensive instruments such as magnetometers,
  radio antennas, GPS receivers, all-sky cameras, etc. around the
  world to provide global measurements of ionospheric and heliospheric
  phenomena. This program is a collaboration between the IHY and the
  United Nations Basic Space Science (UNBSS) program, which has been
  dedicated to the IHY through 2009. The small instrument program is
  envisioned as a partnership between instrument providers, and instrument
  host countries. The lead scientist will provide the instruments (or
  fabrication plans for instruments) in the array; the host country
  will provide manpower, facilities, and operational support to obtain
  data with the instrument typically at a local university. Instrument
  operational support for local scientists, facilities, data acquisition,
  etc will be provided by the host nation.

Title: Differentiating Between Streamer Deflections and "New Mass"
    in Halo CMEs
Authors: Thompson, B. J.
Bibcode: 2005AGUFMSH13A0303T
Altcode:
  The LASCO coronagraphs on board SOHO have detected hundreds of
  halo coronal mass ejections, exhibiting a wide range of speeds and
  propagation morphologies. However, it is important to distinguish which
  aspects of the halo CME are due to erupting material, or "new mass," and
  which aspects are due to the motion of pre-existing structures. We have
  established a means of determining which aspects of halo CME emission
  are due to newly added mass to the corona, and which aspects of halo
  CME emission are due to the deflection of bright structures towards the
  sky, thereby increasing their scattering efficiency. By mapping the CME
  brightening into the pre-existing corona, it can be shown that some of
  the emission in halo CMEs has a positive correlation with pre-event
  features, which can only explained if we include the contribution of
  streamer motion to the CME brightness. Differentiating between these two
  sources of CME brightness (and apparent mass) is extremely important
  because it allows better determination of the CME mass, morphology,
  and direction of propagation, providing a better linkage to Earth. We
  will discuss several events from different viewing angles, and will
  suggest an algorithm that can be implemented in near-real time for
  forecasting purposes.

Title: Sequential Chromospheric Brightenings beneath a Transequatorial
    Halo Coronal Mass Ejection
Authors: Balasubramaniam, K. S.; Pevtsov, A. A.; Neidig, D. F.; Cliver,
   E. W.; Thompson, B. J.; Young, C. A.; Martin, S. F.; Kiplinger, A.
Bibcode: 2005ApJ...630.1160B
Altcode:
  Analyses of multiwavelength data sets for a solar eruption at ~21:30
  UT on 2002 December 19 show evidence for the disappearance of a
  large-scale, transequatorial coronal loop (TL). In addition, coronal
  manifestations of the eruption (based on SOHO EIT and LASCO images)
  include large-scale coronal dimming, flares in each associated active
  region in the northern and southern hemispheres, and a halo CME. We
  present detailed observations of the chromospheric aspects of this
  event based on Hα images obtained with the ISOON telescope. The
  ISOON images reveal distant flare precursor brightenings, sympathetic
  flares, and, of most interest herein, four nearly cospatial propagating
  chromospheric brightenings. The speeds of the propagating disturbances
  causing these brightenings are 600-800 km s<SUP>-1</SUP>. The inferred
  propagating disturbances have some of the characteristics of Hα
  and EIT flare waves (e.g., speed, apparent emanation from the flare
  site, subsequent filament activation). However, they differ from
  typical Hα chromospheric flare waves (also known as Moreton waves)
  because of their absence in off-band Hα images, small angular
  arc of propagation (&lt;30°), and their multiplicity. Three of
  the four propagating disturbances consist of a series of sequential
  chromospheric brightenings of network points that suddenly brighten in
  the area beneath the TL that disappeared earlier. SOHO MDI magnetograms
  show that the successively brightened points that define the inferred
  propagating disturbances were exclusively of one polarity, corresponding
  to the dominant polarity of the affected region. We speculate that
  the sequential chromospheric brightenings represent footpoints of
  field lines that extend into the corona, where they are energized in
  sequence by magnetic reconnection as coronal fields tear away from
  the chromosphere during the eruption of the transequatorial CME. We
  report briefly on three other events with similar narrow propagating
  disturbances that were confined to a single hemisphere.

Title: On the Origins of Solar EIT Waves
Authors: Cliver, E. W.; Laurenza, M.; Storini, M.; Thompson, B. J.
Bibcode: 2005ApJ...631..604C
Altcode:
  Approximately half of the large-scale coronal waves identified in
  images obtained by the Extreme-Ultraviolet Imaging Telescope (EIT) on
  the Solar and Heliospheric Observatory from 1997 March to 1998 June
  were associated with small solar flares with soft X-ray intensities
  below C class. The probability of a given flare of this intensity
  having an associated EIT wave is low. For example, of ~8,000 B-class
  flares occurring during this 15 month period, only ~1% were linked to
  EIT waves. These results indicate the need for a special condition that
  distinguishes flares with EIT waves from the vast majority of flares
  that lack wave association. Various lines of evidence, including the
  fact that EIT waves have recently been shown to be highly associated
  with coronal mass ejections (CMEs), suggest that this special condition
  is a CME. A CME is not a sufficient condition for a detectable EIT wave,
  however, because we calculate that ~5 times as many front-side CMEs
  as EIT waves occurred during this period, after taking the various
  visibility factors for both phenomena into account. In general, EIT
  wave association increases with CME speed and width.

Title: Putting the Rubber to the Road: The Whos, Whys and Hows of
    the International Heliophysical Year 2007
Authors: Thompson, B. J.; Davila, J. M.; Drobnes, E.; Gopalswamy,
   N.; Wesenberg, R. P.
Bibcode: 2005AGUSM.U23A..07T
Altcode:
  In 1957 a program of international research, inspired by the
  International Polar Years of 1882 and 1932, was organized as the
  International Geophysical Year (IGY) to study global phenomena
  of the Earth and geospace. Fifty years later, the world's science
  community will again come together for international programs of
  scientific collaboration: the International Heliophysical Year
  (IHY), the electronic Geophysical Year (eGY), and the International
  Polar Year (IPY) 2007. This time, research will extend out into the
  heliosphere to focus on solar-terrestrial-planetary interactions. The
  ambitious plans for the IHY, eGY and IPY incorporate the activities
  of scientists in 191 nations, the "IGY Gold" Historical Preservation
  initiative, a series of coordinated campaigns involving more than
  100 instruments and models, education and public outreach programs,
  a developing nations instrument development program, and opportunities
  for supported research worldwide. The presentation will focus on the
  efforts and operations which will make these activities possible.

Title: Multialtitude Observations of a Coronal Jet during the Third
    Whole Sun Month Campaign
Authors: Ko, Y. -K.; Raymond, J. C.; Gibson, S. E.; Alexander, D.;
   Strachan, L.; Holzer, T.; Gilbert, H.; Cyr, O. C. St.; Thompson, B. J.;
   Pike, C. D.; Mason, H. E.; Burkepile, J.; Thompson, W.; Fletcher, L.
Bibcode: 2005ApJ...623..519K
Altcode:
  On 1999 August 26, a coronal jet occurred at the northwest limb near
  a sigmoid active region (AR 8668) that was the target for a joint
  observation plan (SOHO joint observing program 106) during the third
  Whole Sun Month Campaign. This jet was observed by several instruments
  at the limb (SOHO/CDS, SOHO/EIT, TRACE, and Mauna Loa Solar Observatory
  CHIP and PICS) and at 1.64 R<SUB>solar</SUB> (SOHO/UVCS). At the limb,
  this jet event displayed both low- and high-temperature components. Both
  high- and low-temperature components were evident during the early phase
  (first 20 minutes) of the event. However, the low-temperature component
  is maintained for ~1 hr after the higher temperature component is
  gone. There is a second brightening (a possible second jet) seen by
  EIT and TRACE about 50 minutes after the onset of the first jet. The
  line-of-sight motion at the limb began with a 300 km s<SUP>-1</SUP>
  redshift and evolved to a 200 km s<SUP>-1</SUP> blueshift. At
  1.64 R<SUB>solar</SUB>, the intensities of Lyα and Lyβ in the jet
  increased by a factor of several hundred compared with the background
  corona. The C III λ977 line also brightened significantly. This
  indicates low-temperature [~(1-2)×10<SUP>5</SUP> K] emission in the
  jet, while the intensities of O VI λ1032 and O VI λ1037 increased
  by as much as a factor of 8. The UVCS data show evidence of heating at
  the early phase of the event. The Doppler shift in the lines indicates
  that the line-of-sight (LOS) velocity in the jet started from ~150
  km s<SUP>-1</SUP> in blueshift and ended at ~100 km s<SUP>-1</SUP>
  in redshift. This LOS motion seen at 1.64 R<SUB>solar</SUB> was
  apparently opposite to what was observed when the jet emerged from the
  limb. The Doppler dimming analysis indicates that the radial outflow
  speed correlates with the magnitude of the LOS speed. Interestingly,
  UVCS observations at 2.33 and 2.66 R<SUB>solar</SUB> show no trace of
  the jet and SOHO/LASCO observations also yield no firm detection. We
  find that a simple ballistic model can explain most of the dynamical
  properties of this jet, while the morphology and the thermal properties
  agree well with reconnection-driven X-ray jet models.

Title: High-Cadence Radio Observations of an EIT Wave
Authors: White, S. M.; Thompson, B. J.
Bibcode: 2005ApJ...620L..63W
Altcode:
  Sensitive radio observations of the 1997 September 24 EIT wave show
  its velocity to be 830 km s<SUP>-1</SUP>. The wave first appears a
  short distance from the flare site, and its trajectory projects back to
  the flare site at the peak of the impulsive phase. The radio spectrum
  appears to be consistent with optically thin coronal emission rather
  than chromospheric emission. The observed radio brightness temperatures
  are consistent with the EIT fluxes if the temperature of the emitting
  gas is not at the peak formation temperature of the Fe XII 195 Å line
  or if abundances are closer to photospheric than coronal. An important
  result is that no deceleration is observed during the 4 minutes that the
  wave is visible in the radio images: the discrepancy between EIT wave
  and Hα Moreton wave speeds requires that EIT waves slow substantially
  as they propagate, if they are the same disturbance.

Title: Development and calibration of major components for the
    STEREO/PLASTIC (plasma and suprathermal ion composition) instrument
Authors: Blush, L. M.; Allegrini, F.; Bochsler, P.; Daoudi, H.;
   Galvin, A.; Karrer, R.; Kistler, L.; Klecker, B.; Möbius, E.; Opitz,
   A.; Popecki, M.; Thompson, B.; Wimmer-Schweingruber, R. F.; Wurz, P.
Bibcode: 2005AdSpR..36.1544B
Altcode:
  The plasma and suprathermal ion composition (PLASTIC) instrument will
  measure kinetic properties and charge states of solar wind ions and
  suprathermal ions as part of the solar terrestrial relations observatory
  (STEREO) mission. Two identical instruments located on separate
  spacecraft will provide in situ plasma measurements at ∼1 AU to study
  physical processes low in the corona and in the inner heliosphere. In
  conjunction with the other in situ and remote sensing instruments
  of STEREO, as well as existing near-Earth observatories, the PLASTIC
  instrument measurements will contribute to the understanding of the
  three-dimensional structure of the heliosphere, with particular focus
  on Coronal Mass Ejections. As the primary solar wind instrument aboard
  STEREO, PLASTIC will measure bulk solar wind plasma parameters (density,
  velocity, temperature, temperature anisotropy, and alpha/proton ratio)
  and the distribution functions and charge state distributions of major
  heavy solar wind ions (e.g., C, O, Ne, Mg, Si, Fe). The measurement
  apparatus includes an electrostatic deflection analyzer for energy
  per charge measurement ( E/ q), a time-of-flight section utilizing
  carbon foils and microchannel plate detectors for time of flight
  measurement ( TOF), and solid-state detectors for energy measurement
  ( E). The instrument will provide a large instantaneous field of view
  (in-ecliptic and out-of-ecliptic angles distinguished) with measurements
  taken at high time resolution (1-5 min) spanning an ion energy range
  of 0.25-87 keV/e. To accommodate a large range of particle fluxes, the
  PLASTIC Entrance System employs collection apertures with different
  geometric factors for the bulk solar wind (H ∼ 96%, He ∼ 4%) and
  for the heavy, less-abundant ions (&lt;1%) and suprathermal ions. This
  paper focuses on the hardware development of major components for the
  PLASTIC instrument. The PLASTIC measurement principle is explained
  along with a presentation of the ion optic calibrations of the flight
  model Entrance Systems as well as calibrations of the microchannel
  plates and solid-state detectors.

Title: The Solar Energetic Particle Event of 16 August 2001: ~
    400 MeV Protons Following an Eruption at ~ W180
Authors: Cliver, E. W.; Thompson, B. J.; Lawrence, G. R.; Zhukov,
   A. N.; Tylka, A. J.; Dietrich, W. F.; Reames, D. V.; Reiner, M. J.;
   MacDowall, R . J.; Kosovichev, A. G.; Ling, A. G.
Bibcode: 2005ICRC....1..121C
Altcode: 2005ICRC...29a.121C
  No abstract at ADS

Title: The Plasma and SupraThermal Ion Composition (PLASTIC)
Instrument: Final Diagnostic Development Phase for the STEREO Mission
Authors: Blush, L. M.; Bochsler, P.; Daoudi, H.; Galvin, A.; Karrer,
   R.; Kistler, L.; Klecker, B.; Möbius, E.; Opitz, A.; Popecki, M.;
   Thompson, B.; Wimmer-Schweingruber, R.; Wurz, P.
Bibcode: 2004AGUFMSH21B0410B
Altcode:
  The PLAsma and SupraThermal Ion Composition (PLASTIC) instrument
  project is entering the final phases of instrument development prior
  to integration with the Solar Terrestrial Relations Observatory
  (STEREO) spacecraft in early 2005. The STEREO mission will provide
  a unique opportunity to investigate the 3-dimensional structure of
  the heliosphere, with particular focus on the origin, evolution, and
  propagation of Coronal Mass Ejections (CMEs). The mission also seeks to
  determine the sites and mechanisms of energetic particle acceleration as
  well as develop a 3-D time-dependent understanding of the ambient solar
  wind properties. As one of four STEREO instrument packages coordinating
  remote sensing and in situ measurements, the PLASTIC instruments
  will diagnose properties of the solar wind and suprathermal protons,
  alphas, and heavy ions. PLASTIC will determine bulk solar wind plasma
  parameters (density, velocity, temperature, temperature anisotropy,
  and alpha/proton ratio) and the distribution functions of major
  heavy solar wind ions in the energy per charge range 0.25-100keV/e. A
  full characterization of the solar wind and suprathermal ions will
  be achieved with a system that measures ion energy per charge (E/q),
  ion velocity distribution (ěc v), and ion energy (E). Two identical
  PLASTIC instruments located on the separate spacecraft will provide
  in situ plasma measurements in order to study physical processes low
  in the corona and in the inner heliosphere. Elemental and charge state
  abundances provide tracers of the ambient coronal plasma, fractionated
  populations from coronal and heliospheric events, and local source
  populations of energetic particle acceleration. In this presentation,
  the PLASTIC operation principles and aims will be presented along with a
  review of development status and current instrument calibration results.

Title: Coronal Shocks of November 1997 Revisited: The Cme Type II
    Timing Problem
Authors: Cliver, E. W.; Nitta, N. V.; Thompson, B. J.; Zhang, J.
Bibcode: 2004SoPh..225..105C
Altcode:
  We re-examine observations bearing on the origin of metric type
  II bursts for six impulsive solar events in November 1997. Previous
  analyses of these events indicated that the metric type IIs were due to
  flares (either blast waves or ejecta). Our point of departure was the
  study of Zhang et al. (2001) based on the Large Angle and Spectrometric
  Coronagraph's C1 instrument (occulting disk at 1.1 R<SUB>0</SUB>) that
  identified the rapid acceleration phase of coronal mass ejections (CMEs)
  with the rise phase of soft X-ray light curves of associated flares. We
  find that the inferred onset of rapid CME acceleration in each of the
  six cases occurred 1-3 min before the onset of metric type II emission,
  in contrast to the results of previous studies for certain of these
  events that obtained CME launch times ∼25-45 min earlier than type
  II onset. The removal of the CME-metric type II timing discrepancy in
  these events and, more generally, the identification of the onset of
  the rapid acceleration phase of CMEs with the flare impulsive phase
  undercuts a significant argument against CMEs as metric type II shock
  drivers. In general, the six events exhibited: (1) ample evidence
  of dynamic behavior [soft X-ray ejecta, extreme ultra-violet imaging
  telescope (EIT) dimming onsets, and wave initiation (observed variously
  in Hα, EUV, and soft X-rays)] during the inferred fast acceleration
  phases of the CMEs, consistent with the cataclysmic disruption of the
  low solar atmosphere one would expect to be associated with a CME; and
  (2) an organic relationship between EIT dimmings (generally taken to
  be source regions of CMEs) and EIT waves (which are highly associated
  with metric type II bursts) indicative of a CME-driver scenario. Our
  analysis indicates that the broad (∼90° to halo) CMEs observed in
  the outer LASCO coronagraphs for these impulsive events began life
  as relatively small-scale structures, with angular spans of ∼15°
  in the low corona. A review of on-going work bearing on other aspects
  (than timing) of the question of the origin of metric type II bursts
  (CME association; connectivity of metric and decametric-hectometric
  type II shocks; spatial relationship between CMEs and metric shocks)
  leads to the conclusion that CMEs remain a strong candidate to be
  the principal/sole driver of metric type II shocks vis-à-vis flare
  blast waves/ejecta.

Title: Reply to Comment on ``Moving Beyond the IGY: The Electronic
    Geophysical Year (eGY) Concept''
Authors: Baker, Daniel; Barton, Charles; Rodger, Alan; Fraser, Brian;
   Thompson, Barbara; Papitashvili, Vladimir
Bibcode: 2004EOSTr..85Q.302B
Altcode:
  Robert Benson raises interesting points regarding the eGY and the role
  of world data centers. We share the belief that the WDC system was
  one of the great achievements of the IGY. We have also supported the
  many and varied activities of data centers over the years. The eGY is
  not intended to replace data centers, but rather to enhance them. We
  believe that data center holdings should be even more accessible than
  is presently the case, and that governments should support more, not
  less, active archiving and tending of data. We sincerely hope that
  people in the community do not interpret the eGY concept as in any
  way advocating the disbanding of active data centers.

Title: A Comparison of CME-Associated Atmospheric Waves Observed in
    Coronal (Fe XII 195 Å) and Chromospheric (He I 10830 Å) Lines
Authors: Gilbert, Holly R.; Holzer, Thomas E.; Thompson, Barbara J.;
   Burkepile, Joan T.
Bibcode: 2004ApJ...607..540G
Altcode:
  Although ``Moreton'' waves have historically been observed in Hα
  data, more recently waves have also been observed in chromospheric
  He I λ10830 images obtained at the Mauna Loa Solar Observatory. In
  an effort to better understand the nature of chromospheric waves and
  their relationship to coronal waves observed in EUV Imaging Telescope
  (EIT) data, we focus on two events in which waves are observed
  simultaneously in He I λ10830 and Fe XII λ195, lines that are formed
  in the chromosphere and the corona, respectively. Comparing the waves
  observed in these two lines allows the determination of the spatial
  relationship between coronal and chromospheric waves and thus aids
  in the understanding of the underlying physics of waves in the solar
  atmosphere. The main goal of this work is to begin an investigation
  into whether both coronal and chromospheric waves are mechanical
  (e.g., MHD waves) by looking at their spatial relationship. We find
  that the chromospheric waves in these two events are cospatial with
  their coronal counterparts, indicating that they are not mechanical in
  nature but are chromospheric imprints of mechanical waves propagating
  through the corona. This conclusion is based on the nature of the
  formation of the He I absorption line.

Title: Development of MHD Wave Diagnostic and Models of Coronal
    Active Regions
Authors: Ofman, L.; Thompson, B. J.; Davila, J. M.
Bibcode: 2004AAS...204.9504O
Altcode: 2004BAAS...36..826O
  We investigate the generation, propagation, and damping of MHD waves in
  active regions, with the goal to develop a diagnostic tool of active
  region structure, dynamics, and stability. We used 3D MHD model to
  study the generation and the propagation of EIT waves in a simple
  model of an active regions, and the interaction of EIT waves with
  the active region magnetic field. We model the oscillation of active
  region loops numerically using the 3D MHD model active regions. Such
  oscillations have been recently observed by TRACE. We use photospheric
  magnetograms as the boundary conditions for the magnetic field model,
  and construct an initial field using force-free extrapolation. Finite
  plasma temperature, density, and gravity are included in the model. We
  construct loop density structures in the model, guided by TRACE and EIT
  observations in the EUV. We demonstrate that by comparing the results
  of the MHD models of waves in an active region to observations we will
  be able to construct a diagnostic tool for the physical properties of
  the active regions, such as magnetic field and density structure.

Title: Multi-Altitude Observations of a Coronal Jet
Authors: Ko, Y. -K.; Raymond, J. C.; Gibson, S. E.; Alexander, D.;
   Strachan, L.; Holzer, T.; Gilbert, H.; St. Cyr, O. C.; Thompson,
   B. J.; Pike, C. D.; Burkepile, J.; Thompson, W.; Fletcher, L.
Bibcode: 2004AAS...204.5413K
Altcode: 2004BAAS...36..759K
  A coronal jet occurred on August 26, 1999 at the NW limb near a sigmoid
  active region (AR8668). This jet was observed by several instruments
  at the limb (SOHO/CDS, SOHO/EIT, TRACE, MLSO/CHIP, MLSO/PICS) and
  at 1.64 Ro (SOHO/UVCS). At the limb, this jet event has both low and
  high temperature components. The high temperature component appeared
  at the early phase (first 20 minutes) of the event along with the low
  temperature component while the latter seems to last long ( ∼ 1 hour)
  after the higher temperature component was gone. The line-of-sight
  motion at the limb started with red-shifted (by as much as 300 km/s)
  and turned blue-shifted (by as much as 200 km/s). At 1.64 Ro, the
  intensities of Lyα , Lyβ in the jet increased by a factor of several
  hundreds compared with the background corona. C III λ 977 line also
  brightened significantly. This indicates low temperature ( ∼ 1-2×
  10<SUP>5</SUP> K) emission in the jet, while the intensities of O VI
  λ 1032 and O VI λ 1037 increased by a factor of as large as 8. Both
  UVCS and CDS data show evidence of heating at the early phase of the
  event. The line-of-sight velocity seen at 1.64 Ro started with ∼ 150
  km/sec in blue shift and ended at ∼ 100 km/sec in red shift. This is
  apparently opposite to what were observed when the jet emerged from
  the limb. The Doppler dimming analysis indicates that the radial
  outflow speed correlates with the magnitude of the line-of-sight
  speed. Interestingly, UVCS observations at 2.33 and 2.66 Ro show no
  trace of the jet and LASCO observations also yield no firm sight of the
  jet. In this paper, we present the observations by these instruments
  and discuss the dynamical structure and physical properties of this
  jet. Y.-K. Ko acknowledges the support by NASA grant NAG5-12865.

Title: The electronic Geophysical Year (eGY) 2007-2008
Authors: Barton, C.; Baker, D. N.; Fraser, B.; Papitashvili, V.;
   Rodger, A.; Thompson, B.; Allen, J. H.; Arora, B.; Kerridge, D.;
   Kamide, Y.
Bibcode: 2004AGUSM.U23A..03B
Altcode:
  An Electronic Geophysical Year (eGY) is planned for 2007/08 as a
  50-year sequel to the highly successful International Geophysical
  Year. The central objective is to bring the management of geoscientific
  information worldwide into the 21st century through an e-Science
  approach and the development of virtual observatories. The challenge in
  1957-58 was to acquire and make available to the world community the
  observational data required to build a comprehensive understanding
  of the Earth and its processes. That challenge remains and is
  yet more pressing because of the growing demands we place on our
  natural resources and environment. Our observational data gathering
  capabilities have expanded enormously during the past 50 years,
  particularly through space-based observations. For example, the US
  National Virtual Observatory will be adding 500 TB of astronomical
  data per year from 2004. This proliferation of data requires a modern,
  distributed approach to data management and dissemination. To meet
  this challenge, we have at our disposal the power of the Internet
  and grid computing infrastructures for data sharing, processing,
  and visualization. The eGY concept arose within the International
  Union of Geodesy and Geophysics, with support from the Scientific
  Committee on Solar-Terrestrial Physics, the International Union of
  Geological Sciences, and the Society of Exploration Geophysicists, as
  a means of providing an international focus for e-Science and virtual
  observatory development across all the geosciences. It provides a
  common thread among other global geoscientific initiatives - the 4th
  International Polar Year, the International Year of Planet Earth,
  the International Heliospheric Year, and Climate and Weather of the
  Sun-Earth System. Virtual observatories provide exciting prospects
  in the geosciences, and are under varying stages of development, for
  example the Virtual Seismic Network (http://equinfo.ucsd.edu/vsn/),
  the Virtual Solar Observatory (http://vso.nso.edu/), and the Virtual
  Geomagnetic Observatory (http://maggy.emgin.umich.edu/mist/). It is
  only a matter of time before virtual observatories are a standard
  feature across all the discipline areas within the geosciences, and
  add a new dimension to the role of the World Data Centers.

Title: Moving Beyond the IGY: The Electronic Geophysical Year
    (eGY) Concept
Authors: Baker, D. N.; Barton, C.; Rodger, A. S.; Fraser, B.; Thompson,
   B.; Papitashvili, V.
Bibcode: 2004EOSTr..85..105B
Altcode:
  The International Geophysical Year (1957-1958) was inspired by the
  realization that much better and more complete information was needed
  about the Earth and geospace to understand and manage the complete
  terrestrial environment on which we depend. So it was that the IGY
  member countries worked together to deploy a large number of geophysical
  observatories around the world. These nations were pursuing the major
  IGY objectives to collect geophysical data as widely as possible,
  and to provide free access to these data for all scientists around
  the globe. About 50 permanent stations were set up in the Arctic
  and Antarctic, and the World Data Center System was established
  to ensure that the data collected were properly archived and made
  available without restrictions for scientific research and practical
  applications. IGY was an outstanding success. It elevated geophysical
  monitoring to a new level, and set new standards for international
  collaboration and data-sharing. Many successes of the geophysical
  sciences in recent times have origins that can be traced back to the
  IGY. A notable example is the modern era of space exploration. As we
  approach the 50-year anniversary of the IGY, it is appropriate to seek
  to build on the IGY achievements through renewed global resolves as well
  as to review the outcomes of the IGY and celebrate its successes. This
  is the ``IGY+50'' concept.

Title: Moving Beyond IGY: An Electronic Geophysical Year (eGY) Concept
Authors: Baker, D. N.; Barton, C. E.; Rodger, A. S.; Thompson, B. J.;
   Fraser, B.; Papitashvili, V.
Bibcode: 2003AGUFM.U21A..01B
Altcode:
  During the International Geophysical Year (1957-1958), member countries
  established many new geophysical observatories pursuing the major IGY
  objectives - to collect geophysical data as widely as possible and
  to provide free access to these data for all scientists around the
  globe. Today, geophysics has attained a rather good understanding
  within traditional regions, i.e., the atmosphere, ionosphere,
  magnetosphere, and other such geospheres. At the same time, it has
  become clear that much of the new and important science is coming
  from the studies of interfaces and coupling between geospheres. Thus,
  if geophysical data are made `'transparently'' available to a much
  wider range of scientists and students than to those who do the
  observations, then new and exciting discoveries can be expected. An
  International Association of Geomagnetic and Aeronomy (IAGA) task force,
  recognizing that a key achievement of the IGY was the establishment
  of a worldwide system of data centers and physical observatories,
  proposes that for the 50th anniversary of IGY, the worldwide scientific
  community should endorse and promote an electronic Geophysical Year
  (eGY) initiative. The proposed eGY concept would both commemorate
  the IGY in 2007-2008 and provide a forward impetus to geophysics
  in 21st century, similar to that provided by the IGY fifty years
  ago. The IAGA task force strongly advocates: (1) Securing permission
  and release of existing data; (2) Creating access to information;
  and (3) Conversion of relevant analog data to digital form. The eGY
  concept embraces all available and upcoming geophysical data (e.g.,
  atmospheric, ionospheric, geomagnetic, gravity, etc.) through the
  establishment of a series of virtual geophysical observatories now
  being `'deployed'' in cyberspace. The eGY concept is modern, global,
  and timely; it is attractive, pragmatic, and affordable. The eGY is
  based on the existing and continually developing computing/networking
  technologies (e.g., XML, Semantic Web, etc.) and international cyber
  infrastructure. Moreover, the International Union of Geodesy and
  Geophysics (IUGG) has supported the eGY concept, which can smoothly be
  incorporated into various existing `'International Year'' initiatives -
  such as the International Polar Year, International Heliophysical Year,
  or International Year of the Planet Earth.

Title: A Survey of Coronal Dimmings and EIT Wave Transients
Authors: West, M.; Thompson, B. J.
Bibcode: 2003AGUFMSH22B..01W
Altcode:
  We present the results of a comprehensive catalog of EIT wave
  transients and coronal dimmings. We will compiled a set of more than
  170 events, and we present strong evidence for the association of
  the co-development of coronal dimmings and EIT waves. Both limb and
  disk events are included in this study. We also include the speeds,
  locations, and associated flare timing in this study.

Title: Large solar energetic particle events of cycle 23: A global
    view
Authors: Gopalswamy, N.; Yashiro, S.; Lara, A.; Kaiser, M. L.;
   Thompson, B. J.; Gallagher, P. T.; Howard, R. A.
Bibcode: 2003GeoRL..30.8015G
Altcode: 2003GeoRL..30lSEP3G
  We report on a study of all the large solar energetic particle
  (SEP) events that occurred during the minimum to maximum interval
  of solar cycle 23. The main results are: 1. The occurrence rate of
  the SEP events, long-wavelength type II bursts and the fast and wide
  frontside western hemispheric CMEs is quite similar, consistent with the
  scenario that CME-driven shocks accelerate both protons and electrons;
  major flares have a much higher rate. 2. The SEP intensity is better
  correlated with the CME speed than with the X-ray flare class. 3. CMEs
  associated with high-intensity SEPs are about 4 times more likely to
  be preceded by wide CMEs from the same solar source region, suggesting
  the importance of the preconditioning of the eruption region. We use
  a specific event to demonstrate that preceding eruption from a nearby
  source can significantly affect the properties of SEPs and type II
  radio bursts.

Title: High-Energy <SUP>3</SUP>He-Rich Solar Particle Events
Authors: Torsti, Jarmo; Kocharov, Leon; Laivola, Jarno; Chertok,
   Ilya; Thompson, Barbara J.
Bibcode: 2003SoPh..214..177T
Altcode:
  Energetic particle observations of the ERNE instrument on board SOHO
  enable measurements of <SUP>3</SUP>He and <SUP>4</SUP>He fluxes beyond
  15 MeV nucleon<SUP>−1</SUP> with good statistical resolution. We
  report results of a survey of the ERNE observations covering the period
  from 8 February 1999 to 6 December 2000. We find 10 and 5 days during
  which the <SUP>3</SUP>He-to-<SUP>4</SUP>He ratio exceeds the levels
  of 20% and 50%, respectively. Those periods include, in particular,
  four <SUP>3</SUP>He-rich events that are sufficiently strong for
  a reasonably accurate estimate of the time-intensity profiles. We
  analyze the history of solar and interplanetary phenomena associated
  with these high-energy <SUP>3</SUP>He-rich events. Basic properties
  of such events and significant solar and interplanetary factors are
  formulated. The significant factors comprise, in particular, a strong,
  impulsive flare, typically observed about day before the <SUP>3</SUP>He
  onset, and an interplanetary shock wave or magnetic field enhancement
  arriving at 1 AU about frac43 day after the <SUP>3</SUP>He onset. The
  high-energy <SUP>3</SUP>He-rich events make up a new kind of hybrid
  events, possessing the impulsive-type composition and the gradual-type
  time-profiles. We emphasize a dependence of the resultant particle
  event on the history of the particular solar eruption comprising
  coronal mass ejection (CME) and the flare associated with the CME.

Title: The "Whole Sun Month" Campaigns As a Prototype for IHY
Authors: Thompson, B. J.; Biesecker, D. A.; Breen, A. R.; Gibson, S. E.
Bibcode: 2003EAEJA....11571T
Altcode:
  The International Heliophysical Year (IHY) in 2007 will consist of
  a series of coordinated observations combining data and models from
  an expansive group of international participants. Campaigns will be
  planned to target all aspects of heliophysics, including solar and
  interplanetary physics, geospace science and the climatary impact
  on Earth. These campaigns will require extensive coordination to
  ensure that available ground-based and space missions are utilized
  to the greatest scientific benefit. The "Whole Sun Month" campaigns
  serve as an excellent prototype for IHY. The first Whole Sun Month
  campaign (10 August - 8 September 1996) consisted of an entire
  month of coordinated solar and heliospheric observations, followed
  by workshops which combined the analysis of the campaign data with
  the utilization of these data to constrain interpretive 3-D models
  solar and heliospheric structure. The subsequent campaigns (in 1998
  and 1999) targetted more specific topics, again allowing a broad base
  of participants to establish a comprehensive base of observations for
  model interpretation. The many scientific successes of the Whole Sun
  Month campaigns (publications, workshops, model refinement and ongoing
  collaborations) and the framework of campaign coordination provides an
  excellent basis for the planning of IHY campaigns. We will discuss the
  campaigns in detail and begin an outline for how the campaigns could
  be expanded to incorporate more observations and a greater timeline
  for IHY.

Title: Drinking From the Data Firehose: The SDO Ground System
Authors: Pages, R.; Potter, W. J.; Thompson, B. J.
Bibcode: 2002AGUFMSH21C..07P
Altcode:
  The Solar Dynamics Observatory will generate an unprecedented space
  science data stream of 150 Mbps. The primary challenge of the SDO Ground
  System is to provide continuous, near-real-time science delivery of
  the large volumes of science data. Other challenges include high data
  completeness requirements and utilization of a new Ka band antenna
  network for the data capture. The presentation will report on the
  progress of the SDO Ground Systems team in designing a cost-effective,
  reliable ground system for SDO.

Title: Two wave morphologies in SOHO/EIT - EIT waves and Moreton waves
Authors: Biesecker, D. A.; Thompson, B. J.; Hudson, H. S.; Warmuth,
   A.; White, S.
Bibcode: 2002AGUFMSH52A0450B
Altcode:
  EIT waves are global waves observed to propagate across quiet
  coronal field regions in the SOHO/EIT data. The waves are initiated in
  association with other transient activity. The literature now contains
  many references to EIT waves and observers have published observations
  of associated waves at a variety of wavelengths. We show in this
  poster that there is confusion in the literature as to what an EIT
  wave is. We use YOHKOH SXT, Nobeyama Radioheliograph and He I 10830A
  observations to show that the EIT instrument observes waves with two
  distinct properties and morphologies. These two morphologies correspond
  to the classical Moreton wave and to what we call the EIT wave. The
  Moreton waves in EIT appear as a sharp, bright feature, travelling at
  super-Alfvenic velocities. The EIT waves instead appear as a diffuse,
  faint feature, moving at relatively slower velocities. The EIT waves
  appear much more frequently than the Moreton waves and Moreton waves
  are usually seen in tandem with EIT waves. Both types of waves have
  been modelled by various researchers as MHD waves.

Title: The SDO Mission
Authors: Schwer, K.; Lilly, R. B.; Thompson, B. J.; Brewer, D. A.
Bibcode: 2002AGUFMSH21C..01S
Altcode:
  The Solar Dynamics Observatory, scheduled to launch in August 2007, will
  view the Sun continuously from an inclined geosynchronous orbit. The
  spacecraft will be a robust, three-axis stabilized spacecraft with
  low jitter and will deliver 150 Mbps of continuous high rate data. The
  spacecraft will be built, tested and integrated in-house at the NASA
  Goddard Space Flight Center, with four instruments to be developed
  by three Principal Investigator teams. The primary challenges include
  maintaining an ambitious schedule, designing a communications and ground
  system which can handle an unprecedented volume of space science data,
  and a baseline of five years reliability. The presentation will focus
  on the progress of the GSFC SDO Project team in developing the Solar
  Dynamics Observatory.

Title: EUV Dimmings: Simple or Enigmatic?
Authors: Thompson, B.; Biesecker, D. A.; Ofman, L.; St. Cyr, O. C.;
   Wills-Davey, M. J.
Bibcode: 2002AGUFMSH52A0488T
Altcode:
  EUV dimmings are large-scale depletions in coronal EUV emission
  associated with coronal mass ejections. Their occurrence is nearly
  perfect in correlation with fast CMEs. Many of the EUV dimming
  observations appear to correspond well in appearance and behavior to
  SXR dimmings. It has been assumed that the dimmings are merely the
  location of the CME mass removal in the corona, and that their similar
  appearance to coronal holes is because they are transient coronal
  holes with fieldlines opened by the coronal mass ejection. However,
  not all CMEs have dimmings, and large-scale EUV dimmings have also
  been caused by heating of local plasma, and due to absorption by cool
  material "clouds" evolving in the wake of an eruption. Additionally,
  there are several ways in which these regions "heal," presumably due to
  the closing down of the open field lines. The presentation will include
  a range of EUV dimming observations, a discussion of their origin,
  and what they might imply about the nature of the associated CMEs.

Title: SDO: A Systems Challenge
Authors: Ruffa, J.; Ward, D. K.; Anderson, T. A.; Schwer, K. O.;
   Thompson, B. J.
Bibcode: 2002AGUFMSH51A0435R
Altcode:
  The Solar Dynamics Observatory, scheduled to launch in August 2007,
  presents several significant challenges to the Systems Engineering
  team. The spacecraft will be built, tested and integrated in-house
  at the NASA Goddard Space Flight Center, with four instruments to
  be developed by three Principal Investigator teams. Though few new
  technologies are required in developing a robust, reliable and versatile
  spacecraft, the combination of numerous requirements (scientific and
  otherwise) require a significant effort to ensure complete mission
  success. The presentation will include a discussion of the SDO
  subsystems and the status of the SDO Systems Engineering team efforts.

Title: The International Heliophysical Year (IHY)
Authors: Davila, J. M.; Harrison, R.; Poland, A.; Thompson, B.;
   Gopalswamy, N.
Bibcode: 2002AGUFMSH21A0518D
Altcode:
  In 1957 a program of international research, inspired by the
  International Polar Years of 1882-83 and 1932-33, was organized as
  the International Geophysical Year (IGY) to study global phenomena of
  the Earth and geospace. The IGY involved about 60,000 scientists from
  66 nations, working at thousands of stations, from pole to pole to
  obtain simultaneous, global observations on Earth and in space. There
  had never been anything like it before. The fiftieth anniversary of
  the International Geophysical Year will occur in 2007. We propose to
  organize an international program of scientific collaboration for this
  time period called the International Heliophysical Year (IHY). Like
  it predecessors, the IHY will focus on fundamental global questions
  of Earth science.

Title: The Structure and Evolution of a Sigmoidal Active Region
Authors: Gibson, S. E.; Fletcher, L.; Del Zanna, G.; Pike, C. D.;
   Mason, H. E.; Mandrini, C. H.; Démoulin, P.; Gilbert, H.; Burkepile,
   J.; Holzer, T.; Alexander, D.; Liu, Y.; Nitta, N.; Qiu, J.; Schmieder,
   B.; Thompson, B. J.
Bibcode: 2002ApJ...574.1021G
Altcode:
  Solar coronal sigmoidal active regions have been shown to be precursors
  to some coronal mass ejections. Sigmoids, or S-shaped structures,
  may be indicators of twisted or helical magnetic structures, having
  an increased likelihood of eruption. We present here an analysis of a
  sigmoidal region's three-dimensional structure and how it evolves in
  relation to its eruptive dynamics. We use data taken during a recent
  study of a sigmoidal active region passing across the solar disk
  (an element of the third Whole Sun Month campaign). While S-shaped
  structures are generally observed in soft X-ray (SXR) emission, the
  observations that we present demonstrate their visibility at a range of
  wavelengths including those showing an associated sigmoidal filament. We
  examine the relationship between the S-shaped structures seen in SXR
  and those seen in cooler lines in order to probe the sigmoidal region's
  three-dimensional density and temperature structure. We also consider
  magnetic field observations and extrapolations in relation to these
  coronal structures. We present an interpretation of the disk passage
  of the sigmoidal region, in terms of a twisted magnetic flux rope
  that emerges into and equilibrates with overlying coronal magnetic
  field structures, which explains many of the key observed aspects of
  the region's structure and evolution. In particular, the evolving flux
  rope interpretation provides insight into why and how the region moves
  between active and quiescent phases, how the region's sigmoidicity is
  maintained during its evolution, and under what circumstances sigmoidal
  structures are apparent at a range of wavelengths.

Title: Interaction of EIT Waves with Coronal Active Regions
Authors: Ofman, L.; Thompson, B. J.
Bibcode: 2002ApJ...574..440O
Altcode:
  Large-scale coronal waves associated with flares were first observed
  by the Solar and Heliospheric Observatory (SOHO) Extreme ultraviolet
  Imaging Telescope (EIT). We present the first three-dimensional MHD
  modeling of the interaction of the EIT waves with active regions and the
  possibility of destabilization of an active region by these waves. The
  active region is modeled by an initially force-free, bipolar magnetic
  configuration with gravitationally stratified density. We include
  finite thermal pressure and resistive dissipation in our model. The
  EIT wave is launched at the boundary of the region, as a short time
  velocity pulse that travels with the local fast magnetosonic speed
  toward the active region. We find that the EIT wave undergoes strong
  reflection and refraction, in agreement with observations, and induces
  transient currents in the active region. The resulting Lorentz force
  leads to the dynamic distortion of the magnetic field and to the
  generation of secondary waves. The resulting magnetic compression
  of the plasma induces flows, which are particularly strong in the
  current-carrying active region. We investigate the effect of the
  magnetic field configuration and find that the current-carrying active
  region is destabilized by the impact of the wave. Analysis of the
  three-dimensional interaction between EIT waves and active regions can
  serve as a diagnostic of the active region coronal magnetic structure
  and stability.

Title: Halo-coronal mass ejections near the 23rd solar minimum:
    lift-off, inner heliosphere, and in situ (1 AU) signatures
Authors: Berdichevsky, D. B.; Farrugia, C. J.; Thompson, B. J.;
   Lepping, R. P.; Reames, D. V.; Kaiser, M. L.; Steinberg, J. T.;
   Plunkett, S. P.; Michels, D. J.
Bibcode: 2002AnGeo..20..891B
Altcode:
  The extreme ultraviolet (EUV) signatures of a solar lift-off, decametric
  and kilometric radio burst emissions and energetic particle (EP)
  inner heliospheric signatures of an interplanetary shock, and in
  situ identification of its driver through solar wind observations
  are discussed for 12 isolated halo coronal mass ejections (H-CMEs)
  occurring between December 1996 and 1997. For the aforementioned twelve
  and the one event added in the discussion, it is found that ten passed
  several necessary conditions for being a "Sun-Earth connection". It
  is found that low corona EUV and Ha

Title: Relation between a Moreton Wave and an EIT Wave Observed on
    1997 November 4
Authors: Eto, Shigeru; Isobe, Hiroaki; Narukage, Noriyuki; Asai, Ayumi;
   Morimoto, Taro; Thompson, Barbara; Yashiro, Seiji; Wang, Tongjiang;
   Kitai, Reizaburo; Kurokawa, Hiroki; Shibata, Kazunari
Bibcode: 2002PASJ...54..481E
Altcode:
  We consider the relationship between two flare-associated waves,
  a chromospheric Moreton wave and a coronal EIT wave, based on an
  analysis of an X-class flare event in AR 8100 on 1997 November 4. A
  Moreton wave was observed in Hα + 0.8 Å, and Hα - 0.8 Å with the
  Flare-Monitoring Telescope (FMT) at the Hida Observatory. An EIT wave
  was observed in EUV with the Extreme ultraviolet Imaging Telescope
  (EIT) on board SOHO. The propagation speeds of the Moreton wave and
  the EIT wave were approximately 715 km s<SUP>-1</SUP> and 202 km
  s<SUP>-1</SUP>, respectively. The times of visibility for the Moreton
  wave did not overlap those of the EIT wave, but the continuation of the
  former is indicated by a filament oscillation. Data on the speed and
  location clearly show that the Moreton wave differed physically from
  the EIT wave in this case. The Moreton wave preceded the EIT wave,
  which is inconsistent with an identification of the EIT wave with a
  fast-mode MHD shock.

Title: Radio Observations of the Onset of an EIT Wave
Authors: White, S. M.; Thompson, B. J.
Bibcode: 2002AAS...200.2904W
Altcode: 2002BAAS...34R.681W
  We present observations of the early development of an ``EIT wave'' made
  with the Nobeyama Radio Heliograph at 17 GHz. EIT waves are propagating
  disturbances generated in conjunction with solar flares. They have
  most easily been seen to date as emission enhancements in full-disk
  EUV images taken in spectral lines sensitive to 1-2 million degree
  material. We demonstrate that they can also be seen in high dynamic
  range radio observations as well. The high cadence of the radio data
  allows us to show that the EIT wave is not visible until after the onset
  of the impulsive phase of the flare. A radio movie of the event will
  be shown. We discuss the implications of this result for the nature
  of EIT waves and their relationship with other phenomena such as CMEs.

Title: Can EIT Waves be used to Predict Halo CME Properties?
Authors: Biesecker, D. A.; Thompson, B. J.
Bibcode: 2002AAS...200.3708B
Altcode: 2002BAAS...34..695B
  A recent paper by Biesecker et al (2002) showed that EIT waves are
  correlated with Coronal Mass Ejections. Not all CME's produce EIT
  waves, but all EIT waves have associated CME's. If one assumes that
  an EIT wave is a response to the initiation of a CME, then there
  may be circumstances where EIT wave properties would be related to
  CME properties. EIT waves have been modelled as fast magnetosonic
  waves. Thus, their propagation speed across the solar disk depends
  on the local magnetic field and density and one would not expect a
  correlation between EIT wave speeds and CME properties, such as speed
  or intensity. On the other hand, one might expect the intensity of
  the EIT wave to be related to CME properties. If such an association
  can be found, then observations of EIT waves at disk center will give
  information about Earth directed CME's which is currently hard to
  determine. This work examines EIT waves initiated at large distances
  from disk center, so that the associated CME's are well observed. EIT
  wave speeds and intensities are compared to CME speed, intensity and
  other properties, such as kinetic energy.

Title: A Comparison of CME-associated Atmospheric Waves Observed in
    Coronal (Fe XII 19.5 nm) and Chromospheric (He I 1083 nm) Lines
Authors: Gilbert, H. R.; Thompson, B. J.; Holzer, T. E.; Burkepile,
   J. T.
Bibcode: 2002AAS...200.3808G
Altcode: 2002BAAS...34..699G
  In an effort to better understand the relationship between coronal waves
  (EIT waves) and chromospheric waves, we study two events in which waves
  are observed simultaneously in both Fe XII (19.5 nm) and He I (1083 nm):
  lines formed in the corona and chromosphere, respectively. Comparing
  the waves observed in these two lines allows the determination of the
  spatial relationship between coronal and chromospheric waves, and thus
  aids in the understanding of the underlying physics of waves. The main
  goal of this work is to begin an investigation into whether coronal
  and chromospheric waves are both mechanical waves (e.g., MHD waves),
  or whether chromospheric waves are simply "reflections" of mechanical
  waves propagating in the corona.

Title: Gravity Recovery and Precise Orbit Determination With CHAMP
Authors: Lemoine, F. G.; Luthcke, S. B.; Rowlands, D. D.; Cox, C. M.;
   Chinn, D. S.; Pavlis, D. E.; Williams, T.; Thompson, B.; Nerem, R. S.
Bibcode: 2002AGUSM.G22A..10L
Altcode:
  The CHAMP mission, launched in July 2000, is the first in a series
  of missions that will revolutionize our ability to model the Earth's
  geopotential. The CHAMP spacecraft is equiped for precision tracking
  by the Global Positioning System (GPS) and Satellite laser ranging
  (SLR) and along with precision accelerometer to provide measurements
  of the surface forces. In preparation for CHAMP and GRACE, extensive
  modifications have been made to NASA GSFC's GEODYN orbit determination
  software to enable the simultaneous reduction of spacecraft tracking,
  three-axis accelerometry, and precise attitude data. We report in this
  paper on the analysis of over 80 days CHAMP tracking and accelerometry
  and how these data contribute to satellite-only and combination
  geopotential solutions for the Earth. We evaluate the quality of the
  precise orbits and summarize the strategies we have applied in our
  GPS orbit analyses.

Title: Solar Phenomena Associated with ``EIT Waves''
Authors: Biesecker, D. A.; Myers, D. C.; Thompson, B. J.; Hammer,
   D. M.; Vourlidas, A.
Bibcode: 2002ApJ...569.1009B
Altcode:
  In an effort to understand what an ``EIT wave'' is and what its causes
  are, we have looked for correlations between the initiation of EIT
  waves and the occurrence of other solar phenomena. An EIT wave is
  a coronal disturbance, typically appearing as a diffuse brightening
  propagating across the Sun. A catalog of EIT waves, covering the period
  from 1997 March through 1998 June, was used in this study. For each
  EIT wave, the catalog gives the heliographic location and a rating
  for each wave, where the rating is determined by the reliability of
  the observations. Since EIT waves are transient, coronal phenomena, we
  have looked for correlations with other transient, coronal phenomena:
  X-ray flares, coronal mass ejections (CMEs), and metric type II radio
  bursts. An unambiguous correlation between EIT waves and CMEs has been
  found. The correlation of EIT waves with flares is significantly weaker,
  and EIT waves frequently are not accompanied by radio bursts. To
  search for trends in the data, proxies for each of these transient
  phenomena are examined. We also use the accumulated data to show the
  robustness of the catalog and to reveal biases that must be accounted
  for in this study.

Title: What is the source of the magnetic helicity shed by CMEs? The
    long-term helicity budget of AR 7978
Authors: Démoulin, P.; Mandrini, C. H.; van Driel-Gesztelyi, L.;
   Thompson, B. J.; Plunkett, S.; Kovári, Zs.; Aulanier, G.; Young, A.
Bibcode: 2002A&A...382..650D
Altcode:
  An isolated active region (AR) was observed on the Sun during seven
  rotations, starting from its birth in July 1996 to its full dispersion
  in December 1996. We analyse the long-term budget of the AR relative
  magnetic helicity. Firstly, we calculate the helicity injected
  by differential rotation at the photospheric level using MDI/SoHO
  magnetograms. Secondly, we compute the coronal magnetic field and
  its helicity selecting the model which best fits the soft X-ray loops
  observed with SXT/Yohkoh. Finally, we identify all the coronal mass
  ejections (CMEs) that originated from the AR during its lifetime using
  LASCO and EIT/SoHO. Assuming a one to one correspondence between CMEs
  and magnetic clouds, we estimate the magnetic helicity which could be
  shed via CMEs. We find that differential rotation can neither provide
  the required magnetic helicity to the coronal field (at least a factor
  2.5 to 4 larger), nor to the field ejected to the interplanetary
  space (a factor 4 to 20 larger), even in the case of this AR for
  which the total helicity injected by differential rotation is close
  to the maximum possible value. However, the total helicity ejected is
  equivalent to that of a twisted flux tube having the same magnetic flux
  as the studied AR and a number of turns in the interval [0.5,2.0]. We
  suggest that the main source of helicity is the inherent twist of the
  magnetic flux tube forming the active region. This magnetic helicity
  is transferred to the corona either by the continuous emergence of the
  flux tube for several solar rotations (i.e. on a time scale much longer
  than the classical emergence phase), or by torsional Alfvén waves.

Title: New insights on the onsets of coronal mass ejections from soho
Authors: Plunkett, S. P.; Michels, D. J.; Howard, R. A.; Brueckner,
   G. E.; St. Cyr, O. C.; Thompson, B. J.; Simnett, G. M.; Schwenn, R.;
   Lamy, P.
Bibcode: 2002AdSpR..29.1473P
Altcode:
  Coronal mass ejections (CMES) are among the most dramatic forms of
  transient activity occurring in the solar atmosphere. Despite over
  twenty years of research, many basic questions related to the physics
  of CMEs have remained unanswered. Observations with the LASCO and EIT
  experiments on SOHO, combined with recent theoretical modeling, have
  provided new insights on some of these outstanding questions and have
  also raised many new ones that need to be addressed in the future. In
  this paper, we present some of the new results from SOHO pertaining
  to the source regions and onsets of CMEs, and their evolution in the
  corona. We emphasize the important role that studies of CMEs will play
  in the International Solar Cycle Studies program.

Title: Helicity Loading and Dissipation: The Helicity Budget of AR
    7978 from the Cradle to the Grave
Authors: van Driel-Gesztelyi, L.; Démoulin, P.; Mandrini, C. H.;
   Plunkett, S.; Thompson, B.; Kövári, Zs.; Aulanier, G.; Young, A.;
   López Fuentes, M.; Poedts, S.
Bibcode: 2002mwoc.conf..143V
Altcode:
  An isolated active region was observed on the Sun during seven
  rotations, starting in July 1996. I will present a study of its magnetic
  field, concentrating on its helicity budget. The photospheric field
  is extrapolated into the corona in a linear force-free approach,
  using SOHO/MDI magnetograms and Yohkoh/SXT images, allowing us to
  compute, in a crude way, the relative coronal magnetic helicity of
  the active region. Using the observed magnetic field distribution
  (SOHO/MDI magnetograms) we also calculate the helicity injected by
  the differential rotation during seven solar rotations. Finally, using
  SOHO/LASCO and EIT as well as Yohkoh/SXT observations, we identify all
  the 26 CMEs which originated from this active region during its lifetime
  and using average values of the field and radius of magnetic clouds,
  we estimate the helicity which should be shed via CMEs. We compare
  these three values to evaluate the importance of the differential
  rotation relative to twisted flux emergence as a source of magnetic
  helicity. We find that the differential rotation can neither provide
  enough helicity to account for the diagnosed coronal heicity values,
  nor for the helicity carried away by CMEs. We suggest that the main
  source of the magnetic helicity must be the inherent twist of the
  magnetic flux tube forming the active region. This magnetic helicity is
  transferred to the corona either by a slow continuous emergence of the
  flux tube or by torsional Alfven waves, during several solar rotations.

Title: Solar particle events with helium-over-hydrogen enhancement
    in the energy range up to 100 MeV nucl<SUP>−1</SUP>
Authors: Torsti, J.; Kocharov, L.; Laivola, J.; Pohjolainen, S.;
   Plunkett, S. P.; Thompson, B. J.; Kaiser, M. L.; Reiner, M. J.
Bibcode: 2002SoPh..205..123T
Altcode:
  Flux measurements of solar energetic particles (SEPs) in the
  ERNE instrument onboard SOHO indicate that the abundance of
  <SUP>4</SUP>He-nuclei compared to protons in the energy range up to
  100 MeV nucl<SUP>−1</SUP> was exceptionally high during the particle
  events on 27 May 1998 and 28 December 1999. The <SUP>4</SUP>He/p ratio
  stayed between 0.15-0.50 for more than ten hours. There was also
  a prolonged enhancement in helium-3, <SUP>3</SUP>He/<SUP>4</SUP>H
  ≈1%. Observations of EIT and LASCO on board SOHO confirm that the
  originators of both SEP events were western eruptions, flares and
  coronal mass ejections (CMEs). The onset of the SEP release took
  place close to the maximum of flares which were probably triggered
  by the rising CMEs. The observations suggest that the SEP events were
  started with the flare-(pre)accelerated particles, but impact of the
  CME-associated shocks might explain the continuation and modification
  of the helium and proton fluxes well after the flare production. These
  observations support the idea that the helium enhancements in the
  CME-associated events reflect the availability of seed particles that
  originate previously in flares.

Title: Using Solar Wind Composition As A Tracer For Solar Processes:
    Applications For Plastic On Stereo
Authors: Wimmer-Schweingruber, Robert F.; Allegrini, Frédéric;
   Blush, Lisa; Bochsler, Peter; Fischer, Josef; Wurz, Peter; Galvin,
   A. B.; Moebius, E.; Klecker, B.; Thompson, B.; Plastic Team
Bibcode: 2002EGSGA..27.2220W
Altcode:
  Solar wind composition is increasingly being used as a tracer for
  various processes in the solar atmosphere and in interplanetary
  space. We will discuss applications of solar wind composition
  measurements that are relevant for the STEREO mission and that will be
  supplied by the PLASTIC sensor. <P />Solar wind elemental abundances
  are affected by processes acting in the solar interior, chromosphere,
  and in the corona, while charge-state composition is largely determined
  in the corona. Farther out in the inner heliosphere, composition
  measurements can give information about interplanetary processes and
  serves as an excellent tracer for the coronal and chromospheric origin
  of the measured solar wind. <P />Coronal mass ejections often exhibit
  unusual charge-state and elemental composition that is indicative of
  unusual conditions in the solar atmosphere prior and during the launch
  of the ejection. <P />We will discuss observational opportunities
  unique to collaborative studies with vari- ous instruments on STEREO.

Title: Radio Shocks from Reconnection Outflow Jet? - New Observations
Authors: Aurass, H.; Karlicky, M.; Thompson, B. J.; Vršnak, B.
Bibcode: 2002mwoc.conf..401A
Altcode:
  The common analysis of dynamic radio spectrograms with Yohkoh X-ray
  images yields information about possible associations between
  nonthermal electron acceleration and changes in hot and dense
  plasma-magnetic field structures of the corona. Examples are correlated
  X-ray-jet--electron beam injections (type III/U bursts), motions of
  X-ray blobs and correlated shock-driven (type II) radio bursts, and
  sigmoid evolution associated with characteristic type IV burst spectral
  fine structures. Here, we demonstrate the first identification of the
  radio signature of a reconnection outflow termination shock during a
  dynamic flare. Reconnection of magnetic fields is one flare energy
  release mechanism. During dynamic flares there is formed a system
  of standing slow and - sometimes - also fast mode shock waves in the
  space around the diffusion region. This standing fast mode shock is
  revealed by a zero-drift type II burst between 300 and 400 MHz. It
  exists more than 30 min starting 1 hour after the impulsive flare on
  07 April 1997 in AR 8027. It shows herringbone fine structure and 10%
  band splitted lanes. We argue for having detected fundamental mode
  emission. No fundamental-harmonic pattern was observed. Simultaneous
  imaging observations (Hα, Yohkoh SXT, SOHO EIT) show a postflare loop
  arcade with a bright soft X-ray cusp. Preferable conditions for the
  radio detection of the termination shock are a low plasma to magnetic
  pressure ratio eta upstream of the slow shocks, a low diffusion region
  rise velocity, and a low reconnection rate. The occurrence of the
  termination shock is most probable in late stage of flares.

Title: SXT and EIT Observations of A Quiet Region Large-Scale
Eruption: Implications for Eruption Theories
Authors: Sterling, A. C.; Moore, R. L.; Thompson, B. J.
Bibcode: 2002mwoc.conf..165S
Altcode:
  We present Yohkoh/SXT and SOHO/EIT observations of a set of slow, large
  scale, quiet-region solar eruptions. In SXT data, these events seem to
  appear ``out of nothing,'' indicating that they are associated initially
  with weak magnetic fields and corresponding low heating rates. These
  events evolve relatively slowly, affording us an opportunity to
  examine in detail their development. We look for signatures of the
  start of the eruptions through intensity variations, physical motions,
  and dimming signatures in the SXT and EIT data. In particular, we look
  to see whether the earliest signatures are brightenings occurring in
  the ``core'' region (i.e., the location where the magnetic shear is
  strongest and the post-flare loops develop); such early brightenings in
  the core could be indicative of a ``tether-cutting'' process, whereby
  the eruption is instigated by magnetic reconnection among highly-sheared
  core fields. In our best-observed case, we find motions of the core
  fields beginning well before brightenings in the core. This is new
  evidence that tether-cutting is not the primary mechanism operating
  in solar eruptions. Rather, our observations are more consistent with
  the eruption process known as the ``breakout model'' (Antiochos et
  al. 1999), which holds that the eruption results from initial slow
  magnetic reconnections occurring high above (far from) the core region.

Title: Progress Towards the Solar Dynamics Observatory
Authors: Thompson, B.; Schwer, K.
Bibcode: 2002cosp...34E1987T
Altcode: 2002cosp.meetE1987T
  The Solar Dynamics Observatory, or SDO, is scheduled to be the first
  mission to launch in 2007 under the new Living With a Star (LWS)
  program. It builds on the success of SOHO and other recent solar
  missions, but will observe the Sun at greater resolution and faster
  time cadence with a set of remote sensing instruments generating data
  in excess of 100 Mbps. The Science Definition Team produced a report
  consisting of a series of science objectives and a baseline instrument
  complement. Instrument proposals were due in April 2002, with selection
  to occur in the late summer of 2002. The spacecraft is being built
  at NASA Goddard Spacecraft Center by a team of engineers which are
  currently undergoing the formulation process. The presentation will
  discuss the current status of the science investigation selection and
  the spacecraft formulation.

Title: Upstream Shocks and Interplanetary Magnetic Cloud Speed and
Expansion: Sun, Wind, and Earth Observations
Authors: Lepping, R. P.; Berdichevsky, D.; Szabo, A.; Lazarus, A. J.;
   Thompson, B. J.
Bibcode: 2002swsm.conf...87L
Altcode:
  No abstract at ADS

Title: Observations of Moreton Waves and EIT Waves
Authors: Shibata, K.; Eto, S.; Narukage, N.; Isobe, H.; Morimoto,
   T.; Kozu, H.; Asai, A.; Ishii, T.; Akiyama, S.; Ueno, S.; Kitai, R.;
   Kurokawa, H.; Yashiro, S.; Thompson, B. J.; Wang, T.; Hudson, H. S.
Bibcode: 2002mwoc.conf..279S
Altcode:
  The Moreton wave is a flare-associated wave observed in H alpha, and
  is now established to be a fast mode MHD shock emitted from the flare,
  but the physical mechanism to create the wave is still puzzling. On
  the other hand, the EIT wave is a newly discovered flare-associated
  wave observed in EUV with the Extreme ultraviolet Imaging Telescope
  (EIT) aboard SOHO, and in this case, not only its origin but also
  its physical property are both puzzling. We study the relationship
  of these two flare-associated waves, Moreton waves and EIT waves, by
  analyzing 4 events observed on Nov. 3 and 4, 1997, Aug. 8, 1998, and
  Mar. 3, 2000 (Narukage et al. 2001). The Moreton waves were observed
  in Ha, Ha+0.8A and Ha-0.8A with the Flare Monitoring Telescope (FMT)
  at the Hida Observatory of Kyoto University, while the EIT waves were
  observed with SOHO/EIT. In the typical case associated with an X-class
  flare in AR 8100 on 4 November 1997 (Eto et al. 2001) the propagation
  speeds of the Moreton wave and the EIT wave were approximately 780
  km/s and 200 km/s respectively. The data on speed and location show
  clearly that the Moreton wave differs physically from the EIT wave in
  this case. The detailed analyses of the other events (Nov. 3, 1997,
  Aug. 8, 1998, and Mar. 3, 2000) will also be presented, with Yohkoh/SXT
  data in the lucky case.

Title: Phenomena Associated with EIT Waves
Authors: Thompson, B.; Biesecker, D.; Gopalswamy, N.
Bibcode: 2002cosp...34E2672T
Altcode: 2002cosp.meetE2672T
  We discuss phenomena associated with "EIT Wave" transients. "EIT
  Waves" are propagating disturbances first observed in SOHO/EIT EUV
  images. However, a number of studies have been conducted to determine
  their relationship to other observations, using data from a variety
  of instruments. These phenomena include coronal mass ejections,
  flares, EUV/SXR dimmings,chromospheric waves, Moreton waves, solar
  energetic particle events, energetic electron events, and radio
  signatures. Although the occurrence of many phenomena correlate with the
  appearance of EIT waves, it is difficult to infer which associations are
  causal. The presentation will include a discussion of the correlation
  statistics of these phenomena.

Title: The International Heliophysical Year Concept
Authors: Davila, J.; Harrison, R.; Poland, A.; St-Cyr, O.; Thompson, B.
Bibcode: 2002cosp...34E.529D
Altcode: 2002cosp.meetE.529D
  In 1957 a program of international research, inspired by the
  International Polar Years of 1882-83 and 1932-33, was organized as
  the International Geophysical Year (IGY) to study global phenomena of
  the Earth and geospace. The IGY involved about 60,000 scientists from
  66 nations, working at thousands of stations, from pole to pole to
  obtain simultaneous, global observations on Earth and in space. There
  had never been anything like it before. The fiftieth anniversary of
  the International Geophysical Year will occur in 2007. We propose to
  organize an international program of scientific collaboration for this
  time period called the International Heliophysical Year (IHY). Like
  its predecessors, the IHY will focus on fundamental global questions
  of Earth science.

Title: Relationships between CME's and prominences
Authors: Schmieder, B.; van Driel-Gesztelyi, L.; Aulanier, G.;
   Démoulin, P.; Thompson, B.; De Forest, C.; Wiik, J. E.; Saint Cyr,
   C.; Vial, J. C.
Bibcode: 2002AdSpR..29.1451S
Altcode:
  We have studied the erupting prominences which were associated with
  coronal mass ejections during a series of campaigns involving both
  spacecraft and ground-based observatories. The evolution of the
  physical conditions within the prominences was established from Hα
  and magnetic field observations. Particular attention ahs been paid
  to the presence of mixed amgnetic polarity in the filament channel,
  the evolution of the shear of the large-scale magnetic field, and
  the existence of multiple magnetic inversion lines. We conclude that
  reconnection of large-scale coronal magnetic fields is responsible
  for both the CME and filament eruption.

Title: Erupting Solar Magnetic Flux Ropes: Theory and Observation
Authors: Krall, J.; Chen, J.; Duffin, R. T.; Howard, R. A.; Thompson,
   B. J.
Bibcode: 2001ApJ...562.1045K
Altcode:
  Measurements of coronograph (LASCO) and extreme-ultraviolet (EIT)
  images are presented for 11 coronal mass ejection (CME) events. Detailed
  measurements of these events, selected because they have flux-rope-like
  morphological features, show excellent agreement with results from a
  theoretical model of erupting flux-rope dynamics. Here, data are used
  to provide inputs and constraints on the model wherever possible. We
  conclude that flux rope CMEs constitute a distinct class of CMEs,
  characterized by specific morphological and dynamical properties.

Title: Proton Storms Associated with Far-Sided Coronal Mass Ejections
Authors: Lawrence, G. R.; Thompson, B. J.
Bibcode: 2001AGUFMSH41B0753L
Altcode:
  A fast, bright, full-halo CME, characterised by emission around all 360
  degrees of the occulting disk, was observed late on August 15th 2001
  by the LASCO white-light coronagraphs onboard SOHO, and was followed
  within an hour by an intense proton storm at 1 AU. Such a sequence of
  events is normally indicative of an earth-directed event with a source
  region on the near-side solar disk close to the notional footpoints
  of IMF field lines connecting to 1 AU at the event time. However,
  EUV images of the low corona from EIT, also onboard SOHO, show no
  significant activity whatsoever. Also, during the event the X-ray flux,
  as monitored by GOES, was low and decreasing. Thus it seems likely
  that the source region was located on the far-side. We speculate
  that it was a known active region that had traversed the west limb
  a week previously, thus placing it close to central meridian at the
  time of event onset. The subsequent activity from this region after
  it had traversed the east limb a week later support this picture. We
  discuss the nature and timeline of the event in detail, and consider
  implications for the generation of particles at 1 AU, particularly in
  terms of the fluxes and spectra observed.

Title: A Comparison of CME-associated atmospheric waves observed in
    coronal (19.5 nm) and chromospheric (He I 1083 nm and H-alpha 656
    nm) lines
Authors: Gilbert, H. R.; Thompson, B. J.; Holzer, T. E.; Burkepile,
   J. T.
Bibcode: 2001AGUFMSH12B0746G
Altcode:
  Coronal Mass Ejections (CMEs) are frequently associated with wave
  phenomena observed in the corona, and sometimes with wave phenomena
  observed in the chromosphere. We have studied CME-associated waves
  observed in both coronal (19.5 nm) and chromospheric (He I 1083 nm and
  H-alpha 656 nm) lines. Comparison of the coronal and chromospheric
  signatures allows us to understand better the relationship between
  the two wave phenomena.

Title: EIT and SXT Observations of a Quiet-Region Filament Ejection:
    First Eruption, Then Reconnection
Authors: Sterling, Alphonse C.; Moore, Ronald L.; Thompson, Barbara J.
Bibcode: 2001ApJ...561L.219S
Altcode:
  We observe a slow-onset quiet-region filament eruption with the EUV
  Imaging Telescope (EIT) on the Solar Heliospheric Observatory (SOHO)
  and the soft X-ray telescope (SXT) on Yohkoh. This event occurred on
  1999 April 18 and was likely the origin of a coronal mass ejection
  detected by SOHO at 08:30 UT on that day. In the EIT observation,
  one-half of the filament shows two stages of evolution: stage 1 is a
  slow, roughly constant upward movement at ~1 km s<SUP>-1</SUP> lasting
  ~6.5 hr, and stage 2 is a rapid upward eruption at ~16 km s<SUP>-1</SUP>
  occurring just before the filament disappears into interplanetary
  space. The other half of the filament shows little motion along the
  line of sight during the time of stage 1 but erupts along with the rest
  of the filament during stage 2. There is no obvious emission from the
  filament in the SXT observation until stage 2; at that time, an arcade
  of EUV and soft X-ray loops forms first at the central location of the
  filament and then expands outward along the length of the filament
  channel. A plot of EUV intensity versus time of the central portion
  of the filament (where the postflare loops initially form) shows a
  flat profile during stage 1 and a rapid upturn after the start of
  stage 2. This light curve is delayed from what would be expected if
  ``tether-cutting'' reconnection in the core of the erupting region
  were responsible for the initiation of the eruption. Rather, these
  observations suggest that a loss of stability of the magnetic field
  holding the filament initiates the eruption, with reconnection in the
  core region occurring only as a by-product.

Title: Three-dimensional numerical simulation of MHD waves observed
    by the Extreme Ultraviolet Imaging Telescope
Authors: Wu, S. T.; Zheng, Huinan; Wang, S.; Thompson, B. J.; Plunkett,
   S. P.; Zhao, X. P.; Dryer, M.
Bibcode: 2001JGR...10625089W
Altcode:
  We investigate the global large amplitude waves propagating across
  the solar disk as observed by the SOHO/Extreme Ultraviolet Imaging
  Telescope (EIT). These waves appear to be similar to those observed
  in H<SUB>α</SUB> in the chromosphere and which are known as
  ``Moreton waves,'' associated with large solar flares [Moreton,
  1960, 1964]. Uchida [1968] interpreted these Moreton waves as the
  propagation of a hydromagnetics disturbance in the corona with
  its wavefront intersecting the chromosphere to produce the Moreton
  wave as observed in movie sequences of H<SUB>α</SUB> images. To
  search for an understanding of the physical characteristics of
  these newly observed EIT waves, we constructed a three-dimensional,
  time-dependent, numerical magnetohydrodynamic (MHD) model. Measured
  global magnetic fields, obtained from the Wilcox Solar Observatory
  (WSO) at Stanford University, are used as the initial magnetic field
  to investigate hydromagnetics wave propagation in a three-dimensional
  spherical geometry. Using magnetohydrodynamic wave theory together
  with simulation, we are able to identify these observed EIT waves as
  fast mode MHD waves dominated by the acoustic mode, called magnetosonic
  waves. The results to be presented include the following: (1) comparison
  of observed and simulated morphology projected on the disk and the
  distance-time curves on the solar disk; (2) three-dimensional evolution
  of the disturbed magnetic field lines at various viewing angles;
  (3) evolution of the plasma density profile at a specific location
  as a function of latitude; and (4) computed Friedrich's diagrams to
  identify the MHD wave characteristics.

Title: Eruption and acceleration of flare-associated coronal mass
    ejection loops in the low corona
Authors: Neupert, W. M.; Thompson, B. J.; Gurman, J. B.; Plunkett,
   S. P.
Bibcode: 2001JGR...10625215N
Altcode:
  Observations made by the EUV imaging telescope (EIT) and the Large-Angle
  Spectrometric Coronagraph (LASCO) on board the Solar Heliospheric
  Observatory (SOHO) have been used to characterize the eruption and
  acceleration of flare-associated coronal mass ejections (CMEs) in the
  low corona. For three well-observed limb events we tracked CME loops
  back to preexisting but faint EUV-emitting loops at heights of 100-250
  Mm that initially brightened slowly and possibly increased slowly in
  height, apparently in response to filament activity and eruption in the
  associated active regions. Subsequent CME acceleration coincided with
  a rapid rise of the soft X-ray flux, occurred between 100 and 350 Mm
  above the surface, and may have been as high as 0.5 km s<SUP>-1</SUP>
  s<SUP>-1</SUP>, consistent with an impulsive acceleration of the CME
  to the speeds observed in subsequent white-light observations. The
  existence of a delay of up to 30 min observed between initial filament
  eruption in H alpha and subsequent high acceleration of the CME in
  one event implies that there may have been two separate phases of
  magnetic reconnection, with the initial filament activity acting as
  a trigger for subsequent CME and energetic particle acceleration in
  the impulsive stage of the flare. The presence or absence of this
  impulsive phase may provide a basis for the two types of CMEs that
  have been discussed in the literature.

Title: Reconnection remnants in the magnetic cloud of October 18-19,
1995: A shock, monochromatic wave, heat flux dropout, and energetic
    ion beam
Authors: Collier, Michael R.; Szabo, A.; Farrell, W. M.; Slavin,
   J. A.; Lepping, R. P.; Fitzenreiter, R.; Thompson, B.; Hamilton,
   D. C.; Gloeckler, G.; Ho, G. C.; Bochsler, P.; Larson, D.; Ofman, L.
Bibcode: 2001JGR...10615985C
Altcode:
  Evidence is presented that the Wind spacecraft observed particle and
  field signatures on October 18-19, 1995, due to reconnection near
  the foot points of a magnetic cloud (i.e., between 1 and 5 solar
  radii). These signatures include (1) an internal shock traveling
  approximately along the axis of the magnetic cloud, (2) a simple
  compression of the magnetic field consistent with the foot point
  magnetic fields being thrust outward at speeds much greater than the
  solar wind speed, (3) an electron heat flux dropout occurring within
  minutes of the shock, indicating a topological change resulting from
  disconnection from the solar surface, (4) a very cold 5 keV proton
  beam, and (5) an associated monochromatic wave. We expect that given
  observations of enough magnetic clouds, Wind and other spacecraft
  will see signatures similar to the ones reported here indicating
  reconnection. However, these observations require the spacecraft to
  be fortuitously positioned to observe the passing shock and other
  signatures and will therefore be associated with only a small fraction
  of magnetic clouds. Consistent with this, a few magnetic clouds observed
  by Wind have been found to possess internal shock waves.

Title: On-the-Disk Development of the Halo Coronal Mass Ejection on
    1998 May 2
Authors: Pohjolainen, S.; Maia, D.; Pick, M.; Vilmer, N.; Khan, J. I.;
   Otruba, W.; Warmuth, A.; Benz, A.; Alissandrakis, C.; Thompson, B. J.
Bibcode: 2001ApJ...556..421P
Altcode:
  A halo coronal mass ejection (CME) was observed at 15:03 UT on 1998 May
  2 by the Solar and Heliospheric Observatory Large-Angle Spectrometric
  Coronagraph. The observation of the CME was preceded by a major soft
  X-ray flare in NOAA Active Region 8210, characterized by a delta spot
  magnetic configuration and some activity in region 8214. A large
  transequatorial interconnecting loop (TIL) seen in the soft X-rays
  connected AR 8210 to a faint magnetic field region in the periphery
  of region 8214. Smaller loop systems were also connecting AR 8210 to
  other fainter bipolar magnetic structures, the interconnecting loop
  (IL) east of AR 8210 being one of the most visible. We present here
  a multiwavelength analysis of the large- and small-scale coronal
  structures associated with the development of the flare and of the
  CME, with emphasis placed on radio-imaging data. In the early phases
  of the flare, the radio emission sources traced the propagation paths
  of electrons along the TIL and the IL, which are accelerated in the
  vicinity of AR 8210. Furthermore, jetlike flows were observed in soft
  X-rays and in Hα in these directions. Significantly, the TIL and
  IL loop systems disappeared at least partially after the CME. An EUV
  Imaging Telescope (EIT) dimming region of similar size and shape to the
  soft X-ray TIL, but noticeably offset from it, was also observed. During
  the ``flash'' phase of the flare, new radio sources appeared, presenting
  signatures of destabilization and reconnection at discrete locations of
  the connecting loops. We interpret these as possible signatures of the
  CME liftoff on the disk. An Hα Moreton wave (blast wave) and an ``EIT
  wave'' were also observed, originating from the flaring AR 8210. The
  signatures in radio, after the wave propagated high into the corona,
  include type II-like emissions in the spectra. The radio images link
  these emissions to fast-moving sources, presumably formed at locations
  where the blast wave encounters magnetic structures. The opening of
  the CME magnetic field is revealed by the radio observations, which
  show large and expanding moving sources overlying the later-seen EIT
  dimming region.

Title: SOHO Observations of a Coronal Mass Ejection
Authors: Akmal, Arya; Raymond, John C.; Vourlidas, Angelos; Thompson,
   Barbara; Ciaravella, A.; Ko, Y. -K.; Uzzo, M.; Wu, R.
Bibcode: 2001ApJ...553..922A
Altcode:
  We describe a coronal mass ejection (CME) observed on 1999 April 23 by
  the Ultraviolet Coronagraph Spectrometer (UVCS), the Extreme-Ultraviolet
  Imaging Telescope (EIT), and the Large-Angle and Spectrometric
  Coronagraphs (LASCO) aboard the Solar and Heliospheric Observatory
  (SOHO). In addition to the O VI and C III lines typical of UVCS spectra
  of CMEs, this 480 km s<SUP>-1</SUP> CME exhibits the forbidden and
  intercombination lines of O V at λλ1213.8 and 1218.4. The relative
  intensities of the O V lines represent an accurate electron density
  diagnostic not generally available at 3.5 R<SUB>solar</SUB>. By
  combining the density with the column density derived from LASCO,
  we obtain the emission measure of the ejected gas. With the help
  of models of the temperature and time-dependent ionization state of
  the expanding gas, we determine a range of heating rates required to
  account for the UV emission lines. The total thermal energy deposited
  as the gas travels to 3.5 R<SUB>solar</SUB> is comparable to the
  kinetic and gravitational potential energies. We note a core of colder
  material radiating in C III, surrounded by hotter material radiating
  in the O V and O VI lines. This concentration of the coolest material
  into small regions may be a common feature of CMEs. This event thus
  represents a unique opportunity to describe the morphology of a CME,
  and to characterize its plasma parameters.

Title: Solar Phenomena Associated With EIT Waves
Authors: Myers, D. C.; Biesecker, D. A.; Thompson, B. J.; Vourlidas, A.
Bibcode: 2001AGUSM..SH51B03M
Altcode:
  Observations with the Extreme Ultraviolet Imaging Telescope (EIT)
  on SOHO revealed the existence of transient waves which appear to
  propagate across the disk from a localized starting point. These EIT
  waves may be the coronal counterpart of previously discovered Moreton
  waves. Moreton waves have long been thought to be associated with
  solar flares, though this may have been because flares are more easily
  observed than other phenomena, such as Coronal Mass Ejections. EIT
  waves are observed much more often than Moreton waves, though this
  may also be due to detection efficiency. In this study, we hope to
  gain a better understanding of EIT waves, and in particular their
  initiation, through their relationship to other solar events. This
  study uses a complete catalog of EIT waves observed from March, 1997
  to June, 1998; a period in which 175 waves were found. For each wave,
  the following ancillary data sets were examined for co-temporal and
  co-spatial events: GOES X-ray Monitor, LASCO Coronagraph, and Type II
  radio burst data. EIT waves are classified according to a system which
  measures the reliability of the existence of the event. We investigate
  the rate at which each class of EIT wave is associated with flares,
  CMEs and Type II events. Data are further divided into limb and disk
  events in order to correct for detection efficiency and biases. An
  investigation of EUV dimmings is also included as they offer clues to
  the relationship between EIT waves, flares and CME's.

Title: Solar source regions of coronal mass ejections and their
    geomagnetic effects
Authors: Plunkett, S. P.; Thompson, B. J.; St. Cyr, O. C.; Howard,
   R. A.
Bibcode: 2001JASTP..63..389P
Altcode: 2001JATP...63..389P
  It is generally accepted that the fast interplanetary manifestations of
  coronal mass ejections (ICMEs) are the major solar drivers of many space
  weather phenomena, including large, non-recurrent geomagnetic storms
  and solar energetic particle events. High-quality synoptic observations
  of the solar corona, as carried out by the EIT and LASCO experiments on
  SOHO, provide near real-time imaging of CMEs from the base of the corona
  out to a projected distance of 30R<SUB>solar</SUB> (R<SUB>solar</SUB> is
  the solar radius). The average characteristics of CMEs observed by LASCO
  are similar to those from earlier coronagraphs. Most CMEs travel with
  approximately constant speed through the LASCO field of view. However,
  a significant number accelerate as they move outward, and some fast
  events have been observed to decelerate. LASCO has observed a great deal
  of internal structure in many CMEs. Concave-outward structures that
  are interpreted as magnetic flux ropes are observed in approximately
  one third of all events. Complex structures are often observed in the
  trailing portions of CMEs. Halo CMEs, many of which are very faint,
  can be routinely observed with LASCO. Extreme-ultraviolet (EUV)
  images of the low corona and solar disk, as recorded by EIT, reveal
  a complex web of CME signatures. These include large-scale waves in
  the inner corona associated with CMEs, extended regions of depleted
  EUV intensity, and bright arcades that form following the occurrence
  of a CME. The combination of LASCO and EIT imagery allows the source
  regions of halo CMEs to be identified, and can be used to help predict
  the occurrence of geomagnetic disturbances several days in advance. The
  most important parameters in determining the geoeffectiveness of an
  ICME are the magnetic field strength and direction, and the speed of
  the disturbance. The most intense geomagnetic storms are associated
  with strong and persistent southward fields, either within the ICME
  itself or in the compressed sheath of solar wind plasma ahead of it.

Title: An Observational Test for Solar Atmospheric Heating
Authors: van Driel-Gesztelyi, L.; Démoulin, P.; Ireland, J.; Thompson,
   B.; Fludra, A.; Oláh, K.; Kövári, Zs.; Harra, L. K.; Mandrini,
   C. H.; Bocchialini, K.; Orlando, S.
Bibcode: 2001IAUS..203..514V
Altcode:
  We study the evolution of the emissivity and heating correlated with
  magnetic observables of an active region from its birth throughout
  its decay during seven solar rotations (July-Dec. 1996). Taking one
  "snapshot" per g:wq: Command not found. time of flares, we analyse
  multi-wavelength and multi-instrument data obtained from SOHO (MDI,
  EIT, CDS and SUMER), Yohkoh (SXT), GOES, SOLSTICE and 10.7 cm radio
  data from DRAO, Canada. We utilise our results to test the validity
  of coronal heating models. We find that models which are based on
  the dissipation of stressed, current-carrying magnetic fields are in
  better agreement with the observations than the models which attribute
  coronal heating to the dissipation of MHD waves.

Title: Magnetic Evolution of a Long-Lived Active Region: The Sources
    of Magnetic Helicity
Authors: Mandrini, C. H.; Démoulin, P.; van Driel-Gesztelyi, L.;
   Aulanier, G.; Thompson, B.; Plunkett, S.; Kövári, Zs.
Bibcode: 2001ASPC..248..139M
Altcode: 2001mfah.conf..139M
  No abstract at ADS

Title: Early life of coronal mass ejections
Authors: Gopalswamy, N.; Thompson, B. J.
Bibcode: 2000JASTP..62.1457G
Altcode: 2000JATP...62.1457G
  Coronal mass ejections (CMEs) are large-scale magnetized plasma
  structures ejected from closed magnetic field regions of the Sun. White
  light coronagraphic observations from ground and space have provided
  extensive information on CMEs in the outer corona. However, our
  understanding of the solar origin and early life of CMEs is still in
  an elementary stage because of lack of adequate observations. Recent
  space missions such as Yohkoh and Solar and Heliospheric Observatory
  (SOHO) and ground-based radioheliographs at Nobeyama and Nancay have
  accumulated a wealth of information on the manifestations of CMEs
  near the solar surface. We review some of these observations in
  an attempt to relate them to what we already know about CMEs. Our
  discussion relies heavily on non-coronagraphic data combined with
  coronagraphic data. Specifically, we discuss the following aspects of
  CMEs: (i) coronal dimming and global disk signatures, (ii) non-radial
  propagation during the early phase, (iii) Photospheric magnetic field
  changes during CMEs, and (iv) acceleration of fast CMEs. The relative
  positions and evolution of coronal dimming, arcade formation, prominence
  eruption will be discussed using specific events. The magnitude and
  spatial extent of CME acceleration may be an important parameter that
  distinguishes fast and slow CMEs.

Title: Sympathetic flaring with BATSE, GOES, and EIT data
Authors: Biesecker, D. A.; Thompson, B. J.
Bibcode: 2000JASTP..62.1449B
Altcode: 2000JATP...62.1449B
  Sympathetic flaring is defined as the initiation of a solar flare
  as a result of a transient phenomenon occurring elsewhere on the
  Sun. Discovery of sympathetic flaring or lack thereof, may lead to a
  greater understanding of the physics of flare initiation. Knowledge of
  a mechanism for initiating solar flares would also aid in predicting
  at least some solar flares. Two studies of sympathetic flaring
  are presented in this paper. The first part of the paper presents
  a test for sympathetic flaring in flares observed with the Burst
  and Transient Source Experiment. A Monte Carlo simulation is used
  to compare the distribution of solar X-ray flares in time to that
  expected from a time-varying, Poisson distribution. No evidence for
  sympathetic flaring is found, though it cannot be ruled out. The X-ray
  flare data also do not allow discovery of sympathetic flares occurring
  within 2 min of the initial flare. Because the observations do allow
  for at least some flares to occur sympathetically, the second part of
  the paper examines one possible mechanism for initiating flares. The
  mechanism examined is large-scale coronal transients observed by the
  SOHO//Extreme Ultraviolet Imaging Telescope: EIT waves. A comparison of
  the rate of flaring in the interval prior to an EIT wave to the rate
  of flaring while the wave traverses the solar disk shows no increase
  in the number of flares due to the EIT wave.

Title: Measurements of the solar wind over a wide range of
    heliocentric distances - a comparison of results from the first
    three Whole Sun Months
Authors: Breen, A. R.; Thompson, B. J.; Kojima, M.; Biesecker, D. A.;
   Canals, A.; Fallows, R. A.; Linker, J. A.; Lazarus, A. J.; Lecinski,
   A.; Mikic, Z.; Moran, P. J.; Williams, P. J. S.
Bibcode: 2000JASTP..62.1527B
Altcode: 2000JATP...62.1527B
  Co-ordinated observations of the Sun and inner heliosphere using a
  large number of space- and ground-based instruments were carried out
  in August-September 1996, August 1998 and August-September 1999 as the
  first, second and third Whole Sun Months. These observations provided
  unprecedented cover of the Sun and inner heliosphere at solar minimum
  (1996) and during the rising phase of the new solar cycle (1998,
  1999). In this paper we review the observations made during the three
  Whole Sun Months and consider the changes in the large-scale structure
  of the heliosphere seen over the four years.

Title: Moreton Waves
Authors: Thompson, B.
Bibcode: 2000eaa..bookE2575T
Altcode:
  `Moreton waves', named for the observer who popularized them, are a
  solar phenomenon also known in scientific literature as `Moreton-Ramsey
  waves', `flare waves', `flare-associated waves', `MHD blast waves',
  `chromospheric shock fronts' and various other combinations of terms
  which connote violently propagating impulsive disturbances. It is
  unclear whether all of the observations to which these t...

Title: Initiation of CMEs: the role of magnetic twist
Authors: van Driel-Gesztelyi, L.; Manoharan, P. K.; Démoulin, P.;
   Aulanier, G.; Mandrini, C. H.; Lopez-Fuentes, M.; Schmieder, B.;
   Orlando, S.; Thompson, B.; Plunkett, S.
Bibcode: 2000JASTP..62.1437V
Altcode: 2000JATP...62.1437V
  Recent multiwavelength observations, modelling results and
  theoretical developments indicate the importance of twisted magnetic
  configurations in solar active regions (ARs) in the initiation of
  coronal mass ejections (CMEs). Through multiwavelength analysis of a
  few representative events we make an attempt to provide constraints
  for CME models. The two events presented here in detail start with
  the expansion of sigmoids (S- or inverse S-shaped loops) observed in
  soft X-rays. Both events (on 25 October /1994 and 14 October /1995)
  occurred before the launch of the SOHO spacecraft, but indirect
  evidences (i.e. signatures of an outward propagation traced up to /~20
  solar radii and an associated magnetic cloud) suggest that both of them
  were related to CMEs. We show evidence that sigmoids are the coronal
  manifestations of twisted magnetic flux tubes, which start expanding
  presumably due to a loss of equilibrium. It is noteworthy that the
  analysed CMEs occurred in a complex (not simply bipolar) magnetic
  environment and in all cases we found evidences of the interaction
  (magnetic reconnection) with the surrounding fields. We propose a
  scenario for sigmoid expansion related CME events and suggest that
  twisted magnetic configurations are good candidates for being source
  regions of CMEs.

Title: Abundance variations and fractionation effects in a gradual
    SEP event
Authors: Galvin, A. B.; Möbius, E.; Popecki, M. A.; Kistler, L. M.;
   Morris, D.; Heirtzler, D.; Hovestadt, D.; Klecker, B.; Bogdanov,
   A. T.; Thompson, B.
Bibcode: 2000AIPC..528..127G
Altcode: 2000atep.conf..127G
  Using data from the ACE SEPICA experiment, we examine elemental
  abundance variations for C, O, Ne, Mg, Si and Fe for the 1998 April
  21-23 ``pure'' gradual SEP event in the energy ranges 0.6-0.8 and
  0.8-1.0 MeV/nucleon. The high FIP element Ne has SEP abundances
  (Ne/O) consistent with nominal photospheric and coronal values. Low
  FIP elements Mg, Fe, and Si show enhancements (relative to O) over
  both photospheric and coronal abundances. Power law fits to the SEP
  abundances (normalized to coronal values) as a function of measured
  &lt;Q&gt;/A are performed and evaluated. It is found that for this event
  the single-parameter power law assumption does not yield a consistently
  good fit. The derived power law index γ varies with both time and
  energy. .

Title: Correction to “Coronal dimmings and energetic CMEs in
    April-May 1998,”
Authors: Thompson, B. J.; Cliver, E. W.; Nitta, N.; Delannée, C.;
   Delaboudinière, J. -P.
Bibcode: 2000GeoRL..27.1865T
Altcode:
  No abstract at ADS

Title: SOHO and radio observations of a CME shock wave
Authors: Raymond, John C.; Thompson, Barbara J.; St. Cyr, O. C.;
   Gopalswamy, Nat; Kahler, S.; Kaiser, M.; Lara, A.; Ciaravella, A.;
   Romoli, M.; O'Neal, R.
Bibcode: 2000GeoRL..27.1439R
Altcode:
  A 1200 km s<SUP>-1</SUP> Coronal Mass Ejection was observed with the
  SOHO instruments EIT, LASCO and UVCS on June 11, 1998. Simultaneously,
  Type II radio bursts were observed with the WAVES experiment aboard
  the Wind spacecraft at 4 MHz and by ground-based instruments at metric
  wavelengths. The density in the shock wave implied by the higher
  frequency is close to that inferred from the SOHO/UVCS experiment. The
  drift rates of the Type II radio bursts suggest shock speeds lower than
  the speed derived from SOHO observations. The SOHO/UVCS spectrum shows
  enhanced emission in lines of O<SUP>5+</SUP> and Si<SUP>11+</SUP>,
  consistent with modest compression in an MHD shock.

Title: Radio-rich solar eruptive events
Authors: Gopalswamy, N.; Kaiser, M. L.; Thompson, B. J.; Burlaga,
   L. F.; Szabo, A.; Lara, A.; Vourlidas, A.; Yashiro, S.; Bougeret,
   J. -L.
Bibcode: 2000GeoRL..27.1427G
Altcode:
  We report on the analysis of a large number of solar eruptive events
  that produced radio emission in the dekameter-hectometric (DH) radio
  window (1-14 MHz), newly opened by the Wind/WAVES experiment. The
  distinguishing characteristics of coronal mass ejections (CMEs)
  associated with the DH type II radio bursts are larger-than-average
  width and speed. Flares of all sizes (X-ray importance B to X) occurring
  at all longitudes were associated with the DH type II bursts and
  CMEs. We found a global enhancement in EUV over an area much larger than
  the flaring active region in the beginning many events. A comparison
  between the ‘Shock Associated’ events and microwave bursts shows
  that at least half of the events do not have temporal relation. A
  majority of the DH type II bursts were associated with IP shocks
  and kilometric type II bursts. In particular, we found a very close
  relationship between the kilometric type II bursts and the IP shocks.

Title: Three-Dimensional Structure of Flux-Rope CME's: Theory and
    Observation*
Authors: Krall, J.; Chen, J.; Howard, R. A.; Thompson, B. J.
Bibcode: 2000SPD....31.0801K
Altcode: 2000BAAS...32R.839K
  A recent program of direct comparison of model CME results and CME
  observations [1-4] has produced a coherent view of the geometry and
  the dynamics of a specific class of CME's, which we refer to as
  ``flux-rope CME's.'' We further support this view by presenting
  LASCO/EIT measurements and model results for 11 flux-rope CME
  events. Each CME is compared to the theoretical results of a flux rope
  model [4,5] under the assumption that the driving mechanism is flux
  injection. In all cases the source region for the CME is determined
  so as to properly account for projection effects in the model/data
  comparisons. This talk will summarize the basic physical understanding
  resulting from the recent work. In particular, we discuss observable
  signatures produced by the model and compare them with the EIT and
  LASCO data. We also discuss photospheric signatures of these events in
  terms of motion (a few meters per second) and changes in the tangential
  magnetic field (about ten percent for tens of minutes). These are very
  small but may be accessible by future observations. Taken as a whole,
  the observational and model results provide a consistent view of the
  three-dimensional structure of this class of CME's. [1] Chen et al.,
  ApJ Lett., 490, L191, 1997. [2] Wood et al, ApJ, 512, 484, 1999. [3]
  Chen et al., to appear in ApJ, 2000. [4] Krall et al., to appear in ApJ,
  2000. [5] Chen, J., JGR, 101, 27499, 1996. *Work supported by ONR.

Title: Coronal dimmings and energetic CMEs in April-May 1998
Authors: Thompson, B. J.; Cliver, E. W.; Nitta, N.; Delannée, C.;
   Delaboudinière, J. -P.
Bibcode: 2000GeoRL..27.1431T
Altcode:
  We have analyzed the coronal dimmings for seven fast (&gt; 600 km/s)
  coronal mass ejections (CMEs) occurring between 23 April and 9 May which
  were associated with flares from NOAA active region (AR) 8210. Each
  of these CMEs had at least one group of interplanetary radio bursts
  associated with them. These dimming regions were identified by their
  strong depletion in coronal EUV emission within a half hour of the
  estimated time of CME lift-off. They included areas which were as
  dark as quiescent coronal holes as well as other regions with weaker
  brightness depletions. While the location of the active region and
  the associated flare did not correspond well with the coronagraph
  observations, we found that the extended dimming areas in these events
  generally mapped out the apparent “footprint” of the CME as observed
  by white-light coronagraph. We briefly discuss the implications of
  these results on models of CME topology.

Title: SOHO/UVCS Observations of a Coronal Jet During the Third
    Whole Sun Month Campaign
Authors: Ko, Y. -K.; Raymond, J.; Gibson, S.; Strachan, L.; Alexander,
   D.; Fletcher, L.; Holzer, T.; Gilbert, H.; Burkepile, J.; St. Cyr,
   C.; Thompson, B.
Bibcode: 2000SPD....31.0271K
Altcode: 2000BAAS...32R.823K
  On August 26 1999, a coronal jet occurred at the north west limb
  near a sigmoid active region which has been the target for a joint
  observation plan during the third Whole Sun Month Campaign. This jet
  was observed by several instruments at the limb (SOHO/CDS, SOHO/EIT,
  TRACE, MLSO/CHIP, MLSO/PICS), at 1.7 Ro (SOHO/UVCS), and at the outer
  corona (SOHO/LASCO). At 1.7 Ro, the intensities of Lyman alpha, Lyman
  beta in the jet increased by as large a factor of 100 compared with the
  background corona, while those for O VI 1032 and O VI 1037 increased
  by a factor of 2. C III 977 line also brightened significantly. The
  line shift in the lines indicates that the line-of-sight velocity in
  the jet started from 150 km/sec blue shift and ended at 120 km/sec
  red shift. This line-of-sight motion seen at 1.7 Ro apparently was
  opposite that observed when the jet emerged from the limb. In this
  paper, we present the observation by SOHO/UVCS and discuss the dynamic
  structure and physical properties of this jet as it passed through
  1.7 Ro. Comparisons will be shown with the observations from other
  instruments. This work is supported by NASA Grant number NAG5-7822.

Title: The Third Whole Sun Month Campaign - Coronal Synoptic Maps
Authors: Biesecker, D. A.; Gibson, S. E.; Alexander, D.; Fludra, A.;
   Hoeksema, J. T.; Panasyuk, A. V.; Thompson, B. J.
Bibcode: 2000SPD....31.0239B
Altcode: 2000BAAS...32..817B
  Observations for the Third Whole Sun Month Campaign were made throughout
  Carrington Rotation 1953 (August 18-September 14, 1999). As in the
  first campaign; the primary focus is on understanding the large scale
  solar corona and the connections to interplanetary space over a full
  solar rotation. The fundamental notion of these campaigns is that the
  observations are available for anyone to work with. In this poster,
  we use synoptic maps to show the morphology of the solar corona during
  CR1953 at a variety of wavelengths, heights, and temperatures. Data
  are shown from YOHKOH SXT, MLSO Mk4, and SOHO MDI, CDS, UVCS, EIT,
  and LASCO. The current campaign differs from the first campaign in that
  near solar maximum conditions prevailed. We held one workshop in order
  to get organized and begin collaborations. The planned studies will
  include determining the plasma parameters in various coronal structures
  and in modeling the structure of the coronal magnetic fields. In
  addition, we had the opportunity to study how a "sigmoidal" active
  region evolved as it crossed the solar disk and affected the global
  corona through a series of flares and eruptive events, and to obtain
  detailed observations of its structure over a wide range of heights
  and temperatures. We will be holding future workshops to analyze the
  data and work on models. We invite you to participate in this campaign
  or at least see our current plans for data analysis and modeling.

Title: Solar Phenomena Associated With EIT Waves
Authors: Myers, D. C.; Biesecker, D. A.; Vourlidas, A.; Thompson, B. J.
Bibcode: 2000SPD....31.0273M
Altcode: 2000BAAS...32..824M
  In an effort to understand what causes an "EIT wave" or what effects
  an EIT wave might have, we are investigating whether EIT waves
  can be associated directly with any other solar phenomena. An EIT
  wave is a coronal disturbance, typically appearing as a bright rim,
  observed to propagate across the Sun. Waves at the solar limb are
  identified by the deflections of magnetic fields that they cause. We
  have taken a working catalogue of "EIT waves" and determined what,
  if any, solar phenomena are associated with each wave. We have thus
  far looked for an association with GOES X-ray flares and with LASCO
  coronal mass ejections. This poster shows the work accomplished thus
  far, in particular, that there is a strong association with GOES flux
  increases and that waves with a higher quality rating tend to have
  a higher GOES flux level. We also plan to determine if there is an
  association with radio transients, particularly type II events. The
  EIT wave catalogue was compiled by examining EIT difference images of
  the Sun from the start of higher cadence images (24-March-1997). Each
  wave is classified by a quality rating from 0 to 6. The quality rating
  describes a confidence level that the given times contain an EIT wave,
  with 0 being the lowest certainty and 6 the highest. The catalogue of
  EIT waves, and this study, are still being expanded and will eventually
  encompass all EIT waves observed with a high image cadence from 1996
  through 1998.

Title: Max Millennium/Whole Sun Month Observations of a Sigmoid Region
    (AR 8668)
Authors: Zarro, D. M.; Canfield, R. C.; Nitta, N.; Myers, D. C.;
   Gregory, S. E.; Qiu, J.; Alexander, D.; Hudson, H. S.; Thompson,
   B. J.; LaBonte, B. J.
Bibcode: 2000SPD....31.0236Z
Altcode: 2000BAAS...32..817Z
  We report on observations of a sigmoidal region AR 8668 obtained
  during the Whole Sun Month #3 campaign and Max Millennium Coordinated
  Observing Program #2. The observations pertain to the period 1999
  August 16-17 during which several GOES B and C class flares occurred
  in AR 8668. Near simultaneous observations were obtained by SOHO (EIT
  195 Angstroms/ and MDI full-disk magnetograms), TRACE 171 Angstroms/,
  Yohkoh SXT, Big Bear (Hα ), and Mees (IVM vector magnetograms). The
  multi-wavelength nature of these data, combined with their overlapping
  spatial and temporal coverages, provide a unique opportunity to study
  the magnetic topology and flaring evolution of twisted flux structures
  associated with sigmoids. An objective of this study is to co-align
  images and magnetograms obtained before and during the observed flares,
  and compare the results with inferences from the topological model of
  Titov and Demoulin, A&amp;A 351, 707 (1999). We will present examples
  of these coalignments and identify sites of magnetic energy release
  that are associated with topological features (e.g. separatrices)
  predicted by this model.

Title: Observations of the 24 September 1997 Coronal Flare Waves
Authors: Thompson, B. J.; Reynolds, B.; Aurass, H.; Gopalswamy, N.;
   Gurman, J. B.; Hudson, H. S.; Martin, S. F.; St. Cyr, O. C.
Bibcode: 2000SoPh..193..161T
Altcode:
  We report coincident observations of coronal and chromospheric `flare
  wave' transients in association with a flare, large-scale coronal
  dimming, metric radio activity and a coronal mass ejection. The two
  separate eruptions occurring on 24 September 1997 originate in the
  same active region and display similar morphological features. The
  first wave transient was observed in EUV and Hα data, corresponding
  to a wave disturbance in both the chromosphere and the solar corona,
  ranging from 250 to approaching 1000 km s<SUP>−1</SUP> at different
  times and locations along the wavefront. The sharp wavefront had a
  similar extent and location in both the EUV and Hα data. The data did
  not show clear evidence of a driver, however. Both events display a
  coronal EUV dimming which is typically used as an indicator of a coronal
  mass ejection in the inner corona. White-light coronagraph observations
  indicate that the first event was accompanied by an observable coronal
  mass ejection while the second event did not have clear evidence of a
  CME. Both eruptions were accompanied by metric type II radio bursts
  propagating at speeds in the range of 500-750 km s<SUP>−1</SUP>,
  and neither had accompanying interplanetary type II activity. The
  timing and location of the flare waves appear to indicate an origin
  with the flaring region, but several signatures associated with coronal
  mass ejections indicate that the development of the CME may occur in
  concert with the development of the flare wave.

Title: Structure of a Large low-Latitude Coronal Hole
Authors: Bromage, B. J. J.; Alexander, D.; Breen, A.; Clegg, J. R.;
   Del Zanna, G.; DeForest, C.; Dobrzycka, D.; Gopalswamy, N.; Thompson,
   B.; Browning, P. K.
Bibcode: 2000SoPh..193..181B
Altcode:
  Coronal holes on the Sun are the source of high-speed solar wind
  streams that produce magnetic disturbances at the Earth. A series
  of multi-wavelength, multi-instrument observations obtained during
  the 1996 `Whole Sun Month' campaign examined a large coronal hole in
  greater detail than ever before. It appeared on the Sun in August, and
  extended from the north pole to a large active region in the southern
  hemisphere. Its physical and magnetic structure and subsequent evolution
  are described.

Title: Relationship of halo coronal mass ejections, magnetic clouds,
    and magnetic storms
Authors: Webb, D. F.; Cliver, E. W.; Crooker, N. U.; Cry, O. C. St.;
   Thompson, B. J.
Bibcode: 2000JGR...105.7491W
Altcode:
  Halo coronal mass ejections (CMEs) had been rarely reported in
  coronagraph observations of the Sun before the Solar and Heliospheric
  Observatory (SOHO) mission. Since mid-1996, however, the SOHO Large
  Angle Spectrometric Coronagraph (LASCO) instruments have observed many
  halo or partial-halo CMEs. A halo CME, especially when associated
  with solar activity near sun center, is important for space weather
  concerns because it suggests the launch of a potentially geoeffective
  disturbance toward Earth. During the post-solar minimum period from
  December 1996 to June 1997, we found that all six halo CMEs that were
  likely Earthward-directed were associated with shocks, magnetic clouds,
  and moderate geomagnetic storms at Earth 3-5 days later. The results
  imply that magnetic cloud-like structures are a general characteristic
  of CMEs. Most of the storms were driven by strong, sustained southward
  fields either in the magnetic clouds, in the post-shock region,
  or both. We discuss the characteristics of the halo events observed
  during this period, their associated signatures near the solar surface,
  and their usefulness as predictors of space weather at Earth.

Title: Yohkoh SXT and SOHO EIT Observations of Sigmoid-to-Arcade
    Evolution of Structures Associated with Halo Coronal Mass Ejections
Authors: Sterling, Alphonse C.; Hudson, Hugh S.; Thompson, Barbara J.;
   Zarro, Dominic M.
Bibcode: 2000ApJ...532..628S
Altcode:
  A subset of the solar-disk counterparts to halo coronal mass ejections
  (CMEs) displays an evolution in soft X-rays (SXR) that is characterized
  by a preflare S-shaped structure, dubbed a ``sigmoid,'' which evolves
  into a postflare cusp or arcade. We examine the morphological properties
  of the evolution of sigmoids into cusps and arcades for four such
  regions associated with SXR flares, using the Soft X-Ray Telescope
  (SXT) on the Yohkoh satellite and the EUV Imaging Telescope (EIT) on
  the Solar and Heliospheric Observatory (SOHO) satellite. Most of our
  EIT observations are with the 1.5 MK 195 Å Fe XII channel. At most,
  there is only a weak counterpart to the SXR sigmoid in the preflare 195
  Å EUV images, indicating that the preflare sigmoid has a temperature
  greater than 1.5 MK. While more identifiable than in the 195 Å channel,
  a clear preflare sigmoid is also not observed in the 2.0 MK EIT 284 Å
  Fe XV channel. During the time of the flare, however, an EUV sigmoid
  brightens near the location of the SXR preflare sigmoid. Initially
  the SXR sigmoid lies along a magnetic neutral line. As the SXR flare
  progresses, new field lines appear with orientation normal to the
  neutral line and with footpoints rooted in regions of opposite polarity;
  these footpoints are different from those of the preflare sigmoid. The
  cusp structures in SXRs develop from these newly ignited field lines. In
  EIT images, the EUV sigmoid broadens as the flare progresses, forming
  an arcade beneath the SXR cusp. Our findings are consistent with a
  standard picture in which the origin of the flare and CME is caused by
  the eruption of a filament-like feature, with the stretching of field
  lines producing a cusp. We infer that the cusp-producing fields may
  be overlying the sigmoid fields in the preflare phase, but we do not
  directly observe such preflare overlying fields.

Title: Catalogue of the 1997 SOHO-EIT coronal transient waves and
    associated type II radio burst spectra
Authors: Klassen, A.; Aurass, H.; Mann, G.; Thompson, B. J.
Bibcode: 2000A&AS..141..357K
Altcode:
  We compare the coronal transient wave phenomenon discovered by SOHO
  extreme ultraviolet observations (``EIT waves'') with the associated
  radio signature of a coronal shock wave (type II burst). 90% of the
  type II bursts are associated with an EIT wave. On average, the speed
  derived from the radio burst is about three times larger than the EIT
  wave speed. Within the sample, there is no correlation between the
  speeds of both tracers of a coronal disturbance. Under very general
  assumptions we conclude that both wave phenomena can be different
  signatures of the same fast magnetosonic disturbance.

Title: Large-Scale Evolution of the Active Region NOAA 7978, 7981,
    7986 Observed by Goes, Soho, and Yohkoh
Authors: Orlando, S.; Khan, J.; van Driel-Gesztelyi, L.; Thompson,
   B.; Fludra, A.; Foing, B.
Bibcode: 2000AdSpR..25.1913O
Altcode:
  We took part in a joint project aimed to study the large-scale
  evolution of an active region from its emergence throughout its decay
  for several solar rotations. Our interest focuses on the understanding
  of how energy is generated, released, deposited, and transformed in
  active regions. To this end, we determined physical parameters like
  intensity, temperature, and emission measure of the whole active region
  as a function of time for the entire period selected. We present the
  preliminary results of the analysis of GOES (Geosynchronous Operational
  Environmental Satellite), SOHO (Solar and Heliospheric Observatory)
  and Yohkoh data of the active region named NOAA 7978, 7981, and 7986
  observed between July and October 1996

Title: Properties of coronal mass ejections: SOHO LASCO observations
    from January 1996 to June 1998
Authors: St. Cyr, O. C.; Plunkett, S. P.; Michels, D. J.; Paswaters,
   S. E.; Koomen, M. J.; Simnett, G. M.; Thompson, B. J.; Gurman, J. B.;
   Schwenn, R.; Webb, D. F.; Hildner, E.; Lamy, P. L.
Bibcode: 2000JGR...10518169S
Altcode: 2000JGR...105.8169S; 2000JGRA..105.8169S
  We report the properties of all the 841 coronal mass ejections (CMEs)
  observed by the Solar and Heliospheric Observatory (SOHO) Large Angle
  Spectroscopic Coronagraph (LASCO) C2 and C3 white-light coronagraphs
  from January 1996 through June 1998, and we compare those properties to
  previous observations by other similar instruments. Both the CME rate
  and the distribution of apparent locations of CMEs varied during this
  period as expected based on previous solar cycles. The distribution
  of apparent speeds and the fraction of CMEs showing acceleration were
  also in agreement with earlier reports. The pointing stability provided
  by an L-1 orbit and the use of CCD detectors have resulted in superior
  brightness sensitivity for LASCO over earlier coronagraphs; however, we
  have not detected a significant population of fainter (i.e., low mass)
  CMEs. The general shape of the distribution of apparent sizes for LASCO
  CMEs is similar to those of earlier reports, but the average (median)
  apparent size of 72° (50°) is significantly larger. The larger
  average apparent size is predominantly the result of the detection of
  a population of partial and complete halo CMEs, at least some of which
  appear to be events with a significant longitudinal component directed
  along the Sun-Earth line, either toward or away from the Earth. Using
  full disk solar images obtained by the Extreme ultraviolet Imaging
  Telescope (EIT) on SOHO, we found that 40 out of 92 of these events
  might have been directed toward the Earth, and we compared the timing
  of those with the Kp geomagnetic storm index in the days following
  the CME. Although the ``false alarm'' rate was high, we found that 15
  out of 21 (71%) of the Kp&gt;=6 storms could be accounted for as SOHO
  LASCO/EIT frontside halo CMEs. If we eliminate three Kp storms that
  occurred following LASCO/EIT data gaps, then the possible association
  rate was 15 out of 18 (83%).

Title: Interplanetary Scintillation Measurements of the Solar Wind
    Above Low-Latitude Coronal Holes
Authors: Breen, A. R.; Moran, P. J.; Williams, P. J. S.; Lecinski,
   A.; Thompson, B. J.; Harra-Murnion, L. K.; Mikic, Z.; Linker, J. A.
Bibcode: 2000AdSpR..26..789B
Altcode:
  Observations of interplanetary scintillation (IPS) made using the EISCAT
  facility provide accurate measurements of solar wind velocity between 15
  and 120 solar radii. In this paper we present observations of the solar
  wind at low latitudes made between 1994 and 1997. Of 178 observations
  of the solar wind at low heliographic latitudes, 112 showed evidence of
  flow velocities significantly faster than the normal slow wind across a
  portion of the ray-path. In all cases, these enhanced flow speeds were
  clearly associated with coronal holes extending towards or across the
  heliographic equator. Fast flow from very close to the heliographic
  equator is clearly associated with equator-crossing coronal holes in
  all cases, suggesting that discrete streams of fast wind observed at
  low latitudes originate exclusively in coronal holes

Title: Energetic Particle Signatures of a Corotating Interaction
Region from a High Latitude Coronal Hole: SOHO, Wind and Ulysses
    Observations
Authors: Posner, A.; Bothmer, V.; Kunow, H.; Gosling, J. T.; Heber,
   B.; Lazarus, A. J.; Linker, J. A.; Marsden, R. G.; Mikić, Z.;
   Müller-Mellin, R.; Sanderson, T. R.; Szabo, A.; Thompson, B. J.
Bibcode: 2000AdSpR..26..865P
Altcode:
  In mid 1996 the Comprehensive Suprathermal and Energetic Particle
  Analyser (COSTEP) onboard the Solar and Heliospheric Observatory, at
  1 AU in the ecliptic plane, detected recurrent periods of enhanced
  MeV ions in association with a corotating interaction region
  (CIR). Measurements of energetic ions from the Cosmic Ray and Solar
  Particle Instrument/Low Energy Telescope (COSPIN/LET) onboard Ulysses
  taken at 5 AU, at mid-northern heliographic latitudes, showed that
  Ulysses encountered recurrent particle events during the same time
  period. We used the solar wind speeds observed at both locations to
  estimate the cor-responding solar source longitudes of the particle
  events. These longitudes are related to warps of the Sun's large high
  latitude northern coronal hole boundaries observed by SOHO's Extreme
  Ultraviolet Imaging Telescope (EIT). The findings are supported
  by threedimensional magnetohydrodynamic (MHD) calculations of the
  footpoint positions of the magnetic field lines at both spacecraft. The
  observations suggest that close to the Sun a superradial expansion of
  the fast solar wind from the Sun's high latitude northern coronal hole
  down to ecliptic latitudes is present

Title: Solar and Heliospheric Observatory Observations of a Helical
    Coronal Mass Ejection
Authors: Ciaravella, A.; Raymond, J. C.; Thompson, B. J.; van
   Ballegooijen, A.; Strachan, L.; Li, J.; Gardner, L.; O'Neal, R.;
   Antonucci, E.; Kohl, J.; Noci, G.
Bibcode: 2000ApJ...529..575C
Altcode:
  The EUV Imaging Telescope (EIT), Large Angle Spectrometric Coronagraph
  (LASCO), and Ultraviolet Coronagraph Spectrometer (UVCS) instruments
  aboard the SOHO satellite observed a prominence eruption (coronal mass
  ejection) on 1997 December 12. Ejected plasma moved at about 130 km
  s<SUP>-1</SUP> in the plane of the sky and showed Doppler shifts between
  -350 and +30 km s<SUP>-1</SUP>. The eruption appeared as a strongly
  curved arch in EIT images low in the corona. Emission in ions ranging
  from Si III to O VI in the UVCS spectra indicates a temperature range
  between 10<SUP>4.5</SUP> and 10<SUP>5.5</SUP> K. The morphology of the
  bright emission regions seen by all three instruments suggests several
  strands of a helical structure of moderate pitch angle. A reasonable
  fit to the spatial structure and the velocity evolution measured by
  UVCS is provided by a left-handed helix untwisting at a rate of about
  9×10<SUP>-4</SUP> radians s<SUP>-1</SUP>.

Title: Comparisons of Interplanetary Scintillation and Optical
    Measurements of Solar Wind Acceleration with Model Results
Authors: Breen, A. R.; de Forest, C. F.; Thompson, B. J.; McKenzie,
   J. F.; Modigliani, A.; Moran, P. J.; Williams, P. J. S.
Bibcode: 2000AdSpR..26..781B
Altcode:
  Observations of the fast, high latitude solar wind show that
  acceleration of the fast wind is complete by 10 solar radii (R),
  while measurements from the LASCO instrument on SOHO show that most
  of the acceleration takes place inside 5 R. A series of observations
  were made in September 1997 using EISCAT and the C2 and C3 coronagraphs
  aboard SOHO to measure the solar wind velocity profile from 3 R out to
  beyond 30 R. The overlapping fields of view of the instruments allowed
  direct comparisons to be made between IPS and optical estimations of
  flow velocity. Together, these measurements provide strong constraints
  on any model seeking to provide an explanation of the acceleration of
  the fast solar wind. We present the results of a comparison between
  out observations and the most recent version of the Lindau-Warsaw
  solar wind acceleration model

Title: Multi-wavelength Signatures of Coronal Mass Ejection
Authors: Gopalswamy, N.; Yashiro, S.; Kaiser, M. L.; Thompson, B. J.;
   Plunkett, S.
Bibcode: 1999spro.proc..207G
Altcode:
  We report on the near-surface and outer coronal manifestations of the
  1998 January 25 coronal mass ejection (CME) using white light, EUV,
  X-ray and hectometric radio data which reveal the three dimensional
  structure and long term evolution of the CME. We find that (i) the
  substructures of the CME (prominence core, cavity, frontal structure
  and the arcade formation) are clearly observed in X-ray and EUV
  wavelengths. (ii) The filament heats up early on and is observed as
  a backbone in X-rays. (iii) The filament also expands considerably
  as it erupts. (iv) The CME is observed through direct leading edge
  signature as well as through dimming process in X-rays and in EUV.

Title: Observations of a Propagating Disturbance in TRACE
Authors: Wills-Davey, M. J.; Thompson, B. J.
Bibcode: 1999SoPh..190..467W
Altcode:
  TRACE observations from 13 June 1998 in 171 and 195 Å wavelengths show
  a propagating disturbance, initiated near the origin of a C-class
  flare. The wave moves through and disrupts diffuse, overarching
  coronal loops. Only these overlying structures are affected by the
  wave; lower-lying coronal structures are unperturbed. The front
  does not appear in contemporaneous Lyman-α observations. The
  disturbance creates two types of displacement: (1) that of the wave
  front itself, and (2) those of large anchored magnetic structures,
  which `bob' due to the wave and show transverse velocities an order
  of magnitude smaller than those of the front. Comparisons between
  the 171 and 195 Å data show that the front appears differently at
  different temperatures. Observations in 171 Å (approx. 0.95 MK)
  show strong displacement of individual magnetic structures, while 195
  Å (approx. 1.4 MK) data reveals a strong wave front and associated
  dimming but resolve much less structural motion. There is also strong
  evidence of heating in the material engulfed by the wave front,
  and comparisons of the 171 and 195 Å data allow us to constrain the
  temperature of the plasma through which the wave is propagating to
  1-1.4 MK. Examination of the trajectories and velocities of points
  along the front suggests that the disturbance is Alfvénic in nature
  but contains a compressive component. This is best explained by a
  fast-mode magnetoacoustic wave. A comparison of the motion of anchored
  structures to that of the wave front gives a constraint on pulse
  width. Comparisons with contemporaneous SOHO-EIT full-disk 195 Å
  data show evidence that the disturbance is contained within a set of
  transequatorial field lines, such that it propagates from a southern
  active region to a northern one with no extensive motion to the east
  or west. The associated transequatorial loops display residual motion
  for about a hour after they are initially disturbed. These results,
  coupled with the deflection of wave trajectories, lead us to speculate
  on field strength differences between the transequatorial loops and
  the region in the TRACE field of view.

Title: Coronal magnetic field topology and source of fast solar wind
Authors: Guhathakurta, M.; Sittler, E.; Fisher, R.; McComas, D.;
   Thompson, B.
Bibcode: 1999GeoRL..26.2901G
Altcode:
  We have developed a steady state, 2D semi-empirical MHD model of the
  solar corona and the solar wind with many surprising results. This
  model for the first time shows, that the boundary between the fast
  and the slow solar wind as observed by Ulysses beyond 1 AU, is
  established in the low corona. The fastest wind observed by Ulysses
  (680-780 km/s) originates from the polar coronal holes at 70°-90°
  latitude at the Sun. Rapidly diverging magnetic field geometry accounts
  for the fast wind reaching down to a latitude of ±30° at the orbit
  of Earth. The gradual increase in the fast wind observed by Ulysses,
  with latitude, can be explained by an increasing field strength towards
  the poles, which causes Alfvén wave energy flux to increase towards
  the poles. Empirically, there is a direct relationship between this
  gradual increase in wind speed and the expansion factor, f, computed
  at r &gt;20R⊙. This relationship is inverse if f is computed very
  close to the Sun.

Title: Coronal Transient Waves and Coronal Shock Waves
Authors: Mann, G.; Aurass, H.; Klassen, A.; Estel, C.; Thompson, B. J.
Bibcode: 1999ESASP.446..477M
Altcode: 1999soho....8..477M
  Coronal transient (or EIT) waves have been discovered by the EIT
  instrument aboard the SOHO spacecraft as a global wave phenomenon in
  the low corona. Most of them are associated with solar type II radio
  bursts appearing predominantly in the radio frequency range 40-100
  MHz. Such type II radio bursts are signatures of shock waves travelling
  outwards in the upper corona. The mean EIT wave velocity of 290 km/s
  is well above the sound speed in the corona. Therefore, these waves are
  considered as fast magnetosonic waves propagating nearly perpendicular
  to the ambient magnetic field in the low corona. On the other hand,
  the type II burst related shock waves have mean velocities of 970
  km/s, which must be well above the local Alfven speed. Considering
  both phenomena, i.e., coronal transient waves and type II burst
  related shock waves, to be caused by the same initial energy release
  (flare), these waves can be used as diagnostic tools for the magnetic
  field in the solar corona. Thus, a magnetic field strength of about
  5 G is deduced from the EIT wave speeds at 0.08 solar radii above the
  photosphere. Such values are well expected above nonactive regions in
  the low corona. In the upper corona, i.e., at 0.5 solar radii above
  the photosphere, typical magnetic field strengths of about 2.5 G are
  deduced from the measurements. This value corresponds to a typical
  Alfven speed of 600-1000 km/s, which is well below the type II related
  shock speeds as expected.

Title: Long-Term Evolution Of Emissivity And Heating In A Solar
    Active Region
Authors: van Driel-Gesztelyi, L.; Thompson, B.; Démoulin, P.; Orlando,
   S.; Bocchialini, K.; Oláh, K.; Kövári, Z.; Deforest, C.; Khan,
   J.; Fludra, A.; Mandrini, C.
Bibcode: 1999ESASP.446..663V
Altcode: 1999soho....8..663V
  We study the evolution of the heating and emissivity of an active
  region from its birth throughout its decay during six solar rotations
  (July-Nov. 1996). We analyse multi-wavelength and multi-instrument
  data obtained from SOHO (EIT, SUMER, CDS, MDI), Yohkoh (SXT), GOES
  and 10.7cm radio data from DRAO, Canada. We take one "snapshot" per
  rotation at the time of the central meridian passage (CMP) of the
  AR, outside of time of flares, which appears to be representative
  enough to allow us to make some general conclusions about the
  long-term evolution. Deriving physical parameters like intensity
  (flux), temperature and emission measure of the entire AR vs. time,
  we formulate mathematically the change in radiation emitted by the
  decaying AR at several wavelengths. Combining the emissivity data with
  the evolution of magnetic flux density as the flux is being dispersed
  by small- and larger-scale convective motions, we make an attempt to
  understand the physics behind the emission and heating. We also analyse
  the effects of flaring on the heating of the AR, and study whether and
  how the flare properties evolve during the life of the active region.

Title: Long-Term Magnetic Evolution of an AR and its CME Activity
Authors: van Driel-Gesztelyi, L.; Mandrini, C. H.; Thompson, B.;
   Plunkett, S.; Aulanier, G.; Démoulin, P.; Schmieder, B.; de Forest, C.
Bibcode: 1999ASPC..184..302V
Altcode:
  Using SOHO/MDI full-disc magnetic maps, we follow the magnetic
  evolution of a solar active region for several months in the period of
  July-November 1996. We extrapolate the photospheric magnetic fields in
  the linear force-free approximation and match the modelled field lines
  with the soft X-ray loops observed with the Yohkoh/SXT in order to
  diagnose the coronal magnetic shear. We find that while the turbulent
  motions diffuse the flux, the differential rotation, and possibly
  twisted flux emergence, increase the magnetic shear. Flares are observed
  during the first three rotations, while CME events (observed by SOHO/EIT
  and LASCO) originate from this AR from its emergence throughout its
  decay. Several early CMEs, while none of the late CMEs, are related to
  flare events above the GOES B1 level. We find that the late CMEs occur
  when the magnetic shear, after accumulating for four rotations, reaches
  a high level and saturates. We propose that CME activity serves as a
  valve through which the AR could get rid of excess shear and helicity.

Title: SOHO EIT Observations of Extreme-Ultraviolet ``Dimming''
    Associated with a Halo Coronal Mass Ejection
Authors: Zarro, Dominic M.; Sterling, Alphonse C.; Thompson, Barbara
   J.; Hudson, Hugh S.; Nitta, Nariaki
Bibcode: 1999ApJ...520L.139Z
Altcode:
  A solar flare was observed on 1997 April 7 with the Soft X-ray Telescope
  (SXT) on Yohkoh. The flare was associated with a ``halo'' coronal
  mass ejection (CME). The flaring region showed areas of reduced soft
  X-ray (SXR) brightness--``dimmings''--that developed prior to the CME
  observed in white light and persisted for several hours following the
  CME. The most prominent dimming regions were located near the ends of
  a preflare SXR S-shaped (sigmoid) feature that disappeared during the
  event, leaving behind a postflare SXR arcade and cusp structure. Based
  upon these and similar soft X-ray observations, it has been postulated
  that SXR dimming regions are the coronal signatures (i.e., remnants)
  of magnetic flux ropes ejected during CMEs. This Letter reports
  new observations of coronal dimming at extreme-ultraviolet (EUV)
  wavelengths obtained with the Extreme-ultraviolet Imaging Telescope
  (EIT) on the Solar and Heliospheric Observatory (SOHO). A series of
  EIT observations in the 195 Å Fe XII wavelength band were obtained
  simultaneously with SXT during the 1997 April 7 flare/CME. The EIT
  observations show that regions of reduced EUV intensity developed at
  the same locations and at the same time as SXR dimming features. The
  decrease in EUV intensity (averaged over each dimming region) occurred
  simultaneously with an increase in EUV emission from flaring loops in
  the active region. We interpret these joint observations within the
  framework of flux-rope eruption as the cause of EUV and SXR coronal
  dimmings, and as the source of at least part of the CME.

Title: The Three-dimensional Coronal Magnetic Field during Whole
    Sun Month
Authors: Gibson, S. E.; Biesecker, D.; Guhathakurta, M.; Hoeksema,
   J. T.; Lazarus, A. J.; Linker, J.; Mikic, Z.; Pisanko, Y.; Riley, P.;
   Steinberg, J.; Strachan, L.; Szabo, A.; Thompson, B. J.; Zhao, X. P.
Bibcode: 1999ApJ...520..871G
Altcode:
  Combining models and observations, we study the three-dimensional
  coronal magnetic field during a period of extensive coordinated
  solar observations and analysis known as the Whole Sun Month (WSM)
  campaign (1996 August 10-September 8). The two main goals of the WSM
  campaign are addressed in this paper, namely, (1) to use the field
  configuration to link coronal features observed by coronagraphs and
  imaging telescopes to solar wind speed variations observed in situ and
  (2) to study the role of the three-dimensional coronal magnetic field
  in coronal force balance. Specifically, we consider how the magnetic
  field connects the two fastest wind streams to the two regions that
  have been the main foci of the WSM analysis: the equatorial extension
  of the north coronal hole (known as the Elephant's Trunk) and the
  axisymmetric streamer belt region on the opposite side of the Sun. We
  then quantitatively compare the different model predictions of coronal
  plasma and solar wind properties with observations and consider the
  implications for coronal force balance and solar wind acceleration.

Title: On the Origin of Impulsive Electron Events Observed at 1 AU
Authors: Krucker, Säm; Larson, Davin E.; Lin, Robert P.; Thompson,
   Barbara J.
Bibcode: 1999ApJ...519..864K
Altcode:
  A statistical survey of 12 impulsive electron events detected
  at energies down below 1 keV and 58 events detected above 25
  keV observed at 1 AU by the 3-D Plasma and Energetic Particles
  experiment on the Wind spacecraft is presented. Timing analysis of the
  velocity dispersion reveals two different kinds of electron events:
  (1) events released from the Sun at the onset of a radio type III
  burst, which suggest that these electrons are part of the population
  producing the type III radio emission; and (2) events in which the
  electrons are released up to half an hour later than the onset of
  the type III burst. These electrons therefore may be produced by a
  different acceleration mechanism than the population producing the
  radio emission. Both types of behavior can be observed during the
  same impulsive electron event at different energies, but most events
  show the same timing at all energies. At lower energies (&lt;25 keV),
  type III-related impulsive electron events are more often observed
  (nine of 12 events), whereas at higher energies (&gt;25 keV), events
  not related to type III bursts are more numerous (41 of 58). However,
  events of both classes are observed below 1 keV. Impulsive electron
  events not related to type III radio bursts are observed to be proton
  rich, with an order-of-magnitude lower electron-to-proton ratio than
  events related to type III bursts. <P />For roughly 3/4 of the events
  not related to type III bursts, large-scale coronal transient waves,
  also called EIT waves or coronal Moreton waves, are observed by the
  Extreme Ultraviolet Imaging Telescope (EIT) on board SOHO. Temporal
  and spatial correlations together with hydromagnetic simulations show
  that at least some impulsive electron events are more likely related
  to the propagating Moreton wave than to the flare phenomenon itself.

Title: Is the chromosphere hotter in coronal holes?
Authors: Gopalswamy, N.; Shibasaki, K.; Thompson, B. J.; Gurman,
   J. B.; Deforest, C. E.
Bibcode: 1999AIPC..471..277G
Altcode: 1999sowi.conf..277G
  Coronal holes are brighter than the quiet Sun in microwaves. Microwave
  emission from the quiet Sun is optically thick thermal bremsstrahlung
  from the upper chromosphere. Therefore, the optically thick layer in the
  coronal hole chromosphere must be hotter than the corresponding layer
  in the quiet chromosphere. We present microwave and SOHO observations
  in support of this idea. Because of the availability of simultaneous
  EUV and microwave images it is now possible to obtain more details
  of this enigmatic phenomenon. In this paper, we highlight the primary
  properties of the microwave enhancement in coronal holes and point out
  some related phenomena. Finally, we summarize the possible explanations
  of the radio enhancement.

Title: Large-scale structure and coronal dynamics from joint radio,
    SOHO/EIT and coronagraph observations
Authors: Pick, M.; Maia, D.; Vourlidas, A.; Benz, A. O.; Howard, R.;
   Thompson, B. J.
Bibcode: 1999AIPC..471..649P
Altcode: 1999sowi.conf..649P
  This study presents joint observations of an `halo' coronal mass
  ejection from the EIT telescope and LASCO coronagraphs on SOHO, from
  the Nançay Radioheliograph (NRH) and the Zurich ETH radiospectrograph
  (Phoenix-2). This event includes different manifestations: a coronal
  wave and a dimming region detected by EIT, a CME showing bright discrete
  portions above east and west limbs. Radio signatures of all these
  manifestations are found and the interpretation is briefly discussed.

Title: SOHO/EIT Observations of the 1997 April 7 Coronal Transient:
    Possible Evidence of Coronal Moreton Waves
Authors: Thompson, B. J.; Gurman, J. B.; Neupert, W. M.; Newmark,
   J. S.; Delaboudinière, J. -P.; Cyr, O. C. St.; Stezelberger, S.;
   Dere, K. P.; Howard, R. A.; Michels, D. J.
Bibcode: 1999ApJ...517L.151T
Altcode:
  We report observations obtained with the Extreme ultraviolet
  Imaging Telescope (EIT) on board SOHO of a large-scale coronal
  transient propagating across the disk of the Sun at a speed of 250 km
  s<SUP>-1</SUP>, in apparent association with a flare and coronal mass
  ejection. The observations consist of a series of images taken in the
  Fe XII 195 Å bandpass at an average cadence of 15 minutes. A visible
  increase in coronal emission propagates away from the erupting region,
  traveling across most of the solar disk in less than an hour. As the
  wave propagates through the ambient corona, its path is not homogeneous,
  and it is less observable near strong magnetic features such as
  active regions and magnetic neutral lines. The characteristics of
  this event appear to be representative of several other ``EIT waves,''
  which we identify as strong candidates for the coronal manifestation
  of Moreton waves.

Title: Modeling CMEs in three dimensions using an analytic MHD model
Authors: Gibson, Sarah E.; Alexander, David; Biesecker, Doug; Fisher,
   Richard; Guhathakurta, Madhulika; Hudson, Hugh; Thompson, B. J.
Bibcode: 1999AIPC..471..645G
Altcode: 1999sowi.conf..645G
  Because coronal mass ejections (CMEs) are viewed in projection,
  it is difficult to determine their three-dimensional nature. We use
  an analytic model of CMEs as an example of a fully three-dimensional
  magnetic field structure in MHD force balance with an emerging CME. We
  present the CME magnetic field and its associated density structure,
  seen projected at the limb from two viewing angles perpendicular
  to the plane of the sky, and emerging from disk center representing
  ``earth-directed'' CME events. The range of CME structures thus produced
  compares well to existing CME white-light coronagraph and full disk
  EUV and X-ray observations. In particular, we find that both 3-part
  ``front-cavity-core'' and ``U-shaped'' white light CMEs, as well as the
  twin dimmings (also referred to as transient coronal holes) observed in
  X-ray and EUV, can successfully be reproduced by the CME model. All of
  these structures are a direct consequence of a single three-dimensional
  magnetic field topology, viewed from different directions.

Title: Dynamical phenomena associated with a coronal mass ejection
Authors: Gopalswamy, N.; Kaiser, M. L.; MacDowall, R. J.; Reiner,
   M. J.; Thompson, B. J.; Cyr, O. C. St.
Bibcode: 1999AIPC..471..641G
Altcode: 1999sowi.conf..641G
  The flare-CME-shock relationship has been controversial for more than
  two decades. This issue was traditionally addressed using white light
  coronagraphic data on CMEs, H-alpha or GOES data on flares and radio
  spectrographic data on shocks (inferred from metric type II radio
  bursts). A wealth of new information has become available after the
  advent of Yohkoh, SOHO and WIND missions that can be used to address
  the dynamical phenomena associated with CMEs. We present multiwavelength
  observations of the 1998 April 27 CME associated with coronal dimming,
  an X-class flare and type II radio bursts. We find that the coronal
  dimming observed in X-rays and EUV is indeed a CME signature and that
  the CME clearly precedes the accompanying flare.

Title: Relationship between Ulysses plasma observations and solar
    observations during the Whole Sun Month campaign
Authors: Riley, Pete; Gosling, J. T.; McComas, D. J.; Pizzo, V. J.;
   Luhmann, J. G.; Biesecker, D.; Forsyth, R. J.; Hoeksema, J. T.;
   Lecinski, A.; Thompson, B. J.
Bibcode: 1999JGR...104.9871R
Altcode:
  In this report, we summarize measurements made by the plasma experiment
  on the Ulysses spacecraft during the period designated as ``Whole Sun
  Month'' (WSM, August 10 to September 8, 1996). This interval coincided
  with the return of solar wind variability at Ulysses. Ulysses was
  located at ~28°N heliographic latitude, at a heliocentric distance of
  4.25 AU, and on the opposite side of the Sun from Earth. In particular,
  we explore the evolution of the solar wind between the Sun and
  Ulysses for several rotations surrounding WSM. Specifically, we map
  Ulysses measurements back toward the Sun by applying a two-dimensional
  inverse MHD algorithm. This approach is compared with the commonly
  used constant speed (or ballistic) approximation. We find that the MHD
  mapping technique produces substantially better results when compared
  with solar observations. Both the Ulysses MHD-mapped results and the
  solar observations are consistent with a picture of a modestly tilted
  streamer belt (&lt;10°) that was deformed northward by an active
  region at 240°-270° longitude.

Title: SOHO Observations of a Helical Coronal Mass Ejection
Authors: Raymond, J. C.; Ciaravella, A.; van Ballegooijen, A.;
   Thompson, B.
Bibcode: 1999AAS...194.1701R
Altcode: 1999BAAS...31..853R
  The EIT, LASCO and UVCS instruments aboard SOHO observed a CME on
  Dec. 11/12 1997. The ejected prominence material rose relatively
  slowly, averaging 150 km/s, but Doppler shifts as great at -300 km/s
  were seen in the O VI lines. The observed gas spans the temperature
  range from about 30,000 K to 300,000 K. The observations can
  be modeled as left-handed helix which untwists at about 0.0009
  radians/sec. Considerable heating as the plasma moves from the
  solar surface to 1.7 solar radii is required to explain the observed
  temperature range.

Title: Microwave enhancement and variability in the elephant's trunk
coronal hole: Comparison with SOHO observations
Authors: Gopalswamy, N.; Shibasaki, K.; Thompson, B. J.; Gurman, J.;
   DeForest, C.
Bibcode: 1999JGR...104.9767G
Altcode:
  We report on an investigation of the microwave enhancement and its
  variability in the elephant's trunk coronal hole observed during the
  Whole Sun Month campaign (August 10 to September 9, 1996). The microwave
  images from the Nobeyama radioheliograph were compared with magnetograms
  and EUV images obtained simultaneously by the Michelson Doppler imager
  and the extreme ultraviolet imaging telescope (EIT) on board the SOHO
  spacecraft. The combined data set allowed us to understand the detailed
  structure of the microwave enhancement in the spatial and temporal
  domains. We find that the radio enhancement is closely associated
  with the enhanced unipolar magnetic regions underlying the coronal
  hole. The radio enhancement consists of a smooth component originating
  from network cell interiors and a compact component associated with
  network magnetic elements. When a minority polarity is present near
  a majority polarity element, within the coronal hole, the resulting
  mixed polarity region is associated with a bright-point-like emission
  in coronal EUV lines such as the Fe XII 195 Å. These coronal bright
  points are also observed distinctly in the EIT 304 Å band, but not
  in microwaves. On the other hand, the lower-temperature line emission
  (304 Å) and the microwave enhancement are associated with the unipolar
  magnetic flux elements in the network. We found strong time variability
  of the radio enhancement over multiple timescales, consistent with the
  initial results obtained by SOHO instruments. The microwave enhancement
  is most probably due to temperature enhancement in the chromosphere
  and may be related to the origin of solar wind.

Title: Multi-wavelength observations of the onset phase of a coronal
    mass ejection
Authors: Innes, D. E.; Inhester, B.; Srivastava, N.; Brekke, P.;
   Harrison, R. A.; Matthews, S. A.; Noëns, J. C.; Schmieder, B.;
   Thompson, B. J.
Bibcode: 1999SoPh..186..337I
Altcode:
  The structure and dynamics of the initial phases of a coronal mass
  ejection (CME) seen in soft X-ray, extreme ultraviolet and optical
  emission are described. The event occurred on the SW limb of the Sun in
  active region AR 8026 on 9 April 1997. Just prior to the CME there was
  a class C1.5 flare. Images taken with the Extreme Ultraviolet Imaging
  Telescope (EIT) reveal the emergence of a candle-flame shaped extreme
  ultraviolet (EUV) cavity at the time of the flare. Yohkoh images,
  taken about 15 min later, show that this cavity is filled with hot
  X-ray emitting gas. It is most likely that this is the site of the
  flare. Almost simultaneous to the flare, an Hα surge or small filament
  eruption occurs about 50 arc sec northwards along the limb from the EUV
  cavity. At both the site of the core of the hot, EUV cavity and the
  filament ejection are X-ray jets. These jets seem to be connected by
  hot loops near their bases. Both jets disappear within a few minutes
  of one another.

Title: In-ecliptic CIR-associated energetic particle events and polar
coronal hole structures: SOHO/COSTEP observations for the Whole Sun
    Month Campaign
Authors: Posner, Arik; Bothmer, Volker; Thompson, Barbara J.; Kunow,
   Horst; Heber, Bernd; Müller-Mellin, Reinhold; Lazarus, Alan J.;
   Szabo, Adam; Mikić, Zoran; Linker, Jon A.
Bibcode: 1999JGR...104.9881P
Altcode:
  The Solar and Heliospheric Observatory (SOHO), in halo orbit around
  the L1 Lagrangian point of the Sun-Earth system, combines a unique
  set of instruments for studies of the Sun and the heliosphere. SOHO's
  Comprehensive Suprathermal and Energetic Particle Analyser measures
  in situ particles in the energy range 44 keV/particle to above 53
  MeV/nucleon. For the time period of the Whole Sun Month Campaign in
  mid 1996 we have identified recurrent energetic particle intensity
  increases in association with corotating interaction regions (CIRs)
  in the energy range &lt;10 MeV. Solar wind measurements of the Wind
  spacecraft were used to estimate the corresponding magnetic source
  location in Carrington longitude for comparison of energetic particles
  with synoptic maps of the lower corona, derived from images of SOHO's
  Extreme-ultraviolet Imaging Telescope. The comparison reveals a close
  relationship of latitudinal extensions of polar coronal holes, situated
  in regions up to 40° away from the ecliptic, with CIR-associated
  in-ecliptic particle events.

Title: Soft X-ray Observation of a Flare-Associated Coronal Wave
Authors: Hudson, H. S.; Lemen, J. R.; Thompson, B.; Uchida, Y.
Bibcode: 1999AAS...194.2205H
Altcode: 1999BAAS...31..860H
  Recent EUV observations from the EIT instrument of SOHO have shown
  the common occurrence of flare-associated global coronal waves, allies
  of Type II burst exciters and chromospheric Moreton waves. Until now,
  however, no direct soft X-ray detections have been reported. We have
  studied Yohkoh SXT observations to understand this apparent discrepancy
  between EUV and soft X-ray observations,and have now found good X-ray
  evidence for a large-scale coronal wave launched during an X-class
  flare of May 6, 1998. During the impulsive phase of this flare, a rapid
  ( ~ 10(3) km s(-1) ) bright front appeared to the north of the flare
  core; later a more normal loop-like ejection emerged to the west at a
  lower projected speed. We identify the rapid front with enhanced X-ray
  emission from a global coronal wave. Wave signatures also appear in
  SOHO EIT images and in the meter-wave dynamic spectrum from Hiraiso,
  and SOHO LASCO detected a coronal mass ejection. NASA supported this
  work under contract NAS 8-37334.

Title: YOHKOH SXT and SOHO EIT Observations of ``Sigmoid-to-Arcade''
    Evolution of Structures Associated with Halo CMEs
Authors: Sterling, A. C.; Hudson, H. S.; Thompson, B. J.; Zarro, D. M.
Bibcode: 1999AAS...19410107S
Altcode: 1999BAAS...31..999S
  A subset of the solar-disk counterparts to halo coronal mass ejections
  (CMEs) display an evolution in soft X-rays (SXR) characterized by a
  preflare ``S''-shaped structure, dubbed a ``sigmoid,'' evolving into
  a postflare cusp or arcade. We examine the morphological properties
  of the evolution of sigmoids into cusps and arcades for four such
  regions associated with SXR flares, using the Soft X-ray Telescope
  (SXT) on Yohkoh and the 195 Angstroms Fe xii\ channel of the EUV Imaging
  Telescope (EIT) on SOHO. There is, at most, only a weak counterpart to
  the SXR sigmoid in the preflare EUV images, indicating that the preflare
  sigmoid has a temperature &gt;1.5 MK\@. During the time of the flare
  itself, however, an EUV sigmoid brightens near the location of the
  SXR preflare sigmoid. Initially the SXR sigmoid lies along a magnetic
  neutral line. As the SXR flare progresses new field lines appear with
  orientation normal to the neutral line and with footpoints rooted in
  opposite polarity regions; these footpoints are different from those of
  the preflare sigmoid. The cusp structures in SXRs develop from these
  newly-ignited field lines. In EIT images the EUV sigmoid broadens out
  as the flare progresses, forming an arcade which resides beneath the
  SXR cusp. In many respects, our findings are consistent with a standard
  picture where the origin of the flare and CME is due to the eruption
  of a filament-like feature, and the stretching of overlying preflare
  fields produces the cusp. We do not, however, observe these preflare
  overlying fields prior to flare onset. This work was supported by the
  NRL Naval basic research program and NASA.

Title: Magnetohydrodynamic modeling of the solar corona during Whole
    Sun Month
Authors: Linker, J. A.; Mikić, Z.; Biesecker, D. A.; Forsyth, R. J.;
   Gibson, S. E.; Lazarus, A. J.; Lecinski, A.; Riley, P.; Szabo, A.;
   Thompson, B. J.
Bibcode: 1999JGR...104.9809L
Altcode:
  The Whole Sun Month campaign (August 10 to September 8, 1996) brought
  together a wide range of space-based and ground-based observations
  of the Sun and the interplanetary medium during solar minimum. The
  wealth of data collected provides a unique opportunity for testing
  coronal models. We develop a three-dimensional magnetohydrodynamic
  (MHD) model of the solar corona (from 1 to 30 solar radii) applicable
  to the WSM time period, using measurements of the photospheric
  magnetic field as boundary conditions for the calculation. We compare
  results from the computation with daily and synoptic white-light and
  emission images obtained from ground-based observations and the SOHO
  spacecraft and with solar wind measurements from the Ulysses and WIND
  spacecraft. The results from the MHD computation show good overall
  agreement with coronal and interplanetary structures, including the
  position and shape of the streamer belt, coronal hole boundaries,
  and the heliospheric current sheet. From the model, we can infer the
  source locations of solar wind properties measured in interplanetary
  space. We find that the slow solar wind typically maps back to near
  the coronal hole boundary, while the fast solar wind maps to regions
  deeper within the coronal holes. Quantitative disagreements between
  the MHD model and observations for individual features observed during
  Whole Sun Month give insights into possible improvements to the model.

Title: Interplanetary scintillation measurements of the solar
wind during Whole Sun Month: Comparisons with coronal and in situ
    observations
Authors: Breen, A. R.; Mikic, Z.; Linker, J. A.; Lazarus, A. J.;
   Thompson, B. J.; Biesecker, D. A.; Moran, P. J.; Varley, C. A.;
   Williams, P. J. S.; Lecinski, A.
Bibcode: 1999JGR...104.9847B
Altcode:
  Two-site observations of interplanetary scintillation using the
  EISCAT facility can provide measurements of solar wind velocity at
  any point in the heliosphere between 15 and 120 solar radii (R). In
  this paper we discuss a series of observations made as part of the
  Whole Sun Month campaign (August 10 to September 8 1996) and compare
  the results with coronal data and in-situ measurements made during
  the campaign. The results of the comparison revealed extremely good
  agreement between solar wind speeds measured by IPS at 16-73 R and in
  situ measurements at 213 R and beyond, both in the general morphology of
  the solar wind and in the absolute velocities observed. These results
  confirm that structures in the solar wind, originating in the corona,
  preserve their form out to 910 R or more. Observations of fast solar
  wind were always associated with coronal holes and slow wind with the
  bright corona. Velocities intermediate between normal fast and slow
  flow speeds are associated with interaction regions between fast and
  slow flow and are also found above the boundaries of coronal holes.

Title: Synoptic Sun during the first Whole Sun Month Campaign:
    August 10 to September 8, 1996
Authors: Biesecker, D. A.; Thompson, B. J.; Gibson, S. E.; Alexander,
   D.; Fludra, A.; Gopalswamy, N.; Hoeksema, J. T.; Lecinski, A.;
   Strachan, L.
Bibcode: 1999JGR...104.9679B
Altcode:
  A large number of synoptic maps from a variety of instruments are used
  to show the general morphology of the Sun at the time of the First
  Whole Sun Month Campaign. The campaign was conducted from August 10 to
  September 8, 1996. The synoptic maps cover the period from Carrington
  rotation 1912/253° to Carrington rotation 1913/45°. The synoptic maps
  encompass both on-disk data and limb data from several heights in the
  solar atmosphere. The maps are used to illustrate which wavelengths and
  data sets show particular features, such as active regions and coronal
  holes. Of particular interest is the equatorial coronal hole known as
  the ``elephant's trunk,'' which is clearly evident in the synoptic
  maps of on-disk data. The elephant's trunk is similar in appearance
  to the Skylab-era, ``Boot of Italy,'' equatorial coronal hole. The
  general appearance of the limb maps is explained as well. The limb
  maps also show evidence for equatorial coronal holes.

Title: The Characteristics and Geoeffectiveness of SOHO-LASCO
    Halo CMEs
Authors: Webb, D. F.; St. Cyr, O. C.; Plunkett, S. P.; Howard, R. A.;
   Thompson, B. J.
Bibcode: 1999AAS...194.1703W
Altcode: 1999BAAS...31..853W
  Halo-type CMEs had been rarely reported in solar coronagraph
  observations before the SOHO mission. Because of their increased
  sensitivity and dynamic range, the SOHO LASCO coronagraphs are now
  observing many halo or partial-halo CMEs. A halo CME, especially
  when associated with solar activity near sun center, is important
  for Space Weather concerns because it suggests the launch of
  a geoeffective disturbance toward Earth. We present statistical
  summaries of the LASCO halo CMEs observed during the first 2.5 years
  of SOHO observations. These include their occurrence rates, speeds
  and morphology, and comparison of the halo CME population with the
  general characteristics of all LASCO CMEs during this period. As a
  test of the geoeffectiveness of halo CMEs, we also examined a 6-month
  period just after solar minimum from December 1996 through May 1997
  during which halo CMEs and geomagnetic storms occurred at a similar
  rate of 2-3/month. All 7 of the halo CMEs confidently associated with
  frontside activity were followed 3-5 days later by interplanetary
  shocks, magnetic clouds and moderate storms at Earth. In the opposite
  sense most of the moderate storms during this period were associated
  with halo CMEs. We will present the results of this study. This work
  was supported by AFOSR grant AF49620-97-1-0070.

Title: Injection of&gt;~10 MeV Protons in Association with a Coronal
    Moreton Wave
Authors: Torsti, Jarmo; Kocharov, Leon G.; Teittinen, Matti; Thompson,
   Barbara J.
Bibcode: 1999ApJ...510..460T
Altcode:
  We report extreme-UV observations of the coronal Moreton wave and
  concurrent observations of ~10-100 MeV protons. Observations are
  carried out with the Extreme-UV Imaging Telescope and the Energetic
  and Relativistic Nuclei and Electron instrument on board the SOHO
  spacecraft. We study the proton events associated with coronal mass
  ejections (CMEs) centered near the central meridian. Observations reveal
  the initial injection of &gt;~10 MeV protons during the period when the
  coronal Moreton wave was traversing the western hemisphere of the Sun,
  this being an early signature of the CME launch. Acceleration of the
  CME-associated protons starts during the CME liftoff, while the main
  proton production occurs several hours later, when the CME expands
  in the interplanetary medium. Between the first proton production
  and the maximum intensity time, a spectral softening is observed. We
  analyze in detail the 1997 September 24 event. Development of the
  event indicates that the spectral softening may be due to a change
  in the acceleration regime, so the proton production starts with the
  less intensive but hard-spectrum injection and then moves to the more
  intensive but soft-spectrum injection farther from the Sun.

Title: Ultraviolet and Optical Observations of a Coronal Transient
    with SOHO
Authors: Ciaravella, A.; Raymond, J. C.; Strachan, L.; Thompson,
   B. J.; Cyr, O. C. St.; Gardner, L.; Modigliani, A.; Antonucci, E.;
   Kohl, J.; Noci, G.
Bibcode: 1999ApJ...510.1053C
Altcode:
  A coronal transient was observed on 1997 March 6 at 1.6
  R<SUB>solar</SUB> over an active region on the east limb. We observed
  both the edge of horizontally compressed gas and the diffuse curtain of
  coronal material. The region was monitored for 4 hr, and the H I Lyα,
  O VI λλ1031.91, 1037.61, N V λλ1242.80, 1238.80, and O V] λ1218.35
  lines were detected during the ejection evolution. The density,
  velocity, temperature, and oxygen abundance of the ejected plasma have
  been obtained from the observed spectra. Intermediate temperature lines
  of N V, O VI, and O V show a large enhancement, suggesting a quite
  narrow range of plasma temperature around 4×10<SUP>5</SUP> K. Doppler
  shifts of the ejected material evolve from an initial blueshift of 100
  km s<SUP>-1</SUP> to a redshift of 145 km s<SUP>-1</SUP>. The outflow
  velocity, as determined by Doppler dimming analysis of the O VI doublet,
  is only about 20 km s<SUP>-1</SUP>.

Title: Tales of an Elephant's Trunk
Authors: Bromage, B. J. I.; Clegg, J. R.; Del Zanna, G.; Thompson, B.
Bibcode: 1999ASPC..158..370B
Altcode: 1999ssa..conf..370B
  No abstract at ADS

Title: Nonthermal Radio Signatures of Coronal Disturbances with and
    without Coronal Mass Ejections
Authors: Aurass, H.; Vourlidas, A.; Andrews, M. D.; Thompson, B. J.;
   Howard, R. H.; Mann, G.
Bibcode: 1999ApJ...511..451A
Altcode:
  This study presents data on two events from the Extreme-UV Imaging
  Telescope (EIT) and the Large Angle and Spectroscopic Coronagraph
  instruments (C1, C2, and C3), Geostationary Operational Environmental
  Satellite (GOES) soft X-ray data, and 40-800 MHz radio spectra of the
  Astrophysical Institute Potsdam. At first glance, the two events appear
  similar. However, one event decays after a flare-related ejection of
  cold and hot matter into the lower corona causing only brightness
  changes in EIT and C1, while the other event marks the onset of a
  coronal mass ejection (CME) that propagates with a leading-edge speed
  of ~530 km s<SUP>-1</SUP> between 2 and 30 R<SUB>solar</SUB>. The
  radio data reveal two differences between the CME and non-CME events:
  (1) a characteristic faint type III burst group in the time interval
  with the first clearly CME-related structural change in the coronagraph
  images and (2) a continuum emission with a frequency drift during the
  passage of the CME matter through the C1 field of view. Furthermore,
  we show that the radio spectral data can provide essential information
  on the timing of the early stages of CME formation and the initial
  mass motions associated with the ejection.

Title: Observations of Coronal Structures Above an Active Region by
    EIT and Implications for Coronal Energy Deposition
Authors: Neupert, W. M.; Newmark, J.; Delaboudinière, J. -P.;
   Thompson, B. J.; Catura, R. C.; Moses, J. D.; Gurman, J. B.;
   Portier-Fozzani, F.; Gabriel, A. H.; Artzner, G.; Clette, F.; Cugnon,
   P.; Maucherat, A. J.; Defise, J. M.; Jamar, C.; Rochus, P.; Dere,
   K. P.; Howard, R. A.; Michels, D. J.; Freeland, S.; Lemen, J. R.;
   Stern, R. A.
Bibcode: 1998SoPh..183..305N
Altcode:
  Solar EUV images recorded by the EUV Imaging Telescope (EIT) on SOHO
  have been used to evaluate temperature and density as a function of
  position in two largescale features in the corona observed in the
  temperature range of 1.0-2.0 MK. Such observations permit estimates
  of longitudinal temperature gradients (if present) in the corona and,
  consequently, estimates of thermal conduction and radiative losses
  as a function of position in the features. We examine two relatively
  cool features as recorded in EIT's Fe ix/x (171 Å) and Fe xii (195 Å)
  bands in a decaying active region. The first is a long-lived loop-like
  feature with one leg, ending in the active region, much more prominent
  than one or more distant footpoints assumed to be rooted in regions of
  weakly enhanced field. The other is a near-radial feature, observed
  at the West limb, which may be either the base of a very high loop
  or the base of a helmet streamer. We evaluate energy requirements to
  support a steady-state energy balance in these features and find in
  both instances that downward thermal conductive losses (at heights
  above the transition region) are inadequate to support local radiative
  losses, which are the predominant loss mechanism. The requirement that a
  coronal energy deposition rate proportional to the square of the ambient
  electron density (or pressure) is present in these cool coronal features
  provides an additional constraint on coronal heating mechanisms.

Title: Erupting Solar Magnetic Flux Ropes - Theory and Observation
Authors: Krall, J.; Chen, J.; Santoro, R. A.; Duffin, R. T.; Howard,
   R. A.; Thompson, B. J.
Bibcode: 1998APS..DPP.F3S20K
Altcode:
  The dynamics of magnetic flux ropes near the sun and in interplanetary
  space are studied using a modified version of the flux rope model of
  Chen and Garren. (Chen and Garren, GRL, 20, 2319, 1993) In this model, a
  coronal mass ejection (CME) corresponds to a flux rope with foot points
  that remain anchored in the photosphere. The model flux rope eruption
  can be driven by a rapid increase in poloidal flux (flux injection), a
  gradual increase in poloidal flux (photospheric foot-point twisting), or
  a rapid increase in the volume of hot plasma within the flux rope (mass
  injection). Model results are compared with data from the LASCO and EIT
  instruments on the Solar and Heliospheric Observatory spacecraft and
  with interplanetary magnetic cloud data over the range 0.5 to 4.0 AU.

Title: First VLA Observations of Nonthermal Metric Bursts Associated
    with Coronal Mass Ejections Detected by the Solar and Heliospheric
    Observatory
Authors: Willson, R. F.; Redfield, S. L.; Lang, K. R.; Thompson,
   B. J.; St. Cyr, O. C.
Bibcode: 1998ApJ...504L.117W
Altcode:
  We present the first observations of nonthermal decimetric burst
  emission of the Sun using the new 400 cm (74 MHz) system at the VLA. Our
  VLA observations were carried out in collaboration with the Large
  Angle Spectroscopic Coronagraph (LASCO) and the Extreme-Ultraviolet
  Imaging Telescope (EIT) on board the Solar and Heliospheric Observatory
  spacecraft. Full-disk observations at 400 and 91 cm were used to
  study the spatial and temporal variations of nonthermal radio bursts
  during coronal mass ejections (CMEs) detected by LASCO as well as
  transient extreme-ultraviolet brightenings detected by the EIT. VLA
  snapshot maps at 400 cm revealed impulsive burst emission in the low
  corona that began near the estimated start time of the CME activity;
  that beginning also coincided with a C1.1 GOES X-ray burst and an EIT
  flarelike brightening. The nonthermal metric bursts then continued
  sporadically during the next several hours, which included the ejection
  of spatially separated CME components. The 400 cm bursts are contained
  within curved, or archlike, sources at a fixed radial distance but with
  a varying position between two active regions detected by the EIT near
  the limb, suggesting that they were emitted within large-scale magnetic
  loops. Our 91 cm observations also show the onset of a long-lasting type
  I noise storm following the initiation of CME activity, again suggesting
  an intimate relationship between the production of nonthermal particles
  and large-scale evolving plasma-magnetic field structures in the corona.

Title: Geomagnetic storms caused by coronal mass ejections (CMEs):
    March 1996 through June 1997
Authors: Brueckner, G. E.; Delaboudiniere, J. -P.; Howard, R. A.;
   Paswaters, S. E.; St. Cyr, O. C.; Schwenn, R.; Lamy, P.; Simnett,
   G. M.; Thompson, B.; Wang, D.
Bibcode: 1998GeoRL..25.3019B
Altcode:
  (1) All but two geomagnetic storms with Kp ≥ 6 during the operating
  period (March 1996 through June 1997) of the Large Angle Spectroscopic
  Coronagraph (LASCO) experiment on the Solar and Heliospheric Observatory
  (SOHO) spacecraft can be traced to Coronal Mass Ejections (CMEs). (2)
  These geomagnetic storms are not related to high speed solar wind
  streams. (3) The CMEs which cause geomagnetic effects, can be classified
  into two categories: Halo events and toroidal CMEs. (4) The CMEs are
  accompanied by Coronal Shock Waves as seen in the Extreme Ultraviolet
  Imaging Telescope (EIT) Fe XII images. (5) Some CMEs are related to
  flares, others are not. (6) In many cases, the travel time between
  the explosion on the Sun and the maximum geomagnetic activity is about
  80 hours.

Title: The Solar Minimum Active Region 7978, Its X2.6/1B Flare, CME,
    and Interplanetary Shock Propagation of 9 July 1996
Authors: Dryer, M.; Andrews, M. D.; Aurass, H.; DeForest, C.; Galvin,
   A. B.; Garcia, H.; Ipavich, F. M.; Karlický, M.; Kiplinger, A.;
   Klassen, A.; Meisner, R.; Paswaters, S. E.; Smith, Z.; Tappin,
   S. J.; Thompson, B. J.; Watari, S. I.; Michels, D. J.; Brueckner,
   G. E.; Howard, R. A.; Koomen, M. J.; Lamy, P.; Mann, G.; Arzner, K.;
   Schwenn, R.
Bibcode: 1998SoPh..181..159D
Altcode:
  The first X-class flare in four years occurred on 9 July 1996. This
  X2.6/1B flare reached its maximum at 09:11 UT and was located in active
  region 7978 (S10° W30°) which was an old-cycle sunspot polarity
  group. We report the SOHO LASCO/EIT/MDI and SOONSPOT observations before
  and after this event together with Yohkoh SXT images of the flare,
  radio observations of the type II shock, and GOES disk-integrated soft
  X-ray flux during an extended period that included energy build-up in
  this active region.

Title: On the relationship between coronal mass ejections and
    magnetic clouds
Authors: Gopalswamy, N.; Hanaoka, Y.; Kosugi, T.; Lepping, R. P.;
   Steinberg, J. T.; Plunkett, S.; Howard, R. A.; Thompson, B. J.;
   Gurman, J.; Ho, G.; Nitta, N.; Hudson, H. S.
Bibcode: 1998GeoRL..25.2485G
Altcode:
  We compare the substructures of the 1997 February 07 coronal mass
  ejection (CME) observed near the Sun with a corresponding event in
  the interplanetary medium to determine the origin of magnetic clouds
  (MCs). We find that the eruptive prominence core of the CME observed
  near the Sun may not directly become a magnetic cloud as suggested by
  some authors and that it might instead become the ”pressure pulse”
  following the magnetic cloud. We substantiate our conclusions using time
  of arrival, size and composition estimates of the CME-MC substructures
  obtained from ground based, SOHO and WIND observations.

Title: Type II radio emissions in the frequency range from 1-14 MHz
    associated with the April 7, 1997 solar event
Authors: Kaiser, M. L.; Reiner, M. J.; Gopalswamy, N.; Howard, R. A.;
   St. Cyr, O. C.; Thompson, B. J.; Bougeret, J. -L.
Bibcode: 1998GeoRL..25.2501K
Altcode:
  We present an analysis of radio emissions associated with the April
  7, 1997 solar eruptive event. The event consisted of a filament
  disappearance, a complex two-phase coronal mass ejection (CME),
  and a C6.9, 2N flare. At the same time, intermittent type II radio
  emissions in the frequency range 1-10 MHz, corresponding to an altitude
  range of 2-15 R<SUB>o</SUB>, were observed by the Wind/WAVES radio
  receiver. Using the onset times and inferred heights and speeds
  of the radio bursts, we considered both a CME-driven shock and a
  flare-associated blast wave shock as possible causes of the type II
  radio emissions. We conclude that some of the radio emissions in the
  WAVES data are associated with each shock. The type II radio emissions
  associated with the blast wave shock were farther from the sun than
  any emission of this type that has been reported previously.

Title: Cradle to grave tracking of the January 6-11,1997 Sun-Earth
    connection event
Authors: Fox, N. J.; Peredo, M.; Thompson, B. J.
Bibcode: 1998GeoRL..25.2461F
Altcode:
  During the interval January 6-11, 1997, the satellites and ground
  facilities of the International Solar-Terrestrial Physics (ISTP)
  “Observatory” tracked a solar eruption from the Sun to the
  Earth. The resulting Coronal Mass Ejection (CME) took four days to
  travel through interplanetary space before arriving at Earth, where it
  caused electromagnetic disturbances and spectacular aurorae. The initial
  expulsion lifted off the Sun on January 6, the resulting magnetic
  cloud arrived on January 10, and its effects lasted over 24 hours. The
  initial solar observations from SOHO were reported on January 7, during
  an ISTP Science Workshop on Sun-Earth Connection events. This alerted
  the community to the impending arrival of the CME thereby allowing the
  event to be monitored in ‘realtime’ using the wide variety of ISTP
  instruments. This event provided the first ever end to end tracking of
  a space storm. Further, it provided a strong pressure pulse of extremely
  high density resulting in the compression of the magnetopause to within
  geosynchronous orbit during northward IMF conditions. Here we present
  an overview of the event and available observations.

Title: Evidence for multiple ejecta: April 7-11, 1997, ISTP Sun-Earth
    connection event
Authors: Berdichevsky, D.; Bougeret, J. -L.; Delaboudinière, J. -P.;
   Fox, N.; Kaiser, M.; Lepping, R.; Michels, D.; Plunkett, S.; Reames,
   D.; Reiner, M.; Richardson, I.; Rostoker, G.; Steinberg, J.; Thompson,
   B.; von Rosenvinge, T.
Bibcode: 1998GeoRL..25.2473B
Altcode:
  Evidence is presented that the enhanced geomagnetic activity, on
  April 10-11, 1997, was caused by one of two ejecta that left the
  Sun at ≈ 14 UT on April 7. This ejecta was not directly detected
  at the Earth. The evidence for this interpretation is based on WIND
  spacecraft observations in the solar wind (SW). It is consistent with:
  (i) measured velocities of the coronal mass ejections from the SOHO
  coronagraph; (ii) the initial propagation speed of the shock generated
  in this event, estimation from type II radio burst observations from the
  WAVES instrument on WIND, and (iii) the time profile of energetic ions
  observed by EPACT on WIND. This locally unobserved ejecta (moving at 600
  to 700 kms<SUP>-1</SUP>) generated a fast shock which accelerated ions
  to several tens of MeV/amu. The inferred passage of the first ejecta
  close to Earth (on April 10 to 11) is based on the observation of an
  interplanetary shock (IS) ahead of a field and plasma compressional
  region where the draping of the SW flow and possibly the changes in
  the direction of the IMF are consistent with a location northward of a
  faster ejecta. This ejecta was responsible for disturbed SW conditions
  including approximately ten hours of southward orientation of the
  interplanetary magnetic field (IMF) and a ram pressure many times
  above normal. The slower moving ejecta was directed toward Earth and
  was observed with WIND from about 0550 until 1500 UT on April 11. It
  had a strong northward IMF and produced density enhancements which
  elevated the ram pressure to more than four times above normal.

Title: LASCO observations of an Earth-directed coronal mass ejection
    on May 12, 1997
Authors: Plunkett, S. P.; Thompson, B. J.; Howard, R. A.; Michels,
   D. J.; St. Cyr, O. C.; Tappin, S. J.; Schwenn, R.; Lamy, P. L.
Bibcode: 1998GeoRL..25.2477P
Altcode:
  Coronal mass ejections (CMEs) that occur near the center of the
  solar disk are most likely to impact Earth. Detection of such
  events as ‘halos’ in white-light coronagraphs has been somewhat
  controversial in recent years. We present observations from the LASCO
  coronagraphs on SOHO that provide convincing evidence of the detection
  of an Earth-directed CME on May 12, 1997. The event began at about
  04:35 UT and propagated outwards from the Sun with a projected speed
  of around 250 km s<SUP>-1</SUP>. Using some reasonable assumptions
  about the geometry of the CME, we estimate the true speed to be around
  600 km s<SUP>-1</SUP>. The onset of the event in LASCO is coincident
  (to within measurement uncertainties) with an eruptive event detected
  in extreme ultraviolet observations of the solar disk by the SOHO
  EIT. This is the first reported observation of a halo CME at projected
  distances greater than 10 R<SUB>⊙</SUB>, with a clearly identifiable
  solar origin. We discuss the possibility that at least some of the
  enhanced brightness observed by LASCO may be due to a compressional
  wave propagating in the corona.

Title: SOHO/EIT observations of an Earth-directed coronal mass
    ejection on May 12, 1997
Authors: Thompson, B. J.; Plunkett, S. P.; Gurman, J. B.; Newmark,
   J. S.; St. Cyr, O. C.; Michels, D. J.
Bibcode: 1998GeoRL..25.2465T
Altcode:
  An earth-directed coronal mass ejection (CME) was observed on May 12,
  1997 by the SOHO Extreme ultraviolet Imaging Telescope (EIT). The CME,
  originating north of the central solar meridian, was later observed by
  the Large Angle Spectrometric Coronagraph (LASCO) as a “halo” CME:
  a bright expanding ring centered about the occulting disk. Beginning at
  about 04:35 UT, EIT recorded several CME signatures, including dimming
  regions close to the eruption, post-eruption arcade formation, and a
  bright wavefront propagating quasi-radially from the source region. Each
  of these phenomena appear to be associated with the same eruption, and
  the onset time of these features corresponds with the estimated onset
  time observed in LASCO. We discuss the correspondence of these features
  as observed by EIT with the structure of the CME in the LASCO data.

Title: Empirical Models of Temperature, Densities, and Velocities
    in the Solar Corona
Authors: Fludra, A.; Strachan, L.; Alexander, D.; Bagenal, F.;
   Biesecker, D. A.; Dobrzycka, D.; Galvin, A. B.; Gibson, S.; Hassler,
   D.; Yo, Y. -K.; Panasyuk, A. V.; Thompson, B.; Warren, H.; del Zanna,
   G.; Zidowitz, S.; Antonucci, E.; Bromage, B. J. I.; Giordano, S.
Bibcode: 1998EOSTr..79..278F
Altcode:
  We present empirical results for temperatures, densities, and outflow
  velocities of constituents of the solar corona from 1 to 3 Ro in
  polar coronal holes and an equatorial streamer. Data were obtained
  from a variety of space and ground-based instruments during August
  1996 as part of the SOHO Whole Sun Month Campaign. From white light
  data obtained with the SOHO/LASCO/C2 and HAO/Mauna Loa coronagraphs,
  we determine electron densities and compare them to those determined
  from the density-sensitive EUV line ratio of Si IX 350/342 Angstroms
  observed by the SOHO/Coronal Diagnostic Spectrometer (CDS). Moreover,
  from the white light density profiles we calculate temperature profiles
  and compare to temperature diagnostic information from EUV lines and
  soft X-ray images from Yohkoh. H I Ly alpha and O VI 1032/1037 Angstrom
  intensities from the SOHO Ultraviolet Coronagraph Spectrometer (UVCS)
  are used to estimate both the direction and magnitude of plasma outflow
  velocities in coronal holes and streamers above 1.5 Ro. The velocities
  are derived using densities from white light coronagraph data and
  coronal electron temperature estimates derived from Ulysses/SWICS
  ion composition data. Near the base of the corona we find the white
  light and spectral analysis produce consistent density and temperature
  information. In the extended corona we find results consistent with
  high outflow velocities and a superradial outflow geometry in polar
  coronal holes.

Title: Coordinated Observations with SOHO, YOHKOH and VLA
Authors: Aschwanden, Markus J.; Bastian, Tim S.; Nitta, Nariaki;
   Newmark, Jeff; Thompson, Barbara J.; Harrison, Richard A.
Bibcode: 1998ASPC..155..311A
Altcode: 1998sasp.conf..311A
  No abstract at ADS

Title: Comparison of Microwave and SOHO Synoptic Maps of the Sun
    During the Whole Sun Month, 1996
Authors: Gopalswamy, N.; Thompson, B. J.; Shibasaki, K.
Bibcode: 1998ASPC..140..401G
Altcode: 1998ssp..conf..401G
  No abstract at ADS

Title: 3-Dimensional Models of Active Region Loops
Authors: Aschwanden, M. J.; Neupert, W. M.; Newmark, J.; Thompson,
   B. J.; Brosius, J. W.; Holman, G. D.; Harrison, R. A.; Bastian, T. S.;
   Nitta, N.; Hudson, H. S.; Zucker, A.
Bibcode: 1998ASPC..155..145A
Altcode: 1998sasp.conf..145A
  No abstract at ADS

Title: Filament Disparition Brusque and CME - September 25-26,
    1996 Event
Authors: van Driel-Gesztelyi, L.; Schmieder, B.; Aulanier, G.;
   Demoulin, P.; Martens, P. C. H.; Zarro, D.; Deforest, C.; Thompson,
   B.; St. Cyr, C.; Kucera, T.; Burkepile, J. T.; White, O. R.; Hanaoka,
   Y.; Nitta, N.
Bibcode: 1998ASPC..150..366V
Altcode: 1998IAUCo.167..366V; 1998npsp.conf..366V
  No abstract at ADS

Title: LASCO/EIT Observations of Coronal Mass Ejections from
    Large-Scale Filament Channels
Authors: Plunkett, S. P.; Dere, K. P.; Howard, R. A.; Michels, D. J.;
   Brueckner, G. E.; Thompson, B. J.; Delaboudiniere, J. -P.
Bibcode: 1998ASPC..150..475P
Altcode: 1998npsp.conf..475P; 1998IAUCo.167..475P
  No abstract at ADS

Title: Nonthermal Radio Signatures of Coronal Disturbances with and
    without Mass Ejections
Authors: Aurass, H.; Vourlidas, A.; Andrews, M. D.; Thompson, B. J.;
   Howard, R. H.; Mann, G.
Bibcode: 1998cee..workE..20A
Altcode:
  We show that the radio signature of nonthermal electrons can be a
  sensitive indicator of small scale energy release related to topological
  changes in coronal magneto-plasma structures. We compare two events
  using images from the Extreme-UV Imaging Telescope (EIT) and the Large
  Angle and Spectroscopic Coronagraph (LASCO) instruments, GOES soft
  X-ray data, and 40--800 MHz radio spectra of the AI Potsdam. At first
  glance, both events appear similar. One event decays after a prominence
  eruption causing only brightness changes in the EIT and C1 images. But
  the other event marks the onset of a large coronal mass ejection (CME)
  that propagates with a speed of ~530kms^{-1} between 2--30 R_odot. The
  CME formation is accompanied by an unspectacular faint group of metric
  drift bursts starting in the spectral range 170--200 MHz (at a height
  1.20-1.25 R_odot) and lasts for ~3 min. During the CME lift-off,
  the frequency drift of an associated type IV continuum translates to
  a speed of ~90kms^{-1}. The same speed is obtained from the height
  change of leading CME features in LASCO-C1. The non-CME event is
  accompanied by a non-drifting continuum and lacks any type III burst
  activity. We offer a number of explanations for the CME absence. Also,
  in the non-CME case we show that the post-prominence eruption current
  sheet can be detected in the EIT and C1 images. Its lower part appears
  as a bright blob in EIT on the top of a loop arcade. The brightness
  of this blob corresponds to a soft X-ray long duration event (LDE)
  decay. Our study suggests that prominence eruptions and soft X-ray
  LDEs are insufficient to reveal a CME.

Title: New Images of the Solar Corona
Authors: Gurman, Joseph B.; Thompson, Barbara J.; Newmark, Jeffrey A.;
   Deforest, Craig E.
Bibcode: 1998ASPC..154..329G
Altcode: 1998csss...10..329G
  In 1.5 years of operation, The Extreme Ultraviolet Imaging Telescope
  (EIT) on SOHO has obtained over 40,000 images of the Sun in four
  wavebands between 171 Angstroms and 304 Angstroms, with spatial
  resolution limited only by the pixel scale of 2.59 arcsec. These
  images, and in particular compilations of time series of images into
  digital movies, have changed several of our ideas about the corona
  at temperatures of 0.9 - 2.5 MK. For the first time, we are able to
  see outflow in polar plumes and microjets inputting momentum into the
  high-speed, polar wind flow. For the first time, in conjunction with the
  LASCO coronagraphs and ground-based He I imagers, we have been able to
  see all the structures involved in coronal mass ejections (CMEs), from
  the surface of the Sun to 30 solar radii above it. In several cases, we
  have been able to observe directly the dramatic Moreton waves emanating
  from the active region where the CMEs originate, and radiating across
  virtually the entire visible hemisphere of the Sun. We interpret these
  large-scale coronal disturbances as fast-mode waves. Such events appear
  in the SOHO-LASCO coronagraphs as earthward-directed, and several have
  been detected by solar wind monitoring experiments on SOHO and other
  spacecraft. We have been able to view a variety of small-scale phenomena
  as well, including motions in prominences and filaments, macrospicular
  and polar microjet eruptions, and fine structures in the polar crown
  filament belt. The multi-wavelength capability of EIT makes it possible
  to determine the temperature of the coronal plasma and, here, too,
  we have been afforded a novel view: the heating in coronal active
  regions occurs over a considerably larger area than the high-density
  loops structures alone (i.e., bright features) would indicate.

Title: Analysis of Active Regions via 3D Rendering Techniques
Authors: Alexander, D.; Gary, G. Allen; Thompson, B. J.
Bibcode: 1998ASPC..155..100A
Altcode: 1998sasp.conf..100A
  No abstract at ADS

Title: VLA-SOHO Observations of Evolving Coronal Structures on the Sun
Authors: Willson, R. F.; Lang, K. R.; Thompson, B.; Schuehle, U.;
   Zarro, D. M.
Bibcode: 1998ASPC..154..727W
Altcode: 1998csss...10..727W
  Very Large Array (VLA) observations at 3.5, 6.2, and 91.6 cm wavelength
  have been combined with EUV spectroheliograms from the Solar and
  Heliospheric Observatory (SOHO) Coronal Diagnostic Spectrometer (CDS)
  and Extreme Ultraviolet Telescope (EIT) to study evolving sources in the
  transition region and corona above a solar active region. In some cases,
  transient events, lasting minutes to tens of minutes, were observed
  at both radio and EUV wavelengths, while other events were detected
  in only one spectral domain. The combined data sets suggest that the
  EUV-associated microwave sources are produced by thermal gyroresonance
  or nonthermal gyrosynchrotron radiation, primarily in regions of high
  magnetic field strength near sunspots. Observations at 91.6 cm also
  show the sudden appearance of a low-lying, nonthermal source in the
  low corona around the time that cool, outwardly-propagating plasma
  was detected by the SOHO/EIT.

Title: Development of Coronal Mass Ejections and Association with
    Interplanetary Events
Authors: Pick, M.; Maia, D.; Howard, R.; Thompson, B.; Lanzerotti,
   L. J. L.; Bothmer, V.; Lamy, P.
Bibcode: 1997ESASP.415..195P
Altcode: 1997cpsh.conf..195P
  No abstract at ADS

Title: Overview of the ISTP Sun-Earth Connection Event of January
    6-11 1997
Authors: Peredo, M.; Fox, Nicola; Thompson, Barbara
Bibcode: 1997ESASP.415..517P
Altcode: 1997cpsh.conf..517P
  No abstract at ADS

Title: Solar Energetic Particle Events and Coronal Mass Ejections:
    New Insights from SOHO
Authors: Bothmer, V.; Posner, A.; Kunow, H.; Müller-Mellin, R.;
   Herber, B.; Pick, M.; Thompson, B. J.; Delaboudinière, J. -P.;
   Brueckner, G. E.; Howard, R. A.; Michels, D. J.; Cyr, C. St.; Szabo,
   A.; Hudson, H. S.; Mann, G.; Classen, H. -T.; McKenna-Lawlor, S.
Bibcode: 1997ESASP.415..207B
Altcode: 1997cpsh.conf..207B
  No abstract at ADS

Title: White-Light Coronal Mass Ejections: A New Perspective from
    LASCO
Authors: St. Cyr, O. C.; Howard, R. A.; Simnett, G. M.; Gurman, J. B.;
   Plunkett, S. P.; Sheeley, N. R.; Schwenn, R.; Koomen, M. J.; Brueckner,
   G. E.; Michels, D. J.; Andrews, M.; Biesecker, D. A.; Cook, J.; Dere,
   K. P.; Duffin, R.; Einfalt, E.; Korendyke, C. M.; Lamy, P. L.; Lewis,
   D.; Llebaria, A.; Lyons, M.; Moses, J. D.; Moulton, N. E.; Newmark,
   J.; Paswaters, S. E.; Podlipnik, B.; Rich, N.; Schenk, K. M.; Socker,
   D. G.; Stezelberger, S. T.; Tappin, S. J.; Thompson, B.; Wang, D.
Bibcode: 1997ESASP.415..103S
Altcode: 1997cpsh.conf..103S
  No abstract at ADS

Title: Magnetic Flux in Modeled Magnetic Clouds at 1 AU and Some
    Specific Comparisons to Associated Photospheric Flux
Authors: Lepping, R. P.; Szabo, A.; DeForest, C. E.; Thompson, B. J.
Bibcode: 1997ESASP.415..163L
Altcode: 1997cpsh.conf..163L
  No abstract at ADS

Title: Fitting a 3-D Analytic Model of the Coronal Mass Ejection
    to Observations
Authors: Gibson, S. E.; Biesecker, D.; Fisher, R.; Howard, R. A.;
   Thompson, B. J.
Bibcode: 1997ESASP.415..111G
Altcode: 1997cpsh.conf..111G
  No abstract at ADS

Title: The Structure and Evolution of Solar Coronal Holes Observed
    by SOHO During August and September 1996
Authors: Bromage, B. J. I.; del Zanna, G.; Fludra, A.; DeForest, C.;
   Thompson, B.
Bibcode: 1997ESASP.415..307B
Altcode: 1997cpsh.conf..307B
  No abstract at ADS

Title: Fluxes of MeV Particles at Earth's Orbit and their Relationship
with the Global Structure of the Solar Corona: Observations from SOHO
Authors: Posner, A.; Bothmer, V.; Kunow, H.; Herber, B.;
   Müller-Mellin, R.; Delaboudinière, J. -P.; Thompson, B. J.;
   Brückner, G. E.; Howard, R. A.; Muchels, D. J.
Bibcode: 1997ESASP.415..377P
Altcode: 1997cpsh.conf..377P
  No abstract at ADS

Title: Solar Active Region Movies seen by the SOHO Extreme-ultraviolet
    Telescope
Authors: Newmark, J. S.; Thompson, B.; Gurman, J. B.; Delaboudiniere,
   J. P.; Aschwanden, Markus; Mason, Helen
Bibcode: 1997AAS...191.7307N
Altcode: 1997BAAS...29.1321N
  The Extreme-ultraviolet Imaging Telescope (EIT) on board the SOHO (SOlar
  and Heliospheric Observatory) satellite provides wide-field images of
  the corona and transition region on the solar disc and up to 1.4 solar
  radii above the limb. Its normal incidence multilayer-coated optics
  select spectral emission lines from FeIX (171 Ang), FeXII (195 Ang),
  FeXV (284 Ang), and HeII (304 Ang) with 2.6 arcsecond resolution which
  allow us to describe Solar activity over a wide temperature range. EIT
  is providing unique EUV observations of the structure and evolution of
  active regions. Here we show movies of active region 8059 from July
  3-10, 1997. The high temporal variability of the AR loops is very
  evident. Initial temperature and density diagnostics are explored as
  well as a comparison with diagnostics from the SOHO-CDS instrument.

Title: Polar Plume Anatomy: Results of a Coordinated Observation
Authors: DeForest, C. E.; Hoeksema, J. T.; Gurman, J. B.; Thompson,
   B. J.; Plunkett, S. P.; Howard, R.; Harrison, R. C.; Hasslerz, D. M.
Bibcode: 1997SoPh..175..393D
Altcode:
  On 7 and 8 March 1996, the SOHO spacecraft and several other space-
  and ground-based observatories cooperated in the most comprehensive
  observation to date of solar polar plumes. Based on simultaneous
  data from five instruments, we describe the morphology of the plumes
  observed over the south pole of the Sun during the SOHO observing
  campaign. Individual plumes have been characterized from the photosphere
  to approximately 15 R⊙ yielding a coherent portrait of the features
  for more quantitative future studies. The observed plumes arise from
  small (∼ 2-5 arc sec diameter) quiescent, unipolar magnetic flux
  concentrations, on chromospheric network cell boundaries. They are
  denser and cooler than the surrounding coronal hole through which they
  extend, and are seen clearly in both Feix and Fexii emission lines,
  indicating an ionization temperature between 1.0-1.5 x 10<SUP>6</SUP>
  K. The plumes initially expand rapidly with altitude, to a diameter of
  20-30 Mm about 30 Mm off the surface. Above 1.2 R⊙ plumes are observed
  in white light (as `coronal rays') and extend to above 12 R⊙. They
  grow superradially throughout their observed height, increasing their
  subtended solid angle (relative to disk center) by a factor of ∼10
  between 1.05 R⊙ and 4-5 R⊙ and by a total factor of 20-40 between
  1.05 R⊙ and 12 R⊙. On spatial scales larger than 10 arc sec,
  plume structure in the lower corona (R &lt; 1.3 R⊙) is observed to
  be steady-state for periods of at least 24 hours; however, on spatial
  scales smaller than 10 arc sec, plume XUV intensities vary by 10-20%
  (after background subtraction) on a time scale of a few minutes.

Title: EIT Observations of the Extreme Ultraviolet Sun
Authors: Moses, D.; Clette, F.; Delaboudinière, J. -P.; Artzner,
   G. E.; Bougnet, M.; Brunaud, J.; Carabetian, C.; Gabriel, A. H.;
   Hochedez, J. F.; Millier, F.; Song, X. Y.; Au, B.; Dere, K. P.; Howard,
   R. A.; Kreplin, R.; Michels, D. J.; Defise, J. M.; Jamar, C.; Rochus,
   P.; Chauvineau, J. P.; Marioge, J. P.; Catura, R. C.; Lemen, J. R.;
   Shing, L.; Stern, R. A.; Gurman, J. B.; Neupert, W. M.; Newmark,
   J.; Thompson, B.; Maucherat, A.; Portier-Fozzani, F.; Berghmans, D.;
   Cugnon, P.; Van Dessel, E. L.; Gabryl, J. R.
Bibcode: 1997SoPh..175..571M
Altcode:
  The Extreme Ultraviolet Imaging Telescope (EIT) on board the SOHO
  spacecraft has been operational since 2 January 1996. EIT observes
  the Sun over a 45 x 45 arc min field of view in four emission line
  groups: Feix, x, Fexii, Fexv, and Heii. A post-launch determination
  of the instrument flatfield, the instrument scattering function, and
  the instrument aging were necessary for the reduction and analysis
  of the data. The observed structures and their evolution in each
  of the four EUV bandpasses are characteristic of the peak emission
  temperature of the line(s) chosen for that bandpass. Reports on the
  initial results of a variety of analysis projects demonstrate the range
  of investigations now underway: EIT provides new observations of the
  corona in the temperature range of 1 to 2 MK. Temperature studies of
  the large-scale coronal features extend previous coronagraph work
  with low-noise temperature maps. Temperatures of radial, extended,
  plume-like structures in both the polar coronal hole and in a low
  latitude decaying active region were found to be cooler than the
  surrounding material. Active region loops were investigated in detail
  and found to be isothermal for the low loops but hottest at the loop
  tops for the large loops.

Title: Association of Extreme-Ultraviolet Imaging Telescope (EIT)
    Polar Plumes with Mixed-Polarity Magnetic Network
Authors: Wang, Y. -M.; Sheeley, N. R.; Dere, K. P.; Duffin, R. T.;
   Howard, R. A.; Michels, D. J.; Moses, J. D.; Harvey, J. W.; Branston,
   D. D.; Delaboudinière, J. -P.; Artzner, G. E.; Hochedez, J. F.;
   Defise, J. M.; Catura, R. C.; Lemen, J. R.; Gurman, J. B.; Neupert,
   W. M.; Newmark, J.; Thompson, B.; Maucherat, A.; Clette, F.
Bibcode: 1997ApJ...484L..75W
Altcode:
  SOHO EIT spectroheliograms showing the polar coronal holes during the
  present sunspot minimum are compared with National Solar Observatory
  (Kitt Peak) magnetograms taken in Fe I λ8688 and Ca II λ8542. The
  chromospheric λ8542 magnetograms, obtained on a routine, near-daily
  basis since 1996 June, reveal the Sun's strong polar fields with
  remarkable clarity. We find that the Fe IX λ171 polar plumes occur
  where minority-polarity flux is in contact with flux of the dominant
  polarity inside each polar hole. Moreover, the locations of ``plume
  haze'' coincide approximately with the patterns of brightened He
  II λ304 network within the coronal hole. The observations appear
  to be consistent with mechanisms of plume formation involving
  magnetic reconnection between unipolar flux concentrations and nearby
  bipoles. The fact that minority-polarity fields constitute only a small
  fraction of the total magnetic flux within the polar holes suggests
  that plumes are not the main source of the high-speed polar wind.

Title: Tracking a CME from Cradle to Grave: A Multi-wavelength
    Analysis of the February 6-7, 1997 Event
Authors: Gopalswamy, N.; Kundu, M. R.; Hanaoka, Y.; Kosugi, T.; Hudson,
   H.; Nitta, N.; Thompson, B.; Gurman, J.; Plunkett, S.; Howard, R.;
   Burkepile, J.
Bibcode: 1997SPD....28.0501G
Altcode: 1997BAAS...29..908G
  The partially earth-directed coronal mass ejection (CME) event of 1997
  February 6-7 originated from the southwest quadrant of the sun. The
  CME accelerated from 170 km/s to about 830 km/s when it reached a
  distance of 25 solar radii. The CME was an arcade eruption followed
  by bright prominence core structures. The prominence core was tracked
  continuously from the solar surface to the interplanetary medium by
  combining data from the Nobeyama radioheliograph (microwaves), Mauna Loa
  Solar Observatory (He 10830 { Angstroms}), SOHO/EIT (EUV) and SOHO/LASCO
  (white light). The CME was accompanied by an arcade formation, fully
  observed by the YOHKOH/SXT (soft X-rays) and SOHO/EIT (EUV). The X-ray
  and EUV observations suggest that the reconnection proceeded from
  the northwest end to the southeast end of a filament channel. In the
  SOHO/EIT images, the the feet of the soft X-ray arcade were observed
  as EUV ribbons. The CME event also caused a medium sized geomagnetic
  storm: The hourly equatorial Dst values attained storm level during
  18:00-19:00 UT on February 09. This means the disturbance took about
  2.25 days to reach the Earth. The first signatures of an IP shock was
  a pressure jump in the WIND data around 13:00 UT on Feb 09, 1997 which
  lasted for about 14 hours, followed by flux rope signatures. This CME
  event confirms a number of ideas about CMEs: The three part structure
  (frontal bright arcade, dark cavity and prominence core), disappearing
  filament, elongated arcade formation, and terrestrial effects. We make
  use of the excellent data coverage from the solar surface to the Earth
  to address a number of issues regarding the origin and propagation of
  the geoeffective solar disturbances. We benefited from discussions at
  the first SOHO-Yohkoh Coordinated Data Analysis Workshop, held March
  3-7, 1997, at Goddard Space Flight Center.

Title: Fitting a 3-d analytic model of the Coronal Mass Ejection
    to observations
Authors: Gibson, Sarah; Fisher, Richard; Howard, Russ; Thompson,
   Barbara
Bibcode: 1997SPD....28.0110G
Altcode: 1997BAAS...29..880G
  We present the application of an analytic magnetohydrodynamic model
  (Gibson and Low, 1997) to observations of the time-dependent expulsion
  of three-dimensional Coronal Mass Ejections (CMEs) out of the solar
  corona. The model relates the white-light appearance of the CME to
  its internal magnetic field, which takes the form of a closed bubble,
  filled with a partly anchored, twisted magnetic flux rope and embedded
  in an otherwise open background field. The density distribution frozen
  into the expanding CME magnetic field is fully three-dimensional, and
  can be integrated along the line of sight to reproduce observations of
  scattered white light. The model is able to reproduce the conspicuous
  three features often associated with CMEs as observed with white-light
  coronagraphs: a surrounding high-density region, an internal low-density
  cavity, and a high-density core. By varying the model parameters,
  including the location and orientation of the CME magnetic axis relative
  to the limb, we are able to fit the model directly to examples of CMEs
  observed by the HAO/SMM Coronagraph, the HAO/Mark III K-Coronameter,
  and also to an event observed both by the SOHO/LASCO coronagraphs and
  the SOHO/EIT EUV coronal imager.

Title: SOHO/EIT and SOHO/LASCO Observations of the April 1 1997 Event:
    Coronal Observations of a Moreton Wave
Authors: Thompson, B. J.; Newmark, J. S.; Gurman, J. B.; St. Cyr,
   O. C.; Stezelberger, S.
Bibcode: 1997SPD....28.0130T
Altcode: 1997BAAS...29..884T
  The SOHO Extreme ultraviolet Imaging Telescope (EIT) recorded a series
  of events on April 1, 1997 with a 12-minute cadence of 195 Angstrom
  (Fe XII) images. A Moreton wave was observed emanating from a flaring
  active region beginning at 13:56 UT 1-April-1997. The wave travelled
  at initial speeds of approximately 300 km/sec, spreading across the
  solar disk radially from the flare. The CME observed by SOHO/LASCO was
  observable at both the east and west limbs in the C2 (2-6 solar radii)
  and C3 (3.7-30 solar radii) coronagraphs. The event was the site of
  strong emerging flux, and a number of explosive jet-like surges were
  observed at the east edge of the region prior to, throughout, and
  following the event. The discussion will include topology, comparison
  to Moreton wave/MHD theory predictions, and solar wind signatures.

Title: Observations of the January 6, 1997 CME/Magnetic Cloud Event
Authors: Thompson, B. J.
Bibcode: 1997SPD....28.0302T
Altcode: 1997BAAS...29..907T
  Despite the unprecedented degree of scientific coverage, the solar
  origin of the January 6, 1997 CME/Magnetic Cloud Event is not completely
  understood. The eruption was associated with a small disappearing
  filament and long duration event (LDE) but was accompanied by no
  significant CME signatures in soft x-ray and radio data. SOHO/LASCO
  images of the event showed a faint CME encompassing 3/4 of the solar
  disk. This event is of interest for (at least) three reasons: the
  event had a significant impact on geospace, causing activity which
  was detectable throughout the entire magnetosphere. Secondly, it
  adds another event to the list of eruptions which are surprisingly
  subtle in the solar data but are extremely geoeffective. Finally,
  the event was observed with historic completeness: from its origin
  (coronagraph/solar disk imagers), propagation (WIND/WAVES radio
  tracking), magnetospheric impact, and subsequent geomagnetic
  activity. The presentation will include a discussion of the current
  progress towards the understanding of these events and a summary of
  the solar, solar wind, and magnetospheric observations.

Title: Observations of Coronal Features by EIT above an Active Region
    by EIT and Implications for Coronal Heating
Authors: Neupert, W. M.; Newmark, J.; Thompson, B. J.; Catura, R.;
   Moses, J. D.; Portier-Fozzani, F.; Delaboudiniere, J. P.; Gabriel, A.;
   Artzner, G.; Clette, F.; Cugnon, P.; Maucherat, A.; Defise, J. M.;
   Jamar, C.; Rochus, P.; Howard, R.; Michels, D.; Dere, K.; Freeland,
   S.; Lemen, J.; Stern, R.; Gurman, J.
Bibcode: 1997SPD....28.0115N
Altcode: 1997BAAS...29..881N
  The EUV Imaging Telescope (EIT) on the SOHO provides the capability
  for multi-wavelength imaging of the corona in four spectral bands,
  centered at 171, 195, 284, and 304 Angstroms, using multilayer telescope
  technology. These bands encompass coronal temperatures from 1 MK
  to 2.5 MK as well as the upper chromosphere, at about 60,000 K. In
  particular, nearly simultaneous imaging in the 171 and 195 Angstrom
  bands, the former including major Fe IX and Fe X emission lines, the
  latter including a strong Fe XII line, provides a capability to infer
  the morphology and characteristics of the corona at temperatures of
  1.0 - 1.7 MK. We have examined the corona in this temperature range
  over an active region observed from SOHO from May - September, 1996 and
  find that low-lying loops (below a density scale height of 75,000 km,
  characteristic of Fe X) vary little in brightness and temperature along
  their length. For features extending to greater heights, however, both
  brightness gradients and temperature gradients are observed. Preliminary
  analysis of the observations when the region was on the West limb
  on September 30 indicates a small positive temperature gradient of
  approximately 0.5 K/km in one loop system that extended above 100,000
  km. On the other hand, a nearly radial feature extending to the edge of
  the EIT FOV was isothermal or had at most a slight negative temperature
  gradient. Such measurements may have application to the modeling of
  coronal loops and streamers and the processes of coronal heating and
  solar wind acceleration.

Title: The Solar Minimum X2. 6/1B Flare and CME of 9 July 1996;
Part 1: Solar Data
Authors: Andrews, M. D.; Dryer, M.; Aurass, H.; DeForest, C.;
   Kiplinger, A. L.; Meisner, R.; Paswaters, S. E.; Smith, Z.; Tappipn,
   S. J.; Thompson, B. J.; Watari, S. I.; Lamy, P.; Mann, G.; Schwenn,
   R.; Michels, D. J.; Brueckner, G. E.; Howard, R. A.; Koomen, M.
Bibcode: 1997ESASP.404..169A
Altcode: 1997cswn.conf..169A
  No abstract at ADS

Title: A Multi-Wavelength Analysis of the February 6/7, 1997 Coronal
    Mass Ejection
Authors: Plunkett, S. P.; Gopalswamy, N.; Kundu, M. R.; Howard, R. A.;
   Thompson, B. J.; Gurman, J. B.; Lepping, R. P.; Hudson, H. S.; Nitta,
   N.; Hansoka, Y.; Kosugi, T.; Burkepile, J. T.
Bibcode: 1997ESASP.404..615P
Altcode: 1997cswn.conf..615P
  No abstract at ADS

Title: Solar Magnetic Field Events related to CMEs observed with SOHO
    (MDI, EIT, SUMER, LASCO)
Authors: Schmieder, B.; van Driel-Gesztelyi, L.; Wiik, J. E.; Thompson,
   B.; de Forest, C.; Saint Cyr, C.; Vial, J. -C.; Nitta, N.; Simnett, G.
Bibcode: 1997IAUJD..19E..42S
Altcode:
  We shall present two CMEs observed by LASCO during the minimum of
  activity of the Sun. These are associated with filament disparitions
  brusques (DB). CME and DB definitively seem to be consequences of global
  magnetic field instability, which causes reconnection of pre-existing
  field lines in the corona. We shall demonstrate how cancelling flux
  and converging magnetic field in photosphere may destabilize coronal
  streamers overlying one or two filament channels.

Title: First Results from SOHO on Waves Near the Solar Transition
    Region
Authors: Steffens, S.; Deubner, F. -L.; Fleck, B.; Wilhelm, K.;
   Schuhle, U.; Curdt, W.; Harrison, R.; Gurman, J.; Thompson, B. J.;
   Brekke, P.; Delaboudiniere, J. -P.; Lemaire, P.; Hessel, B.; Rutten,
   R. J.
Bibcode: 1997ASPC..118..284S
Altcode: 1997fasp.conf..284S
  We present first results from simultaneous observations with the
  CDS, EIT and SUMER instruments {please see Solar Physics 162 (1995)
  for a description of the instruments} onboard SOHO and the VTT at
  Tenerife. Our aim is to study the wave propagation, shock formation,
  and transmission properties of the upper chromosphere and transition
  region. The preliminary results presented here include the variation
  of velocity power spectra with height, difference in power between
  internetwork and network regions, and variations in mean flows displayed
  by different spectral lines.

Title: SOHO EIT Carrington Maps from Synoptic Full-Disk Data
Authors: Thompson, B. J.; Newmark, J. S.; Gurman, J. B.;
   Delaboudiniere, J. P.; Clette, F.; Gibson, S. E
Bibcode: 1997ESASP.404..779T
Altcode: 1997cswn.conf..779T
  No abstract at ADS

Title: The Solar Minimum X2. 6/1B Flare and CME of 9 July 1996;
Part 2: Propagation
Authors: Dryer, M.; Andrews, M. D.; Aurass, H.; DeForest, C.; Karlicky,
   M.; Kiplinger, A.; Klassen, A.; Meisner, R.; Ipavich, F. M.; Galvin,
   A. B.; Paswaters, S. E.; Smith, Z.; Tappin, S. J.; Thompson, B. J.;
   Watari, S. -I.; Michels, D. J.; Brueckner, G. E.; Howard, R. A.;
   Koomen, M. J.; Lamy, P.; Mann, G.; Arzner, K.; Schwenn, R.
Bibcode: 1997ESASP.404..331D
Altcode: 1997cswn.conf..331D
  No abstract at ADS

Title: Prominence Activity Related to CME Observed by SOHO, YOHKOH
    and Ground-Based Observatories
Authors: Schmieder, B.; van Driel-Gesztelyi, L.; Wiik, J. E.; Kucera,
   T.; Thompson, B.; de Forest, C.; Saint Cyr, C.; Simnett, G. M.
Bibcode: 1997ESASP.404..663S
Altcode: 1997cswn.conf..663S
  No abstract at ADS

Title: Scientists track solar event all the way to Earth
Authors: Peredo, M.; Fox, N.; Thompson, B.
Bibcode: 1997EOSTr..78..477P
Altcode:
  For the first time ever, the satellites of the International
  Solar-Terrestrial Physics (ISTP) “Observatory” have tracked a solar
  eruption all the way from the Sun to the Earth. The resulting coronal
  mass ejection (CME) traveled 4 days through interplanetary space before
  arriving at Earth, where it caused violent disturbances of the magnetic
  environment and spectacular auroral displays. The initial expulsion
  occurred on the Sun on January 6, 1997, and the resulting magnetic
  cloud hit the Earth on January 10.The Sun often erupts. It flings out
  whitehot ionized gas (actually hotter than whitehot, to where it glows
  in X rays) with explosive violence. Only occasionally is this gas
  aimed at Earth, however, and it is even more unusual for scientists
  to be watching the potentially disruptive mass ejection (as they were
  in January) just as it leaves the Sun. This made it possible to alert
  other scientific teams of possible activity they might observe 2 to 3
  days later. It normally takes that long for such ejecta to travel the
  150-million-km void from Sun to Earth. Thus while this is not the first,
  or the largest, event to be detected, the ISTP Observatory comprises
  a complement of spacecraft and ground-based missions that allows study
  of this “space storm” on a scale never accomplished before.

Title: A Search for the Coronal Origins of Fast Solar Wind Streams
    During the Whole Sun Month Period
Authors: Lazarus, A. J.; Steinberg, J. T.; Biesecker, D. A.; Forsyth,
   R. J.; Galvin, A. B.; Ipavich, F. M.; Gibson, S. E.; Lecinski, A.;
   Hassler, D. M.; Hoeksema, J. T.; Riley, P.; Strachan, L., Jr.; Szabo,
   A.; Lepping, R. P.; Ogilvie, K. W.; Thompson, B. J.
Bibcode: 1997ESASP.404..511L
Altcode: 1997cswn.conf..511L
  No abstract at ADS

Title: Modeling a Simple Coronal Streamer during Whole Sun Month
Authors: Gibson, S. E.; Bagenal, F.; Biesecker, D.; Guhathakurta,
   M.; Hoeksema, J. T.; Thompson, B. J.
Bibcode: 1997ESASP.404..407G
Altcode: 1997cswn.conf..407G
  No abstract at ADS

Title: Microwave and UV observations of filaments with SOHO and
    the VLA
Authors: Alissandrakis, C. E.; Drago, F.; Bastian, T.; Bocchialini,
   K.; Delaboudiniere, J. -P.; Lemaire, P.; Vial, J. -C.; Harrison,
   R. A.; Thompson, B.
Bibcode: 1997ASPC..118..289A
Altcode: 1997fasp.conf..289A
  Observations performed in coordination between SOHO instruments and
  ground-based observatories offer the unique possibility to derive
  information simultaneously in several wavelengths formed at different
  altitudes and/or temperatures in the solar atmosphere. The SUMER and
  CDS spectrometers, the imaging telescope EIT aboard SOHO, and the VLA
  provide complementary information in the UV and the radio ranges. We
  illustrate such a coordination with observations of filaments in the
  transition region, performed in July 1996. The observations in the UV
  between 10(4) and 10(6) K provide the differential emission measure
  as a function of temperature; this can be used to compute the expected
  brightness temperature in the microwave range and check models of the
  filament-corona transition region.

Title: An Equatorial Coronal Hole at Solar Minimum
Authors: Bromage, B. J. I.; Del Zanna, G.; DeForest, C.; Thompson,
   B.; Clegg, J. R.
Bibcode: 1997ESASP.404..241B
Altcode: 1997cswn.conf..241B
  No abstract at ADS

Title: Electron acceleration by inertial Alfvén waves
Authors: Thompson, B. J.; Lysak, R. L.
Bibcode: 1996JGR...101.5359T
Altcode:
  Alfvén waves reflected by the ionosphere and by inhomogeneities in
  the Alfvén speed can develop an oscillating parallel electric field
  when electron inertial effects are included. These waves, which have
  wavelengths of the order of an Earth radius, can develop a coherent
  structure spanning distances of several Earth radii along geomagnetic
  field lines. This system has characteristic frequencies in the range of
  1 Hz and can exhibit electric fields capable of accelerating electrons
  to several keV. These electric fields have the potential to accelerate
  electrons in several senses: via Landau resonance, bounce or transit
  time resonance as discussed by André and Eliasson [1992] or through
  the effective potential drop which appears when the transit time
  of the electrons is much smaller than the wave period, so that the
  electric fields appear effectively static. A time-dependent model of
  wave propagation is developed which represents inertial Alfvén wave
  propagation along auroral field lines. The disturbance is modeled as it
  travels earthward, experiences partial reflections in regions of rapid
  variation, and finally reflects off a conducting ionosphere to continue
  propagating antiearthward. The wave experiences partial trapping
  by the ionospheric Alfvén resonator, which is the effective cavity
  formed between the ionosphere and the Alfvén speed peak discussed
  earlier by Polyakov and Rapoport [1981] and Trakhtengerts and Feldstein
  [1981, 1984, 1991] and later by Lysak [1991, 1993]. Results of the wave
  simulation and an accompanying test particle simulation are presented,
  which indicate that inertial Alfvén waves are a possible mechanism
  for generating electron conic distributions and field-aligned particle
  precipitation. The model incorporates conservation of energy by allowing
  electrons to affect the wave via Landau damping, which appears to
  enhance the effect of the interactions which heat electron populations.

Title: Some dynamical aspects of a quiescent filament
Authors: Schmieder, B.; Demoulin, P.; Poland, A.; Thompson, B.
Bibcode: 1988A&A...197..281S
Altcode:
  A typical quiescent filament was observed on the disk in the Hα
  and C IV lines during a period of approximately one hour. Vertical
  velocities (&lt;2.5 km s<SUP>-1</SUP>) with a time scale of 5 min and
  a spatial scale of a few tens of seconds of arc were detected in Hα,
  and associated with microturbulence in both lines. The C IV observations
  correlated well with those in Hα, and showed no indication of material
  heating from Hα to C IV temperatures. Two mechanisms to explain these
  observations are proposed: mass motion along twisted magnetic field
  or instabilities triggering waves along the filament.

Title: James Harland Duthie died 13 October 1986.
Authors: Thompson, B.
Bibcode: 1987SouSt..32..102T
Altcode:
  No abstract at ADS

Title: Applied optics and optical engineering. Vol._VI.
Authors: Kingslake, R.; Thompson, B. J.
Bibcode: 1980aooe.book.....K
Altcode:
  No abstract at ADS

Title: REVIEW: Applications of holography
Authors: Thompson, B. J.
Bibcode: 1978RPPh...41..633T
Altcode:
  The current status of holography and its applications are discussed
  with some historical background to place the current activity in
  perspective. Basic types of holograms are described together with
  their properties. Applications in optical image formation include
  photography, microscopy, image storage and image replication. Acoustic,
  X-ray, electron beam and microwave holography are briefly commented
  upon. The second major area of application is contour generation and
  interferometry. Finally, the current status of holographic optical
  elements is assessed.

Title: Recovery of Images from Atmospherically Degraded Short-Exposure
    Photographs
Authors: Knox, K. T.; Thompson, B. J.
Bibcode: 1974ApJ...193L..45K
Altcode:
  The possibility is shown that the phase of an object transform can
  be determined from the autocorrelation of the image transform. The
  two together should give a diffraction-limited image of the object. A
  thereon based technique for the recovery of images from atmospherically
  degraded short-exposure photographs is proposed. Results from a
  one-dimensional computer simulation are used for a preliminary
  demonstration of the technique.

Title: Space optics. Proceedings of the 9th International Congress
    of the International Commission for Optics.
Authors: Thompson, B. J.; Shannon, R. R.
Bibcode: 1974sop..book.....T
Altcode:
  No abstract at ADS

Title: Space optics
Authors: Thompson, B. J.; Shannon, R. R.
Bibcode: 1974spop.conf.....T
Altcode:
  No abstract at ADS

Title: Removal of turbulence from short-time-exposure photographs
    of star images.
Authors: Knox, K. T.; Thompson, B. J.
Bibcode: 1973JOSA...63.1326K
Altcode:
  No abstract at ADS

Title: Fraunhofer Holography for Bubble Chamber Photography
Authors: Thompson, B. J.; Ward, J. H.
Bibcode: 1967moop.conf..649T
Altcode:
  No abstract at ADS

