Author name code: kohl
ADS astronomy entries on 2022-09-14
author:"Kohl, John L." 
------------------------------------------------------------------------  

Title: Global helium abundance measurements in the solar corona
Authors: Moses, John D.; Antonucci, Ester; Newmark, Jeffrey; Auchère,
   Frédéric; Fineschi, Silvano; Romoli, Marco; Telloni, Daniele;
   Massone, Giuseppe; Zangrilli, Luca; Focardi, Mauro; Landini, Federico;
   Pancrazzi, Maurizio; Rossi, Guglielmo; Malvezzi, Andrea M.; Wang,
   Dennis; Leclec'h, Jean-Christophe; Moalic, Jean-Pierre; Rouesnel,
   Frédéric; Abbo, Lucia; Canou, Aurélien; Barbey, Nicolas; Guennou,
   Chloé; Laming, John M.; Lemen, James; Wuelser, Jean-Pierre; Kohl,
   John L.; Gardner, Lawrence D.
Bibcode: 2020NatAs...4.1134M
Altcode: 2020NatAs.tmp..152M
  Solar abundances have been historically assumed to be representative
  of cosmic abundances. However, our knowledge of the solar abundance
  of helium, the second most abundant element, relies mainly on
  models<SUP>1</SUP> and indirect measurements through helioseismic
  observations<SUP>2</SUP>, because actual measurements of helium in the
  solar atmosphere are very scarce. Helium cannot be directly measured
  in the photosphere because of its high first ionization potential,
  and measurements of its abundance in the inner corona have been
  sporadic<SUP>3,4</SUP>. In this Letter, we present simultaneous global
  images of the helium (out to a heliocentric distance of 3R<SUB>⊙</SUB>
  (solar radii)) and hydrogen emission in the solar corona during
  the minimum of solar activity of cycle 23 and directly derive the
  helium abundance in the streamer region and surrounding corona
  (out to 2.2R<SUB>⊙</SUB>). The morphology of the He<SUP>+</SUP>
  corona is markedly different from that of the H corona, owing to
  significant spatial variations in helium abundance. The observations
  show that the helium abundance is shaped according to and modulated
  by the structure of the large-scale coronal magnetic field and that
  helium is almost completely depleted in the equatorial regions during
  the quiet Sun. This measurement provides a trace back to the coronal
  source of the anomalously slow solar wind observed in the heliosphere
  at the Sun-Earth Lagrangian point L1 in 2009, during the exceptionally
  long-lasting minimum of solar activity cycle 23.

Title: The Evolution of Plasma Parameters on a Coronal Source Surface
    at 2.3 R <SUB>⊙</SUB> during Solar Minimum
Authors: Strachan, L.; Panasyuk, A. V.; Kohl, J. L.; Lamy, P.
Bibcode: 2012ApJ...745...51S
Altcode: 2011arXiv1111.1206S
  We analyze data from the Solar and Heliospheric Observatory to
  produce global maps of coronal outflow velocities and densities
  in the regions where the solar wind is undergoing acceleration. The
  maps use UV and white light coronal data obtained from the Ultraviolet
  Coronagraph Spectrometer and the Large Angle Spectroscopic Coronagraph,
  respectively, and a Doppler dimming analysis to determine the mean
  outflow velocities. The outflow velocities are defined on a sphere at
  2.3 R <SUB>⊙</SUB> from Sun-center and are organized by Carrington
  Rotations during the solar minimum period at the start of solar cycle
  23. We use the outflow velocity and density maps to show that while the
  solar minimum corona is relatively stable during its early stages, the
  shrinkage of the north polar hole in the later stages leads to changes
  in both the global areal expansion of the coronal hole and the derived
  internal flux tube expansion factors of the solar wind. The polar hole
  areal expansion factor and the flux tube expansion factors (between
  the coronal base and 2.3 R <SUB>⊙</SUB>) start out as super-radial
  but then they become more nearly radial as the corona progresses away
  from solar minimum. The results also support the idea that the largest
  flux tube expansion factors are located near the coronal hole/streamer
  interface, at least during the deepest part of the solar minimum period.

Title: UVCS/SOHO Search for Coronal Suprathermal Seed Particles:
    2011 Campaign
Authors: Kohl, J. L.; Panasyuk, A. V.; Cranmer, S. R.; Raymond, J. C.;
   Rosati, R. E.
Bibcode: 2011AGUFMSH33D..05K
Altcode:
  The Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and
  Heliospheric Observatory is being used to measure precise coronal
  H I Ly-alpha spectral line profiles out to several Doppler half
  widths. Such observations can be used to reveal the proton velocity
  distribution along the line-of-sight. Departures from a Maxwellian
  distribution are believed to be needed for the acceleration of solar
  energetic particles (SEPs) by coronal mass ejection (CME) shocks. It is
  generally believed that the seed particle population needed to produce
  the numbers of SEPs observed in large events would have 0.001 to 0.01
  of the particles with speeds that exceed 1000 km/s. Assuming a kappa
  distribution that is symmetric in the tangential plane and Maxwellian
  in the radial direction, this would correspond to a distribution
  with kappa = 3.5 or smaller. We have shown that UVCS observations can
  distinguish a Gaussian from a kappa exponent of 4 or less. Previously
  reported observations near solar minimum have not yielded any such
  distributions, but the sampling of the corona was not very systematic. A
  new observational campaign was begun on 28 April 2011. Observations
  are all at a heliographic height of 2.7 solar radii from Sun-center
  and at a solar position angle of 290 degrees. Observations are made
  on a continuous basis except during SOHO Keyhole periods when UVCS
  observations are not possible, and at a few other times. Results of this
  campaign and some earlier observations will be reported. This work is
  supported by the National Aeronautics and Space Administration (NASA)
  under Grant NNX11AM46G to the Smithsonian Astrophysical Observatory.

Title: Comparison of Velocity, Density, Temperature, and Mass Flux
    Results with Solar Coronal Models
Authors: Strachan, L.; Cranmer, S. R.; Panasyuk, A.; Kohl, J. L.;
   Lamy, P. L.
Bibcode: 2011AGUFMSH53C..07S
Altcode:
  We have recently computed a series of global maps of plasma parameters
  in the extended corona using data from the Solar and Heliospheric
  Observatory (SOHO). The synoptic maps of velocity, density, temperature,
  and mass flux were derived from UV and white light coronal data
  obtained from the Ultraviolet Coronagraph Spectrometer (UVCS) and
  the Large Angle Spectroscopic Coronagraph (LASCO). The parameters
  are defined on a sphere at 2.3~ R<SUB>⊙</SUB> from Sun-center and
  are organized by Carrington Rotations during the 1996 -- 1998 solar
  minimum for Solar Cycle 23. The data imply that there are large flux
  tube expansion factors near the coronal hole/streamer boundaries,
  but these factors change significantly as the corona evolves from
  minimum to the rising phase. We compare these data to an independently
  developed theoretical model that includes damping and acceleration
  by Alfven waves in the corona (see Cranmer et al. 2007, ApJS, 171,
  520). The data set will be extended in the future and it will be used
  for constraining other theoretical models of the corona and solar wind.

Title: The Coronal Physics Investigator (cpi) Experiment For Iss:
    A New Vision For Understanding Solar Wind Acceleration
Authors: Raymond, John C.; Janzen, P. H.; Kohl, J. L.; Reisenfeld,
   D. B.; Chandran, B. D. G.; Cranmer, S. R.; Forbes, T. G.; Isenberg,
   P. A.; Panasyuk, A. V.; van Ballegooijen, A. A.
Bibcode: 2011SPD....42.2406R
Altcode: 2011BAAS..43S.2406R
  We propose an Explorer Mission of Opportunity program to develop and
  operate a large-aperture ultraviolet coronagraph spectrometer called
  the Coronal Physics Investigator (CPI) as an attached International
  Space Station (ISS) payload. The primary goal of this program is
  to identify and characterize the physical processes that heat and
  accelerate the primary and secondary components of the fast and slow
  solar wind. Also, CPI can make key measurements needed to understand
  CMEs. CPI is dedicated to high spectral resolution measurements of
  the off-limb extended corona with far better stray light suppression
  than can be achieved by a conventional instrument. UVCS/SOHO allowed
  us to identify what additional measurements need to be made to answer
  the fundamental questions about how solar wind streams are produced,
  and CPI's next-generation capabilities were designed specifically to
  make those measurements. Compared to previous instruments, CPI provides
  unprecedented sensitivity, a wavelength range extending from 25.7 to
  126 nm, higher temporal resolution, and the capability to measure line
  profiles of He II, N V, Ne VII, Ne VIII, Si VIII, S IX, Ar VIII, Ca IX,
  and Fe X, never before seen in coronal holes above 1.3 solar radii. CPI
  will constrain the properties and effects of coronal MHD waves by (1)
  observing many ions over a large range of charge and mass,(2) providing
  simultaneous measurements of proton and electron temperatures to probe
  turbulent dissipation mechanisms, and (3) measuring amplitudes of
  low-frequency compressive fluctuations. CPI is an internally occulted
  ultraviolet coronagraph that provides the required high sensitivity
  without the need for a deployable boom, and with all technically mature
  hardware including an ICCD detector. A highly experienced Explorer and
  ISS contractor, L-3 Com Integrated Optical Systems and Com Systems East
  will provide the tracking and pointing system as well as the instrument,
  and the integration to the ISS.

Title: The Coronal Physics Investigator (CPI) Experiment for ISS:
    A New Vision for Understanding Solar Wind Acceleration
Authors: Kohl, J. L.; Cranmer, S. R.; Raymond, J. C.; Norton, T. J.;
   Cucchiaro, P. J.; Reisenfeld, D. B.; Janzen, P. H.; Chandran, B. D. G.;
   Forbes, T. G.; Isenberg, P. A.; Panasyuk, A. V.; van Ballegooijen,
   A. A.
Bibcode: 2011arXiv1104.3817K
Altcode:
  In February 2011 we proposed a NASA Explorer Mission of Opportunity
  program to develop and operate a large-aperture ultraviolet
  coronagraph spectrometer called the Coronal Physics Investigator
  (CPI) as an attached International Space Station (ISS) payload. The
  primary goal of this program is to identify and characterize the
  physical processes that heat and accelerate the primary and secondary
  components of the fast and slow solar wind. In addition, CPI can make
  key measurements needed to understand CMEs. UVCS/SOHO allowed us to
  identify what additional measurements need to be made to answer the
  fundamental questions about how solar wind streams are produced, and
  CPI's next-generation capabilities were designed specifically to make
  those measurements. Compared to previous instruments, CPI provides
  unprecedented sensitivity, a wavelength range extending from 25.7 to
  126 nm, higher temporal resolution, and the capability to measure line
  profiles of He II, N V, Ne VII, Ne VIII, Si VIII, S IX, Ar VIII, Ca IX,
  and Fe X, never before seen in coronal holes above 1.3 solar radii. CPI
  will constrain the properties and effects of coronal MHD waves by
  (1) observing many ions over a large range of charge and mass, (2)
  providing simultaneous measurements of proton and electron temperatures
  to probe turbulent dissipation mechanisms, and (3) measuring amplitudes
  of low-frequency compressive fluctuations. CPI is an internally occulted
  ultraviolet coronagraph that provides the required high sensitivity
  without the need for a deployable boom, and with all technically mature
  hardware including an ICCD detector. A highly experienced Explorer and
  ISS contractor, L-3 Com Integrated Optical Systems and Com Systems East,
  will provide the tracking and pointing system as well as the instrument,
  and the integration to the ISS.

Title: Testing Coronal and Solar Wind MHD Models with UV Spectroscopic
    and Visible Light Coronagraph Data
Authors: Strachan, L.; Panasyuk, A.; Kohl, J. L.; Woolsey, L.; Lamy,
   P. L.
Bibcode: 2010AGUFMSH42A..08S
Altcode:
  We present synoptic maps of coronal outflow velocities obtained at 2.3
  Rs in the solar wind acceleration region of the corona during Solar
  Cycle 23. The outflow velocities are obtained by using data from the
  SOHO coronagraphs: H I Lyman alpha and O VI line profiles (from UVCS)
  and white light polarized brightness data (from LASCO). The information
  contained in the maps provide constraints on the electron densities,
  bulk outflow speeds, and anisotropic kinetic temperatures (velocity
  distributions for protons and minor ions. We show some examples of how
  these data can be used to test MHD models of the solar corona and solar
  wind. The data set can be used to compare empirically derived plasma
  parameters directly with the MHD model parameters or alternatively it
  can be used to compare the observed profiles with synthetic profiles
  obtained by forward modeling of the MHD data.

Title: Ultraviolet Coronagraph Spectroscopy: A Key Capability for
    Understanding the Physics of Solar Wind Acceleration
Authors: Cranmer, S. R.; Kohl, J. L.; Alexander, D.; Bhattacharjee,
   A.; Breech, B. A.; Brickhouse, N. S.; Chandran, B. D. G.; Dupree,
   A. K.; Esser, R.; Gary, S. P.; Hollweg, J. V.; Isenberg, P. A.; Kahler,
   S. W.; Ko, Y. -K.; Laming, J. M.; Landi, E.; Matthaeus, W. H.; Murphy,
   N. A.; Oughton, S.; Raymond, J. C.; Reisenfeld, D. B.; Suess, S. T.;
   van Ballegooijen, A. A.; Wood, B. E.
Bibcode: 2010arXiv1011.2469C
Altcode:
  Understanding the physical processes responsible for accelerating the
  solar wind requires detailed measurements of the collisionless plasma
  in the extended solar corona. Some key clues about these processes
  have come from instruments that combine the power of an ultraviolet
  (UV) spectrometer with an occulted telescope. This combination enables
  measurements of ion emission lines far from the bright solar disk,
  where most of the solar wind acceleration occurs. Although the UVCS
  instrument on SOHO made several key discoveries, many questions remain
  unanswered because its capabilities were limited. This white paper
  summarizes these past achievements and also describes what can be
  accomplished with next-generation instrumentation of this kind.

Title: Time Evolution of a Coronal Velocity Source Surface during
    Solar Cycle 23
Authors: Strachan, L.; Panasyuk, A. V.; Kohl, J. L.
Bibcode: 2010ASPC..428..187S
Altcode:
  We present preliminary results of a study to create coronal outflow
  velocity maps for the period from 1996 to 2005. The velocities are
  derived from the UVCS/SOHO synoptic observations of the O VI 103.2 nm
  and 103.7 nm intensities. The maps are made at a constant heliocentric
  height of 2.3 R<SUB>sun</SUB>, near the traditional coronal source
  surface height of 2.5 R<SUB>sun</SUB>. Our results for the Cycle
  22/23 minimum show that the classic solar minimum conditions, where
  high-speed wind dominates the polar regions, lasted only until May
  1997. However, during the same time period there was very little change
  in the fraction of fast or slow speed wind at low heliographic latitudes
  (&lt; 30°). When completed, the coronal velocity maps will be used to
  show the connections between structures in the corona and solar wind
  streams at greater distances from the Sun. It will also help clarify
  how variations in the spatial distribution of outflow velocities are
  controlled by the coronal magnetic field and plasma conditions at the
  source regions.

Title: SOHO-23: Understanding a Peculiar Solar Minimum
Authors: Cranmer, S. R.; Hoeksema, J. T.; Kohl, J. L.
Bibcode: 2010ASPC..428.....C
Altcode:
  No abstract at ADS

Title: Extended Coronal Heating and Solar Wind Acceleration over
    the Solar Cycle
Authors: Cranmer, S. R.; Kohl, J. L.; Miralles, M. P.; van
   Ballegooijen, A. A.
Bibcode: 2010ASPC..428..209C
Altcode: 2010arXiv1002.0297C
  This paper reviews our growing understanding of the physics behind
  coronal heating (in open-field regions) and the acceleration of the
  solar wind. Many new insights have come from the last solar cycle's
  worth of observations and theoretical work. Measurements of the
  plasma properties in the extended corona, where the primary solar wind
  acceleration occurs, have been key to discriminating between competing
  theories. We describe how UVCS/SOHO measurements of coronal holes and
  streamers over the last 14 years have provided clues about the detailed
  kinetic processes that energize both fast and slow wind regions. We also
  present a brief survey of current ideas involving the coronal source
  regions of fast and slow wind streams, and how these change over the
  solar cycle. These source regions are discussed in the context of recent
  theoretical models (based on Alfvén waves and MHD turbulence) that have
  begun to successfully predict both the heating and acceleration in fast
  and slow wind regions with essentially no free parameters. Some new
  results regarding these models—including a quantitative prediction
  of the lower density and temperature at 1 AU seen during the present
  solar minimum in comparison to the prior minimum—are also shown.

Title: Variations in the Absolute Ultraviolet Intensities of Polar
    Coronal Holes
Authors: Gardner, L. D.; Kohl, J. L.; Cranmer, S. R.; Lin, M.;
   Panasyuk, A. V.; Uzzo, M.
Bibcode: 2010ASPC..428..191G
Altcode:
  The well-maintained UVCS/SOHO radiometric calibration is used
  to determine the variations in the ultraviolet intensities in
  polar coronal holes between the Solar Cycle 22/23 and Cycle 23/24
  minima. The radiometric calibration has been carefully monitored
  and updated during the mission by observing an ensemble of B stars,
  which, as a group, are believed to have a stable mean irradiance. These
  observations, along with data from the freshly calibrated Ultraviolet
  Coronal Spectrometer on the Spartan 201 satellite in 1998, have been
  used to determine the changes in the calibration. The Spartan 201
  inter-calibration, together with the original laboratory calibration,
  was used to establish the in-flight absolute radiometric calibration
  scale. This paper summarizes the in-flight radiometric calibration of
  UVCS/SOHO and observed variations in polar coronal hole intensities
  as a function of heliographic height above the poles of the Sun.

Title: A Model for the Stray-Light Contamination of the UVCS
    Instrument on SOHO
Authors: Cranmer, S. R.; Gardner, L. D.; Kohl, J. L.
Bibcode: 2010SoPh..263..275C
Altcode: 2010arXiv1001.3843C; 2010SoPh..tmp...31C
  We present a detailed model of stray-light suppression in the
  spectrometer channels of the Ultraviolet Coronagraph Spectrometer (UVCS)
  on the SOHO spacecraft. The control of diffracted and scattered stray
  light from the bright solar disk is one of the most important tasks of
  a coronagraph. We compute the fractions of light that diffract past the
  UVCS external occulter and non-specularly pass into the spectrometer
  slit. The diffracted component of the stray light depends on the
  finite aperture of the primary mirror and on its figure. The amount
  of non-specular scattering depends mainly on the micro-roughness of
  the mirror. For reasonable choices of these quantities, the modeled
  stray-light fraction agrees well with measurements of stray light
  made both in the laboratory and during the UVCS mission. The models
  were constructed for the bright H I Lyα emission line, but they are
  applicable to other spectral lines as well.

Title: Improved Constraints on the Preferential Heating and
    Acceleration of Oxygen Ions in the Extended Solar Corona
Authors: Cranmer, Steven R.; Panasyuk, Alexander V.; Kohl, John L.
Bibcode: 2008ApJ...678.1480C
Altcode: 2008arXiv0802.0144C
  We present a detailed analysis of oxygen ion velocity distributions
  in the extended solar corona, based on observations made with
  the Ultraviolet Coronagraph Spectrometer (UVCS) on the SOHO
  spacecraft. Polar coronal holes exhibit broad line widths and unusual
  intensity ratios of the O VI λλ1032, 1037 emission-line doublet. A
  traditional interpretation of these features is that oxygen ions have
  a strong temperature anisotropy, with the temperature perpendicular
  to the magnetic field being much larger than the temperature parallel
  to the field. However, recent work by Raouafi and Solanki suggested it
  may be possible to model the observations using an isotropic velocity
  distribution. In this paper we analyze an expanded data set to show
  that the original interpretation of an anisotropic distribution is the
  only one fully consistent with the observations. It is necessary to
  search the full range of ion plasma parameters to determine the values
  with the highest probability of agreement with the UVCS data. The
  derived ion outflow speeds and perpendicular kinetic temperatures
  are consistent with earlier results, and there continues to be strong
  evidence for preferential ion heating and acceleration with respect to
  hydrogen. At heliocentric heights above 2.1 solar radii, every UVCS
  data point is more consistent with an anisotropic distribution than
  with an isotropic distribution. At heights above 3 solar radii, the
  exact probability of isotropy depends on the electron density chosen
  to simulate the line-of-sight distribution of O VI emissivity. The
  most realistic electron densities (which decrease steeply from 3 to
  6 solar radii) produce the lowest probabilities of isotropy and most
  probable temperature anisotropy ratios that exceed 10.

Title: Inclined Beams Measurements of Electron Impact Excitation at
    the Harvard-Smithsonian CfA
Authors: Gardner, Larry D.; Rosati, R. E.; Kohl, J. L.
Bibcode: 2008AAS...212.0316G
Altcode: 2008BAAS...40S.186G
  The analysis of absolute spectral line intensities and intensity
  ratios with spectroscopic diagnostic techniques provides empirical
  determinations of plasma parameters in astrophysical objects. Since
  spectral line intensities and their ratios are controlled by the
  excitation rate coefficients for the electron temperature of the
  observed astrophysical structure, it is imperative that one have
  accurate values for the relevant rate coefficients. The technique
  employed at CfA utilizes a modulated beam of a single ion species,
  which is crossed at 45 degrees with a similarly modulated electron
  beam. Photons from the decay of ions excited by collisions with
  the electrons are collected synchronously with the beams' modulation
  pattern by an absolutely calibrated optical system. We will illustrate
  our experimental approach by discussing our current measurements
  of EIE in C<SUP>2+</SUP> (2s<SUP>2</SUP> <SUP>1</SUP>S<SUB>0</SUB>
  - 2s2p <SUP>1</SUP>P<SUP>o</SUP><SUB>1</SUB>), which dominates the
  emission of CIII 97.7 nm in the Sun. Since the wavelength of the decay
  photons is below the transmission cutoff of window materials, our new
  detection system utilizes an open microchannel plate detector and a
  spherical mirror coated with Al/MgF<SUB>2</SUB>/B<SUB>4</SUB>C. These
  new components have been thoroughly calibrated at the wavelengths
  relevant to this experiment and at wavelengths relevant to forthcoming
  measurements in O<SUP>4+</SUP>. The latest research results will
  be reported. This work is supported by NASA Supporting Research and
  Technology grant NNG06GE49G in Solar and Heliospheric Physics and by
  the Smithsonian Astrophysical Observatory.

Title: Physical Properties of a Coronal Streamer at 2.5 Solar Radii
Authors: Uzzo, M.; Strachan, L.; Kohl, J.; Vourlidas, A.
Bibcode: 2008AGUSMSH51B..03U
Altcode:
  In this presentation the plasma properties of a streamer observed in
  April of 2007 at 2.5 solar radii are examined. The data comes from
  observations conducted by the Ultraviolet Coronagraph Spectrometer
  (UVCS) and the Large Angle Spectroscopic Coronagraph (LASCO) C2
  instrument aboard the Solar and Heliospheric Observatory (SOHO). From
  the UV spectral profiles the proton and oxygen kinetic temperatures can
  be derived as a function of latitude across the streamer. The observed
  line intensities are used to calculate the photospheric normalized
  absolute elemental abundances for O, S, N and Fe. The abundances
  are analyzed with respect to the FIP effect and compared to in situ
  measurements at SOHO. An estimate for the electron density is determined
  from both the UV data and the polarized white light data from LASCO C2.

Title: UVCS/SOHO Search for Coronal Suprathermal Seed Particles:
    Results for Solar Minimum
Authors: Kohl, J. L.; Panasyuk, A. V.; Cranmer, S. R.; Gardner, L. D.;
   Raymond, J. C.
Bibcode: 2008AGUSMSH41B..05K
Altcode:
  The Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and
  Heliospheric Observatory is being used to measure precise coronal H I
  Ly-alpha spectral line profiles out to several Doppler half widths. Such
  observations can be used to reveal the proton velocity distribution
  along the line-of-sight. Departures from a Maxwellian distribution are
  believed to be needed for the acceleration of solar energetic particles
  (SEPs) by coronal mass ejection (CME) shocks. We have now completed
  all required instrument characterizations and refined the observations
  to the point where it is possible to distinguish a Gaussian coronal
  velocity distribution from a power law tail of sufficient strength
  to accelerate SEPs. It is generally believed that the required seed
  particle population needed to produce SEPs of interest with a CME shock
  would have a velocity distribution with 0.001 to 0.01 of the particles
  with speeds that exceed 1000 km/s. Assuming a kappa distribution that
  is symmetric in the tangential plane and Maxwellian in the radial
  direction, this would correspond to a distribution with kappa = 3.5
  or smaller. We show that UVCS observations can distinguish a Gaussian
  from a kappa of 4 or less. This paper will report the results of
  examining observations during 2006-2008 and report on any departures
  from a Maxwellian distribution. It will also report the CME/flare
  predecessor history of each observation. This work is supported by
  the National Aeronautics and Space Administration (NASA) under Grant
  NNX07AL72G to the Smithsonian Astrophysical Observatory.

Title: Next generation UV coronagraph instrumentation for solar
    cycle-24
Authors: Kohl, John L.; Jain, Rajmal; Cranmer, Steven R.; Gardner,
   Larry D.; Pradhan, Anil K.; Raymond, John C.; Strachan, Leonard
Bibcode: 2008JApA...29..321K
Altcode:
  No abstract at ADS

Title: Investigation of the solar wind outflows and joint observations
    during the total solar eclipse of March 29, 2006
Authors: Abbo, Lucia; Zangrilli, Luca; Antonucci, Ester; Fineschi,
   Silvano; Kohl, John; Giordano, Silvio; Massone, Giuseppe; Capobianco,
   Gerardo; Calcidese, Paolo; Porcu, Francesco
Bibcode: 2008cosp...37....7A
Altcode: 2008cosp.meet....7A
  During the total solar eclipse of 29 March 2006, SOHO observations of
  JOP158 were coordinated with ground based instruments. In particular,
  the Ultraviolet Coronagraph Spectrometer (UVCS) onboard SOHO has
  observed the south coronal hole in the OVI doublet emission in order
  to probe the role of plume and interplume regions in the dynamics of
  the fast solar wind. From the analysis of the polarized K-solar corona
  measurements obtained with the EKPol polarimeter from the site of c
  (desert of Sahara, Lybia), we estimate the coronal electron density
  radial profiles and perform a Doppler dimming analysis of the OVI
  doublet line intensities to measure the outflow velocity.

Title: Assessment and Validation of MHD Models for the Solar Corona
    and Inner Heliosphere
Authors: Strachan, L.; Zurbuchen, T. H.; Kohl, J. L.; Panasyuk, A. V.;
   Raymond, J. R.; van Ballegooijen, A.
Bibcode: 2007AGUFMSH31A0238S
Altcode:
  We describe the status of a model assessment and validation project
  for testing MHD codes that simulate the solar corona and inner
  heliosphere. The goal of the project is to test MHD codes by applying
  firm empirical constraints to their boundary conditions in the corona
  and at 1 AU. The project has produced a database of coronal and solar
  wind observations from SOHO, ACE, Wind, and Ulysses. In addition to the
  database, software tools for comparing these data sets to the outputs
  for the MHD model codes under test will be demonstrated. The first
  step is to take the plasma parameters that are produced from the model
  codes and apply forward modeling to simulate the coronal observations
  of emission lines (H I Lyman alpha and O VI 103.2 nm). In situ solar
  wind data are used not only to provide benchmarks near 1 AU but also
  to provide coronal constraints for the coronal source regions of the
  solar wind. Future stages will involve making more direct comparisons
  of the plasma properties predicted from the model codes through the
  use of empirical coronal and solar wind models. We also describe a
  set of metrics that are used for making comparisons between the model
  code outputs and the empirical data. This work is supported by NASA
  under Grants NNX07AB98G to the Smithsonian Astrophysical Observatory
  and NNX07AB99G to the University of Michigan.

Title: Hydrogen Lyman Alpha Spectral Line Profiles in Coronal Holes
    from 1.5 - 6.5 Solar Radii
Authors: Suleiman, R. M.; Kohl, J. L.; Cranmer, S. R.
Bibcode: 2007AGUFMSH21A0285S
Altcode:
  UVCS has made detailed measurements of H I Lyα spectral line profiles
  in a polar coronal hole at projected heliocentric heights from 3.5
  to 6.5 R\odot during 1998 January 5 -- 11. Similar polar coronal
  hole measurements were made during 1998 June 16 -- 21. Earlier UVCS
  observations obtained at 1.5 to 2.5 R\odot are used for comparison. In
  addition, new measurements are being made for the current phase of
  the solar cycle. From these measurements we derive 1/e half widths of
  coronal velocity distributions at the observed heights. The velocity
  distribution includes all motions contributing to the Doppler shifts
  along the line of sight (LOS). We also measure absolute intensities that
  can be used to derive outflow speeds via a Doppler dimming analysis. At
  large heights in coronal holes, the outflowing coronal plasma becomes
  nearly collisionless and the ionization balance is believed to become
  frozen. H I Lyα profile measurements characterize the neutral hydrogen
  velocity distribution, which at lower heights can also be used to
  describe the proton distribution. However, in the regions above
  3~R\odot, the H0 velocity distribution may not be the same as that
  for the protons because the characteristic time for charge transfer
  between H0 and protons becomes longer than the time it takes for the
  plasma to flow through a density scale height. Hence, the H0 velocity
  distribution may not be directly affected by transverse wave motion
  or wave damping. An indication of an adiabatic radial decrease in the
  neutral hydrogen temperature would indicate a decoupling of the protons
  and neutral hydrogen, and also indicate the absence of mechanisms that
  would heat the neutrals. We will compare the observations with the
  predictions of a theoretical model of the combined electron, proton and
  neutral hydrogen plasma. Such a comparison could lead to an improved
  knowledge of the proton heating at these large heights. This work is
  supported by the National Aeronautics and Space Administration (NASA)
  under Grant NNX07AL72G to the Smithsonian Astrophysical Observatory.

Title: UVCS Empirical Constraints on Theoretical Models of Solar
    Wind Source Regions
Authors: Kohl, J. L.; Cranmer, S. R.; Miralles, M. P.; Panasyuk, A.;
   Strachan, L.
Bibcode: 2007AGUFMSH22B..02K
Altcode:
  Spectroscopic observations from the Ultraviolet Coronagraph
  Spectrometer (UVCS) on the Solar and Heliospheric Observatory
  (SOHO) have resulted in empirical models of polar coronal holes,
  polar plumes, coronal jets and streamers. These findings have
  been used to make significant progress toward identifying and
  characterizing the physical processes that produce extended heating
  in the corona and accelerate fast and slow solar wind streams. The
  UVCS scientific observations, which began in April 1996 and continue
  at this writing, have provided determinations of proton and minor ion
  temperatures (including evidence for anisotropic microscopic velocity
  distributions in coronal holes and quiescent equatorial streamers),
  outflow velocities, and elemental abundances. The variations in these
  quantities over the solar cycle also have been determined. For example,
  observations of large polar coronal holes at different phases of the
  solar cycle indicate that line width is positively correlated with
  outflow speed and anti-correlated with electron density. This paper
  will review these results, and present new results from measurements
  taken as the current solar activity cycle approaches solar minimum. The
  results regarding preferential ion heating and acceleration of heavy
  ions (i.e., O5+) in polar coronal holes have contributed in a major
  way to the advances in understanding solar wind acceleration that
  have occurred during the past decade. It is important to verify and
  confirm the key features of these findings. Hence, the results from a
  new analysis of an expanded set of UVCS data from polar coronal holes
  at solar minimum by S. R. Cranmer, A. Panasyuk and J. L. Kohl will be
  presented. This work has been supported by the National Aeronautics
  and Space Administration (NASA) under Grants NNG06G188G and NNX07AL72G
  and NNX06AG95G to the Smithsonian Astrophysical Observatory.

Title: Polar Coronal Jets During the 2007 Joint SOHO/Hinode Campaigns
Authors: Miralles, M. P.; Cranmer, S. R.; Raymond, J. C.; Kohl, J. L.
Bibcode: 2007AGUFMSH21B..02M
Altcode:
  We will present ultraviolet spectroscopy of polar coronal jets obtained
  by the Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) during the
  two SOHO/Hinode observing campaigns (9-21 January and 12-20 March,
  2007) for the north and south polar coronal holes. The emphasis is on
  identifying and tracing polar jets from the solar surface out into the
  accelerating solar wind and determining their physical properties as a
  function of height and time. UVCS/SOHO observed ultraviolet counterparts
  in the extended corona of the hot jets resolved by Hinode/XRT. These
  polar jets observed by UVCS have different characteristics in the
  acceleration region of the solar wind than the cooler jets identified
  at the last solar minimum by LASCO, UVCS, and EIT. Observations
  such as these are needed to clarify the relationship between the
  episodic jets, the longer-lived polar plumes, and the fast solar
  wind. This work is supported by NASA grants NNX06AG95G and NNX07AL72G
  to the Smithsonian Astrophysical Observatory. SOHO is a project of
  international cooperation between ESA and NASA.

Title: Measurements of Coronal Proton Velocity Distributions
Authors: Kohl, J. L.; Panasyuk, A.; Cranmer, S. R.; Gardner, L. D.;
   Raymond, J. C.
Bibcode: 2007AGUFMSH21A0298K
Altcode:
  The Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and
  Heliospheric Observatory is being used to measure precise coronal H I
  Ly-alpha spectral line profiles out to several Doppler half widths. Such
  observations can be used to reveal the proton velocity distribution
  along the line-of-sight. Departures from a Maxwellian distribution are
  believed to be needed for the acceleration of solar energetic particles
  (SEPs) by coronal mass ejection (CME) shocks. Our initial attempt to
  measure suprathermal proton velocity distributions has been described
  by Kohl et al. (2006). We have made considerable additional progress
  on such measurements since then. Improvements include the following:
  a much more accurate instrument spectral line profile, an increase
  in the wavelength range used for the observations, an increase in the
  statistical accuracy of the observations by increasing the observation
  time, and inclusion of a background measurement as part of every set of
  observations. We have also investigated the sensitivity to the detector
  high voltage, investigated the effects of diffraction in the instrument,
  determined the stray light effects and the Thompson scattering
  effects, which both turn out to be small except for scattering of Si
  III 120.6 nm. That scattered light is out of the primary wavelength
  range of interest. We believe that we have now demonstrated that
  UVCS has the sensitivity to distinguish between a Gaussian coronal
  velocity distribution and a kappa = 4 or smaller distribution. It is
  generally believed that the required seed particle population needed
  to produce SEPs of interest with a CME shock would have a velocity
  distribution with 0.001 to 0.01 of the particles with speeds that
  exceed 1000 km/s. Assuming a kappa distribution that is symmetric
  in the tangential plane and Maxwellian in the radial direction, this
  would correspond to a distribution with kappa = 3.5 or smaller. This
  paper will report the results of examining a fairly large body of new
  observations obtained with the new procedure and report the departures
  from a Maxwellian distribution. It will also report the CME predecessor
  history of each observation. This work is supported by the National
  Aeronautics and Space Administration (NASA) under Grant NNX07AL72G to
  the Smithsonian Astrophysical Observatory. Kohl J. L., Cranmer, S. R.,
  Fineschi, S., Gardner, L. D., Phillips, D. H., Raymond, J. C., and Uzzo,
  M., Proc. SOHO 17 - 10 Years of SOHO and Beyond (ESA SP-617, July 2006).

Title: Multi-Instrument Searches for Polar Jets: Characterizing Jet
    Heating and Cooling
Authors: Miralles, M. P.; Cranmer, S. R.; Raymond, J. C.; Kohl, J. L.
Bibcode: 2007IUGG...24..691M
Altcode:
  We will present the preliminary results obtained with SOHO, in
  particular UVCS, during the SOHO-TRACE-Hinode coordinated observation
  campaign (8-21 January 2007) for the north and south polar coronal
  holes. The emphasis is on identifying and tracing polar jets from the
  solar surface out into the accelerating solar wind and determining
  their physical properties as a function of height and time. It is still
  unclear whether the hot jets resolved by Hinode are the same phenomenon
  as the cooler jets identified at the last solar minimum by EIT, LASCO,
  and UVCS. We also aim to clarify the relationship between the episodic
  jets and the longer-lived polar plumes.

Title: Tracking UVCS/SOHO Responsivity with Observations of ζ Tau
Authors: Valcu, Bogdan; Smith, Peter L.; Gardner, Larry D.; Raymond,
   John C.; Miralles, Mari-Paz; Kohl, John L.
Bibcode: 2007SoPh..243...93V
Altcode:
  We have tracked the spectral responsivity of the ultraviolet channels of
  the UVCS (Ultraviolet Coronagraph Spectrometer) instrument on SOHO by
  repeated observations of a stable hot star. We demonstrate first that
  the ultraviolet spectral irradiance of the Be star ζ Tau (HD 37202)
  for the 100- to 125-nm wavelength range has been sufficiently constant
  for our purposes when measured periodically over the course of the
  SOHO mission. We then use ζ Tau as a radiometric transfer standard to
  determine an average decrease beginning in November of 1998 of 13.0%
  per year in the responsivity of the UVCS O VI channel for wavelengths
  near H I Ly α and for a particular UVCS unvignetted aperture used
  for science observations. The calibration tracking method involves
  separating two ζ Tau spectral regions that are overlapped on part
  of the detector. The change in the responsivity of UVCS/SOHO began in
  late 1998 as determined by comparison of simultaneous observations of
  the corona carried out with UVCS/SOHO and the freshly-calibrated UVCS
  instrument on the Spartan 201 satellite in early November of 1998.

Title: Towards the UVCS Coronal Hole Atlas for Solar Cycle 23:
    The Data
Authors: Miralles, Mari Paz; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2007AAS...210.3005M
Altcode: 2007BAAS...39..143M
  We have measured with the SOHO Ultraviolet Coronagraph Spectrometer
  (UVCS) the physical properties of over 165 large coronal holes that
  produced a variety of high-speed solar wind conditions at 1 AU. This
  data set includes observations of coronal holes of different sizes and
  latitudes having a range of magnetic field properties. <P />We will
  present measured parameters (intensities, line widths) for protons and
  oxygen ions, as well as electron density as constrained by polarization
  brightness (pB), for the coronal holes observed from the last solar
  minimum in 1996 to the present. We will also present selected portions
  of in-situ solar wind data that are matched, where possible, to source
  regions in the corona, which have been characterized by UVCS. <P />The
  UVCS atlas of coronal holes will provide information about the H I
  Lyman alpha and O VI line profiles in the extended corona. The atlas
  will be made available in electronic format, with machine readable
  tables, as a supplement to a leading archival journal. <P />This work
  is supported by NASA under Grants NNX06AG95G and NNG06GI88G to the
  Smithsonian Astrophysical Observatory, by the Italian Space Agency,
  and by PRODEX (Swiss contribution).

Title: Transition Region Emission and Energy Input to Thermal Plasma
    during the Impulsive Phase of Solar Flares
Authors: Raymond, John C.; Holman, Gordon; Ciaravella, A.; Panasyuk,
   A.; Ko, Y. -K.; Kohl, J.
Bibcode: 2007ApJ...659..750R
Altcode: 2007astro.ph..1359R
  The energy released in a solar flare is partitioned between thermal
  and nonthermal particle energy and lost to thermal conduction and
  radiation over a broad range of wavelengths. It is difficult to
  determine the conductive losses and the energy radiated at transition
  region temperatures during the impulsive phases of flares. We
  use UVCS measurements of O VI photons produced by five flares and
  subsequently scattered by O VI ions in the corona to determine the
  5.0&lt;=logT&lt;=6.0 transition region luminosities. We compare
  them with the rates of increase of thermal energy and the conductive
  losses deduced from RHESSI and GOES X-ray data using areas from RHESSI
  images to estimate the loop volumes, cross-sectional areas, and scale
  lengths. The transition region luminosities during the impulsive phase
  exceed the X-ray luminosities for the first few minutes, but they are
  smaller than the rates of increase of thermal energy unless the filling
  factor of the X-ray-emitting gas is ~0.01. The estimated conductive
  losses from the hot gas are too large to be balanced by radiative
  losses or heating of evaporated plasma, and we conclude that the area
  of the flare magnetic flux tubes is much smaller than the effective
  area measured by RHESSI during this phase of the flares. For the 2002
  July 23 flare, the energy deposited by nonthermal particles exceeds
  the energy radiated in X-rays, the energy radiated at transition region
  temperatures, and the rate of increase of the thermal energy.

Title: 2006 LWS TR &amp; T Solar Wind Focused Science Topic Team:
    The Beginnings
Authors: Miralles, M. P.; Bhattacharjee, A.; Landi, E.; Markovskii,
   S.; Cranmer, S. R.; Doschek, G. A.; Forbes, T. G.; Isenberg, P. A.;
   Kohl, J. L.; Ng, C.; Raymond, J. C.; Vasquez, B. J.
Bibcode: 2006AGUFMSH11A0371M
Altcode:
  The Solar Wind Focused Science Topic (FST) team was created to
  apply a combination of theoretical studies, numerical simulations,
  and observations to the understanding of how the fast and slow solar
  wind are heated and accelerated. Four proposals were selected for this
  FST team. They will investigate the role of energy sources and kinetic
  mechanisms responsible for the heating and acceleration of the solar
  wind. In particular, the FST team will examine magnetic reconnection
  and turbulence as possible heating mechanisms. Plasma properties and
  their evolution over the solar cycle, determined from the analysis of
  remote and in situ measurements, will be used to put firm constraints
  on the models. The work of the Solar Wind FST team is in its initial
  stages. The organization, planning, and findings resulting from the
  first FST team meeting will be reported.

Title: Comparison of UVCS/SOHO Streamer Properties with 1 AU Solar
    Wind Measurements
Authors: Strachan, L.; Panasyuk, A. V.; Miralles, M. P.; Kohl, J. L.
Bibcode: 2006ESASP.617E.108S
Altcode: 2006soho...17E.108S
  No abstract at ADS

Title: Spectroscopic Observations of the Extended Solar Corona Above
    Quiet Sun Regions
Authors: Suleiman, R. M.; Kohl, J. L.; Strachan, L.; Phillips, D.;
   Uzzo, M.
Bibcode: 2006ESASP.617E.109S
Altcode: 2006soho...17E.109S
  No abstract at ADS

Title: Coronal Hole Properties During the First Decade of UVCS/SOHO
Authors: Miralles, M. P.; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2006ESASP.617E..15M
Altcode: 2006soho...17E..15M
  No abstract at ADS

Title: Progress Toward Measurements of Suprathermal Tails in Coronal
    Proton Velocity Distributions
Authors: Kohl, J. L.; Panazyuk, A. V.; Cranmer, S. R.; Fineschi, S.;
   Gardner, L. D.; Phillips, D. H.; Raymond, J. C.; Uzzo, M.
Bibcode: 2006ESASP.617E..25K
Altcode: 2006soho...17E..25K
  No abstract at ADS

Title: Comparisons of H I Ly-Alpha Line Widths in Streamers and
    Coronal Holes Measured with UVCS/SOHO and UVCS/Spartan-201 in
    November 1998
Authors: Gardner, L. D.; Miralles, M. -P.; Panasyuk, A.; Strachan,
   L.; Kohl, J. L.
Bibcode: 2006ESASP.617E..90G
Altcode: 2006soho...17E..90G
  No abstract at ADS

Title: The First Decade of UVCS/SOHO: Coronal Hole Properties
Authors: Miralles, Mari Paz; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2006SPD....37.1003M
Altcode: 2006SPD....37.1003P; 2006BAAS...38R.237M
  We have measured with the SOHO Ultraviolet Coronagraph Spectrometer
  (UVCS) the physical properties of over 155 large coronal holes that
  produced a variety of high-speed solar wind conditions at 1 AU. This
  data set includes observations of coronal holes of different sizes
  and latitudinal locations present throughout solar cycle 23.In the
  spring of 2006, the polar coronal holes have not yet evolved to the
  fully quiescent minimum state seen in 1996-1997, although the next
  solar minimum is expected to occur during 2006-2007. We will present
  the solar cycle dependence of the derived plasma parameters for O5+
  and protons from the last solar minimum in 1996 to present and compare
  them, where possible, with the in situ solar wind properties.This
  work is supported by NASA under Grant NNG05GG38G tothe Smithsonian
  Astrophysical Observatory, by the Italian Space Agency, and by PRODEX
  (Swiss contribution).

Title: Comparison Between Coronal and In Situ Plasma Properties Over
    The Solar Cycle
Authors: Strachan, Leonard, Jr.; Panasyuk, A. V.; Miralles, M. P.;
   Kohl, J. L.
Bibcode: 2006SPD....37.1004S
Altcode: 2006BAAS...38..238S
  The Ultraviolet Coronagraph Spectrometer (UVCS) on SOHO has made
  detailed observations of coronal streamers in the extended corona
  (1.5 R<SUB>o</SUB> &lt; r &lt; 10 R<SUB>o</SUB>) for almost a complete
  solar cycle. Measurements of ultraviolet line profiles and intensities
  and polarized white light intensities are used to determine plasma
  parameters (proton and ion temperatures, electron densities, and ion
  outflow speeds) for these large scale coronal structures. In this
  paper we compare the variations in streamer properties obtained in
  the extended corona with the properties found in the solar wind at
  1 AU. Solar wind velocities and densities derived from in situ data
  are used for comparisons. Such comparisons may be used to distinguish
  between solar wind variations due to changes in physical parameters
  of streamers at the Sun as opposed to changes in flow geometry. This
  work was supported by NASA grants NAG5-12781 and NNG05GG38G to the
  Smithsonian Astrophysical Observatory.

Title: Ultraviolet spectroscopy of the extended solar corona
Authors: Kohl, John L.; Noci, Giancarlo; Cranmer, Steven R.; Raymond,
   John C.
Bibcode: 2006A&ARv..13...31K
Altcode: 2006A&ARv.tmp....1K
  The first observations of ultraviolet spectral line profiles
  and intensities from the extended solar corona (i.e., more than
  1.5 solar radii from Sun-center) were obtained on 13 April 1979
  when a rocket-borne ultraviolet coronagraph spectrometer of the
  Harvard-Smithsonian Center for Astrophysics made direct measurements
  of proton kinetic temperatures, and obtained upper limits on outflow
  velocities in a quiet coronal region and a polar coronal hole. Following
  those observations, ultraviolet coronagraphic spectroscopy has
  expanded to include observations of over 60 spectral lines in
  coronal holes, streamers, coronal jets, and solar flare/coronal
  mass ejection (CME) events. Spectroscopic diagnostic techniques
  have been developed to determine proton, electron and ion kinetic
  temperatures and velocity distributions, proton and ion bulk flow
  speeds and chemical abundances. The observations have been made during
  three sounding rocket flights, four Shuttle deployed and retrieved
  Spartan 201 flights, and the Solar and Heliospheric Observatory (SOHO)
  mission. Ultraviolet spectroscopy of the extended solar corona has led
  to fundamentally new views of the acceleration regions of the solar wind
  and CMEs. Observations with the Ultraviolet Coronagraph Spectrometer
  (UVCS) on SOHO revealed surprisingly large temperatures, outflow speeds,
  and velocity distribution anisotropies in coronal holes, especially for
  minor ions. Those measurements have guided theorists to discard some
  candidate physical processes of solar wind acceleration and to increase
  and expand investigations of ion cyclotron resonance and related
  processes. Analyses of UVCS observations of CME plasma properties
  and the evolution of CMEs have provided the following: temperatures,
  inflow velocities and derived values of resistivity and reconnection
  rates in CME current sheets, compression ratios and extremely high ion
  temperatures behind CME shocks, and three dimensional flow velocities
  and magnetic field chirality in CMEs. Ultraviolet spectroscopy has
  been used to determine the thermal energy content of CMEs allowing the
  total energy budget to be known for the first time. Such spectroscopic
  observations are capable of providing detailed empirical descriptions
  of solar energetic particle (SEP) source regions that allow theoretical
  models of SEP acceleration to be tailored to specific events, thereby
  enabling in situ measurements of freshly emitted SEPs to be used for
  testing and guiding the evolution of SEP acceleration theory. Here we
  review the history of ultraviolet coronagraph spectroscopy, summarize
  the physics of spectral line formation in the extended corona, describe
  the spectroscopic diagnostic techniques, review the advances in our
  understanding of solar wind source regions and flare/CME events provided
  by ultraviolet spectroscopy and discuss the scientific potential of
  next generation ultraviolet coronagraph spectrometers.

Title: Measurements of Electron Impact Excitation Cross Sections at
    the Harvard-Smithsonian Center for Astrophysics
Authors: Gardner, L. D.; Kohl, J. L.
Bibcode: 2006nla..conf..186G
Altcode:
  The analysis of absolute spectral line intensities and intensity
  ratios with spectroscopic diagnostic techniques provides empirical
  determinations of chemical abundances, electron densities and
  temperatures in astrophysical objects. Since spectral line intensities
  and their ratios are controlled by the excitation rate coefficients
  for the electron temperature of the observed astrophysical structure,
  it is imperative that one have accurate values for the relevant rate
  coefficients. Here at the Harvard-Smithsonian Center for Astrophysics,
  we have been carrying out measurements of electron impact excitation
  (EIE) for more than 25 years. We will illustrate our experimental
  approach and apparatus by discussing a measurement of EIE in C^{2+}
  (2s2p ^3P^o → 2p^2 ^3P).

Title: Ultraviolet spectroscopy of the extended solar corona
Authors: Kohl, J.
Bibcode: 2006cosp...36.3317K
Altcode: 2006cosp.meet.3317K
  Since the first observations of HI Ly-alpha spectral line profiles and
  intensities of the extended solar corona were obtained on 13 April 1979
  with a rocket-borne ultraviolet coronagraph spectrometer ultraviolet
  coronagraphic spectroscopy has expanded to include observations of
  over 60 spectral lines in coronal holes streamers coronal jets and
  solar flare coronal mass ejection CME events Spectroscopic diagnostic
  techniques have been developed to determine proton electron and ion
  kinetic temperatures and velocity distributions proton and ion bulk flow
  speeds and chemical abundances Ultraviolet coronagraph spectroscopy has
  led to fundamentally new views of the acceleration regions of the solar
  wind and CMEs Significant progress has been made toward identifying
  and characterizing the physical processes that heat the extended corona
  accelerate the various plasma components of the solar wind and produce
  a wide range of non-equilibrium phenomena in CMEs Perhaps most notably
  the surprisingly extreme plasma conditions observed by UVCS SOHO in
  coronal holes have guided theorists to discard some candidate physical
  processes and to further investigate others The UVCS observations
  of coronal holes---and subsequent theoretical investigations of ion
  cyclotron resonance---have been cited increasingly in literature devoted
  to other plasma environments such as the Earth s aurora Gavrishchaka
  et al backslash 2000 and they have guided new investigations in pure
  plasma physics e g Mizuta backslash Hoshino 2001 Chen et al backslash

Title: A Solar Energetic Particle Mission (SEPM) for the S3C Great
    Observatory
Authors: Strachan, L.; Kohl, J. L.; Cranmer, S. R.; Esser, R.; Gardner,
   L. D.; Lin, J.; Raymond, J. C.; van Ballegooijen, A.; Socker, D. G.
Bibcode: 2005AGUFMSH51C1221S
Altcode:
  The S3C Great Observatory concept is guided by a systems approach
  to understanding the heliosphere. A Solar Energetic Particle Mission
  (SEPM) can make valuable contributions to this Great Observatory in
  conjunction with upcoming Living with a Star (LWS) missions e.g. Solar
  Dynamics Observatory and Sentinels. SEPM can provide the remote sensing
  component to a program for better understanding how, when, and where
  solar energetic particles (SEPs) are produced. Such a coordinated
  approach will include coronagraphic UV spectroscopy and visible light
  polarimetery with SEPM, along with in situ particles and fields,
  X-ray and gamma-ray measurements from spacecraft close to the Sun
  (Inner Heliospheric Sentinels). While SEPM will use plasma diagnostics
  that are derived from the UVCS and LASCO coronagaraphs on SOHO, it
  will have an order of magnitude improvement in its capabilities.

Title: An Initial Attempt to Measure Suprathermal Tails in Coronal
    Proton Velocity Distributions
Authors: Kohl, J. L.; Cranmer, S. R.; Fineschi, S.; Gardner, L. D.;
   Panasyuk, A. V.; Raymond, J. C.; Uzzo, M.
Bibcode: 2005AGUFMSH44A..05K
Altcode:
  Test observations made with the Ultraviolet Coronagraph Spectrometer
  (UVCS) on SOHO in August 2005 are being used to make an initial
  assessment of the possibility of measuring suprathermal tails in the
  proton velocity distribution functions. Any successful theory of solar
  energetic particle (SEP) production by CME shocks must account for the
  large observed variations in SEP spectral characteristics and elemental
  abundances. Some have proposed that this variability arises from an
  inherently variable population of suprathermal seed particles (e.g.,
  Mason et al. 2005): some that exist all the time in the solar wind
  (with varying properties depending on wind speed) and some that are
  associated with prior flares and CME shocks (e.g., Kahler 2004; Tylka
  et al. 2005). As yet, though, the suprathermal particle population in
  the solar corona has never been measured. The seed particle number
  density predicted for typical gradual SEP events is about 0.002 -
  0.01 times the thermal population (e.g., Lee 2005), and should, in at
  least some cases, correspond to a measurable enhancement in the wing
  of the H I Ly-alpha profile. In August 2005, the Ly-alpha channel of
  UVCS was recommissioned and used to observe HI Ly-alpha line profiles
  at 2.0 solar radii in coronal holes, helmet streamers, above active
  regions and after a CME. The holographically ruled diffraction grating
  provides the low stray light level needed to observe the tail of the
  line profile out to about 0.5 nm from line center. New observations
  as well as measurements from the original UVCS laboratory calibration
  and in flight measurements from earlier in the mission are being
  used to characterize the instrument response to monochromatic light
  so such instrument effects can be removed. Initial results will be
  reported. This work is supported by NASA Grant NNG05GG38G to the
  Smithsonian Astrophysical Observatory Kahler, S. W. 2004, ApJ, 603,
  330. Lee, M. A. 2005, ApJ Supp., 158, 38. Mason, G., Desai, M.,
  Mazur, J., &amp; Dwyer, J. 2005, COSPAR 35th Scientific Assemly,
  p. 1596. Tylka, A. J., et al. 2005, ApJ, 625, 474.

Title: Capabilities of UV Coronagraphic Spectroscopy for Studying
    the Source Regions of Solar Energetic Particles and the Solar Wind
Authors: Kohl, J. L.; Cranmer, S. R.; Gardner, L. D.; Lin, Jun;
   Raymond, John C.; Strachan, Leonard
Bibcode: 2005ESASP.592..677K
Altcode: 2005astro.ph..6509K; 2005ESASP.592E.135K; 2005soho...16E.135K
  We summarize the unique capabilities of UV coronagraphic spectroscopy
  for determining the detailed plasma properties (e.g., density,
  temperature, outflow speed, composition) of the source regions of both
  transient phenomena such as CMEs, flares, and solar energetic particles
  (SEPs) and more time-steady solar wind streams. UVCS/SOHO observations
  have provided the first detailed diagnostics of the physical conditions
  of CME plasma in the extended corona. It provided new insights into
  the roles of shock waves, reconnection, and magnetic helicity in CME
  eruptions. We summarize past observations and discuss the diagnostic
  potential of UV coronagraphic spectroscopy for characterizing two
  possible sites of SEP production: CME shocks and reconnection current
  sheets. UVCS/SOHO has also led to fundamentally new views of the
  acceleration region of the solar wind. Understanding the physical
  processes in this region, which ranges from the low corona (1.1 to
  1.5 Rsun) past the sonic points (greater than 5 Rsun), is key to
  linking the results of solar imaging to in situ particle and field
  detection. Despite the advances that have resulted from UVCS/SOHO,
  more advanced instrumentation could determine properties of additional
  ions with a wider sampling of charge/mass combinations. This would
  provide much better constraints on the specific kinds of waves that are
  present as well as the specific collisionless damping modes. Electron
  temperatures and departures from Maxwellian velocity distributions
  could also be measured. The instrumentation capable of making the
  above observations will be described.

Title: Ultraviolet spectroscopy of solar energetic particle source
    regions
Authors: Kohl, J. L.; Cranmer, S.; Esser, R.; Gardner, L. D.; Fineschi,
   S.; Lin, J.; Panasyuk, A.; Raymond, J. C.; Strachan, L.
Bibcode: 2005SPIE.5901..262K
Altcode:
  A problem of fundamental importance for future space travel to the
  Moon and Mars is the determination and prediction of the radiation
  environment generated by the Sun. The sources of solar energetic
  particles (SEP) and the physical processes associated with their
  acceleration and propagation are not well understood. Ultraviolet
  coronagraphic spectroscopy uniquely has the capabilities for determining
  the detailed plasma properties of the likely source regions of such
  particles. This information can be used to develop empirical models
  of the source regions for specific events, and it can provide the key
  information needed to identify and understand the physical processes
  that produce SEP hazards. UVCS/SOHO observations have provided the first
  detailed diagnostics of the plasma parameters of coronal mass ejections
  (CMEs) in the extended corona. These observations have provided new
  insights into the roles of shock waves, reconnection and magnetic
  helicity in CME eruptions. Next generation ultraviolet coronagraph
  spectrometers could provide additional diagnostic capabilities. This
  paper summarizes past observations, and discusses the diagnostic
  potential of advanced ultraviolet coronagraphic spectroscopy for
  characterizing two possible sites of SEP production: CME shocks and
  reconnection current sheets.

Title: Absolute empirical rate coefficient for the excitation of
    the 117.6 nm line in C III
Authors: Gardner, L. D.; Daw, A. N.; Janzen, P. H.; Atkins, N.; Kohl,
   J. L.
Bibcode: 2005AGUSMSP21B..04G
Altcode:
  We have measured the absolute cross sections for electron impact
  excitation (EIE) of C2+ (2s2p 3P° - 2p2 3P) for energies from below
  threshold to 17 eV above and derived EIE rate coefficients required for
  astrophysical applications. The uncertainty in the rate coefficient at a
  typical solar temperature of formation of C2+ is less than ± 6 %. Ions
  are produced in a 5 GHz Electron Cyclotron Resonance (ECR) ion source,
  extracted, formed into a beam, and transported to a collision chamber
  where they collide with electrons from an electron beam inclined at
  45 degrees. The beams are modulated and the radiation from the decay
  of the excited ions at λ 117.6 nm is detected synchronously using an
  absolutely calibrated optical system that subtends slightly over π
  steradians. The fractional population of the C2+ metastable state in
  the incident ion beam has been determined experimentally to be 0.42 ±
  0.03 (1.65 σ). At the reported ± 15 % total experimental uncertainty
  level (1.65 σ), the measured structure and absolute scale of the cross
  section are in fairly good agreement with 6-term close-coupling R-matrix
  calculations and 90-term R-matrix with pseudo-states calculations,
  although some minor differences are seen just above threshold. As
  density-sensitive line intensity ratios vary by only about a factor
  of 5 as the density changes by nearly a factor of 100, even a 30 %
  uncertainty in the excitation rate can lead to a factor of 3 error in
  density. <P />This work is supported by NASA Supporting Research and
  Technology grants NAG5- 9516 and NAG5-12863 in Solar and Heliospheric
  Physics and by the Smithsonian Astrophysical Observatory.

Title: Solar Cycle Variations of Coronal Hole Properties
Authors: Miralles, M. P.; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2005AGUSMSP51B..07M
Altcode:
  As of early 2005, we have measured with the SOHO Ultraviolet
  Coronagraph Spectrometer (UVCS) the physical properties of at least
  136 large coronal holes that produced a variety of high-speed solar
  wind conditions at 1 AU. UVCS has been used to observe O VI (103.2 and
  103.7 nm) and H I Lyman alpha (121.6 nm) emission lines as a function
  of heliocentric distance in coronal holes since 1996. The analysis of
  their spectroscopic parameters allows us to identify similarities
  and differences among coronal holes at different phases of the
  solar cycle. From such measurements we can derive plasma parameters
  (densities, temperatures, velocity distribution anisotropies, and
  outflow speeds) for O5+ and protons as a function of heliocentric
  distance in the coronal holes. These properties, combined with other
  observed quantities such as white-light polarization brightness and the
  more-or-less unipolar magnetic fluxes measured on-disk, let us map out
  the "allowed parameter space" of coronal hole plasma properties more
  fully than ever before. We will present the solar cycle dependence
  of the above plasma parameters from the last solar minimum in 1996
  to present and compare them, where possible, with the in situ solar
  wind properties. We will also present an update on the pattern that
  is beginning to emerge, i.e., coronal holes with lower densities at
  a given heliocentric distance tend to exhibit faster ion outflow and
  higher ion temperatures. This information will thus be used to set firm
  empirical constraints on coronal heating and solar wind acceleration in
  coronal holes. In 2005, the polar coronal holes have not yet evolved
  to the fully quiescent minimum state seen in 1996-1997, though the
  next solar minimum is expected to occur in about 1.5 to 2 years. This
  work is supported by NASA under Grant NNG04GE84G to the Smithsonian
  Astrophysical Observatory, by the Italian Space Agency, and by PRODEX
  (Swiss contribution).

Title: New Synoptic Maps of the Solar Corona from UVCS Observations
Authors: Strachan, L.; Panasyuk, A. V.; Miralles, M.; Kohl, J. L.;
   Baham, M.
Bibcode: 2005AGUSMSH43A..01S
Altcode:
  We present for the first time synoptic maps of the extended solar corona
  (r/Ro &gt; 1.5) based on eight years of data from the SOHO Ultraviolet
  Coronagraph Spectrometer (UVCS). The data reveal the changes in the
  physical properties of the large scale features in the corona. Maps of O
  VI line intensities, line widths, and line ratios for the O VI 1032/1037
  doublet and intensities and line widths for the H I Ly-alpha line reveal
  information about the evolution of coronal densities, temperatures,
  and outflow velocities over the solar cycle. In particular these data
  are used in support of program to understand the solar cycle variation
  of coronal holes and coronal streamers. This work is supported by
  NASA Grant NAG5-12781 to the Smithsonian Astrophysical Observatory and
  NASA subcontract OGSP21010200061SAO awarded to SAO through a grant to
  Southern Universty at Baton Rouge.

Title: On the Incompatibility Between UVCS/SOHO Observations of
    Polar Coronal Holes and Isotropic Oxygen Velocity Distributions
Authors: Cranmer, S. R.; Panasyuk, A. V.; Kohl, J. L.
Bibcode: 2005AGUSMSP33A..02C
Altcode:
  We present a reanalysis of UVCS/SOHO observations of the O VI 1032,
  1037 emission line doublet at large heliocentric distances in polar
  coronal holes during the last solar minimum (1996-1997). The traditional
  interpretation of the broad line widths and unusual intensity ratios
  has been that the oxygen ions exhibit a strong temperature anisotropy,
  with the temperature perpendicular to the magnetic field being much
  larger than the temperature parallel to the field. However, a recent
  paper by Raouafi and Solanki suggested that it may be possible to
  model the observations using an isotropic velocity distribution of
  (still very hot) oxygen ions. In this presentation we show that the
  standard interpretation of an anisotropic distribution is the only
  one that is fully consistent with the observational data. Using the
  same electron density and magnetic field models assumed by Raouafi
  and Solanki, we varied the 3 main ion properties (outflow speed and
  the 2 bi-Maxwellian temperature components) in a 3D data-cube that
  exhaustively treated all possibilities. This data-cube spans the
  parameter space of both earlier UVCS/SOHO empirical models and the new
  proposal of Raouafi and Solanki. Even so, we find that above about 2.5
  solar radii the only points in the data-cube that reproduce the actual
  observed line widths and intensity ratios are those with substantial
  temperature anisotropies.

Title: Absolute Cross Section for Electron Impact Excitation of
    Metastable C<SUP>2+</SUP>
Authors: Daw, Adrian; Gardner, Larry; Janzen, Paul; Kohl, John
Bibcode: 2004APS..DMP.P1103D
Altcode:
  Progress toward measurements of the absolute cross section for electron
  impact excitation (EIE) of C^2+ (2s2p ^3P^o - 2p^2 ^3P) for energies
  below threshold to 15 eV above is reported. These measurements will be
  used to determine the EIE rate coefficients required for astrophysical
  applications. Ions are produced in a 5 GHz Electron Cyclotron Resonance
  (ECR) ion source. A modulated beams technique with inclined electron
  and ion beams is being used. The radiation from the excited ions
  at λ 117.5 nm is detected using an absolutely calibrated optical
  system that subtends slightly over π steradians. The population
  of the C^2+ metastable state in the incident ion beam is determined
  experimentally. This work is supported by NASA Supporting Research and
  Technology grants NAG5-9516 and NAG5-12863 in Solar and Heliospheric
  Physics and by the Smithsonian Astrophysical Observatory.

Title: Advantages of the Photon Detection Method for Beams
    Measurements of Electron Impact Excitation Rates
Authors: Kohl, J. L.; Gardner, L. D.; Daw, A.
Bibcode: 2004AAS...204.5106K
Altcode: 2004BAAS...36R.753K
  Beams experiments are well suited to measurements of electron impact
  excitation (EIE) cross sections for specific transitions of positive
  ions. Excitation events can be determined directly by detecting
  either the emitted photon following excitation and radiative decay
  or by detecting the inelastically scattered electron. The photon
  method has been used at Harvard-Smithsonian to measure absolute cross
  sections involved in the production of C II 133.5 nm, C III 117.6 nm,
  C IV 155.0 nm, and Si III 120.6 nm. The experiments allow the cross
  sections to be determined completely from measured quantities such as
  the distribution of electrons and ions in the beams, the beam energy,
  the photon emission rate and the ground state and metastable state
  population fractions (when required). Typical standard uncertainties
  are +/- 9 percent. Population fractions are determined by two methods:
  1) the beams attenuation method, which relies on differences between
  the ground state and metastable state charge transfer cross sections
  with a selected gas target, and 2) measurement of the radiative decay
  intensity from metastable ions in the incident beam. Collision energies
  from threshold to well above threshold are accessable allowing the
  determination of empirical electron collision rates for both maxwellian
  and non-maxwellian electron velocity distributions. Recent results,
  comparison to theoretical values, astrophysical applications, the
  experimental method and the apparatus, including a new 5 GHz Electron
  Cyclotron Resonance (ECR) ion source, will be described. This work was
  supported by NASA Grant NAG5-12863 to the Smithsonian Astrophysical
  Observatory.

Title: Towards a Physical Characterization of Large Coronal Holes
Authors: Miralles, M. P.; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2004AAS...204.7106M
Altcode: 2004BAAS...36S.797M
  The Ultraviolet Coronagraph Spectrometer (UVCS) aboard SOHO was used
  to observe O VI (103.2 and 103.7 nm) and H I Lyman alpha (121.6 nm)
  emission lines as a function of heliocentric distance in more than 85
  coronal holes, in order to characterize the physical properties of
  coronal holes at different phases of the solar cycle. Our previous
  analyses of UVCS observations have shown that polar and equatorial
  coronal holes produce different acceleration profiles and have
  different oxygen kinetic temperatures. We examine the variation
  in the characteristics of representative large coronal holes
  producing a variety of high-speed conditions at 1 AU. <P />This
  work is supported by NASA under Grant NAG5-12865 to the Smithsonian
  Astrophysical Observatory, by the Italian Space Agency and by PRODEX
  (Swiss contribution).

Title: Differences in Plasma Conditions Among 85 Large Coronal Holes
Authors: Miralles, M. P.; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2004AGUSMSH41A..03M
Altcode:
  We have measured ultraviolet spectroscopic parameters as a function
  of heliocentric distance for more than 85 coronal holes, in order to
  characterize the physical properties of coronal holes at different
  phases of the solar cycle. The Ultraviolet Coronagraph Spectrometer
  (UVCS) aboard SOHO was used to observed O VI (103.2 and 103.7 nm)
  and H I Lyman alpha (121.6 nm) emission lines to determine kinetic
  temperatures, average densities, and outflow speeds in coronal
  holes. UVCS observations provide unique information on the heating and
  acceleration processes in the corona. Our previous analyses of UVCS
  observations have shown that solar minimum (polar) and solar maximum
  (equatorial) coronal holes produce different acceleration profiles
  and have different oxygen kinetic temperatures. We also examine the
  differences in the characteristics of representative coronal holes
  producing a variety of high-speed conditions (550-800 km/s) at 1
  AU. These analyses provide limits on the coronal plasma properties
  and put constraints on the physical processes that are responsible
  for the heating of the extended corona and the acceleration of the
  solar wind. This work is supported by NASA under Grant NAG5-12865 to
  the Smithsonian Astrophysical Observatory, by the Italian Space Agency
  and by PRODEX (Swiss contribution).

Title: Contributions from Ultraviolet Spectroscopy to the Prediction
    of High-energy Proton Hazards from CME Shocks
Authors: Lin, J.; Raymond, J. C.; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2004AAS...204.7205L
Altcode: 2004BAAS...36Q.799L
  A significant potential hazard to astronauts and their equipment
  in interplanetary space is the relativistic proton flux produced by
  coronal mass ejections (CMEs) and solar flares. The longest-duration
  phase of solar energetic particle (SEP) activity is believed to come
  from the CME shock as it propagates through the extended corona and
  heliosphere. Ultraviolet spectroscopy by SOHO has revealed a means
  for: (1) detecting and characterizing CME shocks in the corona, and
  (2) determining the plasma conditions in the pre-CME corona which are
  needed to understand the formation and evolution of shocks. Such remote
  sensing - combined with models of SEP acceleration and transport -
  can be used to predict the strength, duration, and production sites of
  the radiation. <P />This poster describes the specific means by which
  ultraviolet spectroscopy and other remote-sensing data can be used to
  determine the inputs and boundary conditions for individual events (such
  as the October-November 2003 storms) in existing SEP model codes. We
  also discuss an additional potential source of SEP radiation associated
  with electric fields in the current sheets that form in flare regions
  in the wake of CME. Both observations and model calculations show that
  the reconnection-induced electric field can reach a maximum strength
  of a few V/cm within tens of minutes after the onset of the eruption,
  then decreases gradually over several hours. SEPs produced in these
  regions may account for X-rays and γ -rays observed prior to the
  formation of CME shocks. Ultraviolet spectroscopy has been shown to
  provide constraints on the plasma properties in all of the above CME
  features. <P />This work is supported by NASA under grant NAG5-12865 to
  the Smithsonian Astrophysical Observatory, by Agenzia Spaziale Italiana,
  and by the Swiss contribution to ESA's PRODEX program.

Title: Measurement of the Absolute Electron Impact Excitation Cross
    Section for the C III 117.6 nm Transition
Authors: Daw, A.; Janzen, P. H.; Gardner, L. D.; Kohl, J. L.
Bibcode: 2004AAS...204.7309D
Altcode: 2004BAAS...36..801D
  An inclined beams arrangement is being used to measure the absolute
  cross section for electron impact excitation of the C<SUP>2+</SUP>
  (2s2p <SUP>3</SUP>P<SUP>o</SUP> - 2p<SUP>2</SUP> <SUP>3</SUP>P)
  transition for energies below threshold to 15 eV above. These cross
  sections determine the EIE rate coefficients required for astrophysical
  applications. Ions are produced in a 5 GHz Electron Cyclotron Resonance
  (ECR) ion source. A modulated beams technique with inclined electron
  and ion beams is being used. The radiation from the excited ions at
  a wavelength of 117.5 nm is detected using an absolutely calibrated
  optical system that subtends slightly over pi steradians. The
  population of the C<SUP>2+</SUP> metastable state in the incident ion
  beam is determined experimentally. The measured cross sections will
  be presented and compared to those predicted by theory. This work is
  supported by NASA Supporting Research and Technology grants NAG5-9516
  and NAG5-12863 in Solar and Heliospheric Physics and by the Smithsonian
  Astrophysical Observatory.

Title: Low-latitude coronal holes during solar maximum
Authors: Miralles, M. P.; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2004AdSpR..33..696M
Altcode:
  The Ultraviolet Coronagraph Spectrometer (UVCS) on SOHO has been used
  to observe large low-latitude coronal holes during solar maximum that
  produced fast solar wind streams. UVCS observations show that large
  low-latitude coronal holes at solar maximum, coronal holes of at
  least 10° in longitude, have plasma properties that seem to bridge
  the gap between solar minimum polar coronal holes and streamers. The
  ion kinetic perpendicular temperatures in equatorial coronal holes are
  about 2 times larger than those in a solar minimum equatorial streamer,
  and about a factor of 2 smaller than those in polar coronal holes
  above 2 R<SUB>solar</SUB>. The outflow speeds for the large equatorial
  coronal holes observed by UVCS are 3-4 times lower than those in polar
  coronal holes between 2 and 3 R<SUB>solar</SUB>. The values for high-
  and mid-latitude coronal holes are in between those. In all these cases,
  the in situ data corresponding to these coronal holes showed high-speed
  wind streams with asymptotic speeds of 600-750 km s<SUP>-1</SUP>. These
  wind speeds approach those observed over polar coronal holes at solar
  minimum, but the outflow speeds in these coronal holes between 2 and
  3 R<SUB>solar</SUB> are different. In contrast to the polar coronal
  holes, the bulk of the solar wind acceleration must occur above
  3 R<SUB>solar</SUB> for large low-latitude coronal holes at solar
  maximum. These observations provide detailed empirical constraints
  for theoretical models and may be key to understanding how the various
  types of solar wind plasma are heated and accelerated.

Title: Coordinated UVCS/SOHO and VLA Observations of the Solar Corona
Authors: Miralles, M. P.; Cranmer, S. R.; Raymond, J. C.; Spangler,
   S. R.; Kohl, J. L.
Bibcode: 2003AGUFMSH22A0188M
Altcode:
  Coordinated UVCS/SOHO and VLA coronal observations took place during
  August 16--19, 2003. The radio source 3C 228 passed behind a streamer
  in the northeast at a heliocentric distance of about 7 solar radii,
  and behind the north coronal hole at about 4 solar radii in the latter
  part of the radio observation. The goal of this campaign is to combine
  the analysis of radio polarimetric sounding measurements of the corona
  with ultraviolet spectroscopy of the same regions, in order to obtain
  qualitatively new information about the properties of the solar coronal
  plasma. The Ultraviolet Coronagraph Spectrometer (UVCS) aboard SOHO
  observed O VI (103.2 and 103.7 nm) and H I Lyman alpha (121.6 nm)
  emission lines to determine kinetic temperatures, average densities
  and outflow speeds in the corona. UVCS observations provide unique
  information on the heating and acceleration processes in the corona. The
  Very Large Array (VLA) observations reveal the Faraday rotation of
  polarized radio waves due to passage through the magnetized plasma of
  the corona. These measurements provide limits on the coronal magnetic
  field strength and constrain the properties of magnetohydrodynamic (MHD)
  waves. Radio propagation techniques are a useful complementary tool
  to ultraviolet coronagraphic spectroscopy in determining the physical
  processes that are responsible for the heating of the extended corona
  and the acceleration of the solar wind. This work is supported by NASA
  under Grant NAG5-12865 to the Smithsonian Astrophysical Observatory,
  by the Italian Space Agency and by PRODEX (Swiss contribution).

Title: Empirically Determined Anisotropic Velocity Distributions and
    Outflows of O<SUP>5+</SUP> Ions in a Coronal Streamer at Solar Minimum
Authors: Frazin, R. A.; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2003ApJ...597.1145F
Altcode:
  Empirical constraints on the O<SUP>5+</SUP> velocity distributions
  and outflow speeds in a solar minimum equatorial streamer between 2.6
  and 5.1 R<SUB>solar</SUB> are determined using a spectral synthesis
  code that includes O VI Doppler dimming. These constraints follow
  directly from UV spectra taken on 1996 October 12 with the Ultraviolet
  Coronagraph Spectrometer (UVCS) on the Solar and Heliospheric
  Observatory (SOHO) satellite and three-dimensional electron densities
  derived from tomography applied to a time series of polarized
  white-light images taken with the Large Angle and Spectrometric
  Coronagraph (LASCO) also on SOHO. Four conclusions result from this
  work: (1) our analysis shows O<SUP>5+</SUP> velocity distribution
  anisotropy in the streamer legs and stalk and gives strong evidence that
  the microscopic velocity distribution (which excludes wave motions that
  equally affect all charged particles) is anisotropic, where the most
  probable speed perpendicular to the magnetic field direction exceeds
  that in the parallel direction; (2) there is preferential heating of the
  O<SUP>5+</SUP> ions over the protons in the streamer stalk and legs;
  (3) there is no evidence for preferential O<SUP>5+</SUP> heating in
  the core; and (4) the outflow velocity of the O<SUP>5+</SUP> ions is
  determined at heights above 4.6 R<SUB>solar</SUB>. All results have
  a confidence level of at least 70%.

Title: Plasma properties above coronal active regions inferred from
    SOHO/UVCS and radio spectrograph observations
Authors: Mancuso, S.; Raymond, J. C.; Kohl, J.; Ko, Y. -K.; Uzzo,
   M.; Wu, R.
Bibcode: 2003A&A...400..347M
Altcode:
  Information on coronal plasma was inferred from the joint analysis of
  type {II} radio bursts and SOHO UltraViolet Coronagraph Spectrometer
  (UVCS) observations. The data sample comprises 37 metric type {II}
  radio bursts observed by ground-based radio spectrographs in 1999,
  during the rising phase of the solar cycle. The coronal electron
  densities n_e were estimated with the diagnostic provided by UVCS
  observations of the O Vi doublet line intensities. Upper limits to
  the coronal Alfvén speed above active regions were inferred from
  the derived shock speeds by requiring that the disturbances propagate
  at least faster than the local characteristic speed. Information on
  the magnetic field strength B and plasma beta in the middle corona
  were finally extracted from the coronal Alfvén speed upper limits. A
  major improvement with respect to previous studies that used type {II}
  radio bursts to derive plasma properties, is that density profiles of
  the pre-shock plasma obtained a few hours before the passage of the
  shock were used instead of general electron density models taken from
  literature. Our main result is expressed by the inequality B(r) &lt;=
  (0.6 +/- 0.3) (r-1)<SUP>-1.2</SUP> G, that is valid in the range
  1.5 &lt;= r &lt;= 2.3 solar radii, and is consistent with previous
  estimates of the magnetic field above coronal active regions.

Title: Advanced spectroscopic and coronographic explorer: science
    payload design concept
Authors: Gardner, Larry D.; Kohl, John L.; Daigneau, Peter S.; Smith,
   Peter L.; Strachan, Leonard, Jr.; Howard, Russell A.; Socker, Dennis
   G.; Davila, Joseph M.; Noci, Giancarlo C.; Romoli, Marco; Fineschi,
   Silvano
Bibcode: 2003SPIE.4843....1G
Altcode:
  The Advanced Spectroscopic and Coronagraphic Explorer (ASCE) was
  proposed in 2001 to NASA's Medium-Class Explorer (MIDEX) program
  by the Smithsonian Astrophysical Observatory in collaboration with
  the Naval Research Laboratory, Goddard Space Flight Center and the
  Italian Space Agency. It is one of four missions selected for Phase A
  study in 2002. ASCE is composed of three instrument units: an Advanced
  Ultraviolet Coronagraph Spectrometer (AUVCS), an Advanced Large Aperture
  visible light Spectroscopic Coronagraph (ALASCO), and an Advanced Solar
  Disk Spectrometer (ASDS). ASCE makes use of a 13 m long boom that is
  extended on orbit and positions the external occulters of AUVCS and
  ALASCO nearly 15 m in front of their respective telescope mirrors. The
  optical design concepts for the instruments will be discussed.

Title: The ASCE EUV Polarimeter
Authors: Romoli, M.; Fineschi, S.; Uslenghi, M.; Corti, G.; Pace,
   E.; Ciaravella, A.; Tondello, G.; Noci, G.; Gardner, L. D.; Kohl, J. L.
Bibcode: 2003MmSAI..74..835R
Altcode:
  The SOHO mission has achieved important results in the physics of
  solar wind and coronal mass ejection acceleration, but most of the
  processes that drive this acceleration have not yet been explained. The
  Advanced Spectroscopic and Coronagraphic Explorer (ASCE) mission will
  carry on-board spectroscopic and polarimetric instrumentation of new
  generation that is designed to address the fundamental questions on this
  processes. Following a brief description of ASCE scientific objectives
  and instrumentation, the EUV polarimetric channel is described. The
  EUV Polarimeter (EUVP) is designed to measure for the first time the
  magnetic field vector in the extended corona through the Hanle effect,
  and the anisotropy of the ion velocity. The EUVP represents the
  contribution of the Italian solar physics community to the ASCE mission.

Title: The Advanced Spectroscopic and Coronagraphic Explorer (ASCE)
    Mission Concept Study
Authors: Kohl, J.; Howard, R.; Davila, J.; Noci, G.; Gardner, L.;
   Socker, D.; Romoli, M.; Strachan, L.; Floyd, L.; Cranmer, S.; Raymond,
   J.; van Ballegooijen, A.
Bibcode: 2002AGUFMSH52A0463K
Altcode:
  The ASCE Mission is currently in a Phase A feasibility study as a
  candidate for the upcoming MIDEX selection. The ASCE science payload
  provides next generation spectroscopic and polarimetric instrumentation
  aimed at identifying the physical processes governing solar wind
  generation and coronal mass ejections (CMEs). During the current phase,
  engineering design and analyses have demonstrated the feasibility of
  accomplishing the original mission objectives within the MIDEX mission
  constraints. The launch is planned for early 2007 and the operations
  and analyses are expected to continue for 5 years. ASCE data along with
  data analysis software and calibration data will be unrestricted and
  available to the scientific community via an automated web site. A
  Guest Investigator program is planned with an average of 15 grants
  running concurrently during 2008 to 2012. Grants would be awarded in
  response to proposals submitted during the first and subsequent years
  of the mission.

Title: UVCS/SOHO Observations of Large Coronal Holes During Solar
    Cycle 23
Authors: Miralles, M. P.; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2002AGUFMSH52A0451M
Altcode:
  The Ultraviolet Coronagraph Spectrometer (UVCS) aboard SOHO has been
  collecting spectroscopic data from numerous coronal holes as part of
  an ongoing campaign to determine the plasma properties of the solar
  wind acceleration region throughout the current solar cycle. The
  UVCS observations show marked variations of ion properties (in the
  acceleration region of the high-speed solar wind) in different types of
  coronal holes. We present empirical models for the physical properties
  of large coronal holes and the acceleration of the associated high-speed
  solar wind derived from ultraviolet coronagraphic spectroscopy. We
  discuss the role of solar cycle trends and the variation of ambient
  coronal-hole properties (e.g., magnetic field, geometry, density). We
  use these observations to test phenomenological models of coronal
  heating and solar wind acceleration. This work is supported by NASA
  under Grant NAG5-11420 to the Smithsonian Astrophysical Observatory,
  by the Italian Space Agency and by PRODEX (Swiss contribution).

Title: Cyclical variations in the plasma properties of coronal holes
Authors: Miralles, M. P.; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2002ESASP.508..351M
Altcode: 2002soho...11..351M
  UVCS/SOHO has been used to measure the plasma properties of several
  types of coronal holes from 1996 to early 2002 at heights from
  1.5 to 3.5 R<SUB>solar</SUB>. UVCS observations show a variation
  in ion properties between coronal holes from solar minimum to solar
  maximum. Different coronal holes seem to exhibit different heating and
  acceleration rates. Polar coronal holes at solar minimum exhibited
  the most extreme ion properties with O<SUP>5+</SUP> perpendicular
  temperatures in excess of 2×10<SUP>8</SUP>K, O<SUP>5+</SUP> outflow
  speeds of at least 400 km/s by 3 R<SUB>solar</SUB>, and the lowest
  densities. Equatorial coronal holes at solar maximum exhibited the
  least extreme ion plasma properties with O<SUP>5+</SUP> perpendicular
  temperatures less than 8×10<SUP>7</SUP>K, O<SUP>5+</SUP> outflow
  speeds of only 100 km/s by 3 R<SUB>solar</SUB>, and the largest
  densities. However, large polar and equatorial coronal holes produce
  interplanetary wind streams with similar speeds (v ~ 700 km/s). Thus,
  most of the solar wind acceleration in large equatorial coronal
  holes must occur above 3 R<SUB>solar</SUB>. The first high-latitude
  coronal hole of the new negative magnetic polarity observed at the
  north in 2001 exhibited extreme properties similar to those of the
  1996 - 1997 polar coronal holes, even though it was 6 years prior to
  the next minimum. During 2001 - 2002, we have observed mid-latitude
  coronal holes, with properties in between large polar and equatorial
  coronal holes.

Title: Empirical Densities, Kinetic Temperatures, and Outflow
    Velocities in the Equatorial Streamer Belt at Solar Minimum
Authors: Strachan, L.; Suleiman, R.; Panasyuk, A. V.; Biesecker,
   D. A.; Kohl, J. L.
Bibcode: 2002ApJ...571.1008S
Altcode:
  We use combined Ultraviolet Coronagraph Spectrometer and Large Angle
  Spectroscopic Coronagraph data to determine the O<SUP>5+</SUP>
  outflow velocities as a function of height along the axis of an
  equatorial streamer at solar minimum and as a function of latitude
  (at 2.3 R<SUB>solar</SUB> from Sun center). The results show that
  outflow increases rather abruptly in the region between 3.6 and 4.1
  R<SUB>solar</SUB> near the streamer cusp and gradually increases to ~90
  km s<SUP>-1</SUP> at ~5 R<SUB>solar</SUB> in the streamer stalk beyond
  the cusp. The latitudinal variation at 2.3 R<SUB>solar</SUB> shows that
  there is no outflow (within the measurement uncertainties) in the center
  of the streamer, called the core, and that a steep increase in outflow
  occurs just beyond the streamer legs, where the O VI λ1032 intensity
  relative to H I λ1216 (Lyα) is higher than in the core. Velocity
  variations in both height and latitude show that the transitions from
  no measurable outflow to positive outflow are relatively sharp and thus
  can be used to infer the location of the transition from closed to open
  field lines in streamer magnetic field topologies. Such information,
  including the densities and kinetic temperatures derived from the
  observations, provides hard constraints for realistic theoretical
  models of streamers and the source regions of the slow solar wind.

Title: Empirically Determined Anisotropic Velocity Distributions
    and Outflows of O<SUP>5+</SUP>\ Ions in a Coronal Streamer at
    Solar Minimum
Authors: Frazin, R. A.; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2002AAS...200.1601F
Altcode: 2002BAAS...34..667F
  Empirical constraints on the O<SUP>5+</SUP>\ velocity distributions
  and outflow speeds in a solar minimum equatorial streamer between 2.6
  and 5.1 R<SUB>sun</SUB>\ are determined using a spectral synthesis
  code that includes O VI Doppler dimming. These constraints follow
  directly from UV spectra taken on 12 October 1996 with the Ultraviolet
  Coronagraph Spectrometer (UVCS) on the SOHO satellite and 3D electron
  densities derived from tomography applied to a time series of polarized
  white-light images taken with the Large Angle Spectrometric Coronagraph
  Experiment (LASCO) on SOHO. Four conclusions result from this work: 1)
  Our analysis shows O<SUP>5+</SUP>\ velocity distribution anisotropy
  in the streamer legs and stalk and that the microscopic velocity
  distribution (which excludes wave motions that equally affect all
  charged particles) is also anisotropic, where the most probable
  speed perpendicular to the magnetic field direction exceeds that in
  the parallel direction. 2) There is no evidence of anisotropy in the
  streamer core. 3) There is preferential heating of the O<SUP>5+</SUP>\
  ions over the protons in the streamer stalk and legs, but not in the
  core. 4) The outflow velocity of the O<SUP>5+</SUP>\ ions is determined
  at heights above 4.6 R<SUB>sun</SUB>. All results have a confidence
  level of at least 70%. The evidence for microscopic anisotropy in the
  O<SUP>5+</SUP>\ velocity distributions and preferential heating of the
  O<SUP>5+</SUP>\ ions over the protons presented here is reminiscent
  of that provided for coronal holes by Cranmer et al. (1999). One
  particularly favorable candidate mechanism to explain these phenomena
  is ion cyclotron resonance, in which high frequency Alfvén waves
  are absorbed by the heavy ions. Cranmer et al. discuss the relevance
  of this process to an empirical model of a polar coronal hole. Our
  data suggest that the dominant processes that heat the heavy ions in
  coronal holes may also be important in streamers. Reference: Cranmer,
  S.R., et al. 1999, ApJ, 511, 481

Title: Empirical densities, kinetic temperatures, and outflow
    velocities in the equatorial streamer belt at solar minimum
Authors: Strachan, L.; Suleiman, R.; Panasyuk, A. V.; Biesecker,
   D. A.; Kohl, J. L.
Bibcode: 2002AAS...200.5715S
Altcode: 2002BAAS...34..739S
  We use combined Ultraviolet Coronagraph Spectrometer (UVCS) and Large
  Angle Spectroscopic Coronagraph (LASCO) data to determine the O(5+)
  outflow velocities as a function of height along the axis of an
  equatorial streamer at solar minimum and as a function of latitude
  (at 2.3 solar radii from sun center). The results show that outflow
  increases rather abruptly in the region between 3.6 and 4.1 solar radii
  near the streamer cusp, and gradually increases to 90 km/s at about
  5 solar radii in the streamer stalk beyond the cusp. The latitudinal
  variation at 2.3 solar radii shows that there is no outflow (within
  the measurement uncertainties) in the center of the streamer called
  the core, and that a steep increase in outflow occurs just beyond the
  streamer legs, where the O VI 1032 intensity relative to H I 1216 (Ly
  alpha) is higer than in the core. Velocity variations in both height
  and latitude show that the transitions from no measurable outflow to
  positive outflow are relatively sharp and thus can be used to infer the
  location of the transition from closed to open field lines in streamer
  magnetic field topologies. Such information, including the densities
  and kinetic temperatures derived from the observations, provides
  hard constraints for realistic theoretical models of streamers and
  the source regions of the slow solar wind. This work is supported by
  NASA Grant NAG5-11420 to the Smithsonian Astrophysical Observatory,
  by the Italian Space Agency, and by the ESA PRODEX program (Swiss
  contribution). do not accept author defined LaTeX macros.

Title: Empirically Determined Anisotropic Velocity Distributions
    and Outflows of O<SUP>5+</SUP>\ ions in a Coronal Streamer at
    Solar Minimum
Authors: Frazin, R. A.; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2002AGUSMSH21B..06F
Altcode:
  Empirical constraints on the O<SUP>5+</SUP>\ velocity distributions
  and outflow speeds in a solar minimum equatorial streamer between 2.6
  and 5.1 R<SUB>sun</SUB>\ are determined using a spectral synthesis
  code that includes O VI Doppler dimming. These constraints follow
  directly from UV spectra taken on 12 October 1996 with the Ultraviolet
  Coronagraph Spectrometer (UVCS) on the SOHO satellite and 3D electron
  densities derived from tomography applied to a time series of polarized
  white-light images taken with the Large Angle Spectrometric Coronagraph
  Experiment (LASCO) on SOHO. Four conclusions result from this work:
  1) Our analysis shows O<SUP>5+</SUP>\ anisotropy in the streamer legs
  and stalk. The microscopic velocity distribution (which excludes wave
  motions that equally affect all charged particles) is also found to
  be anisotropic, where the most probable speed perpendicular to the
  magnetic field direction exceeds that in the parallel direction. 2)
  There is no evidence of such anisotropy in the streamer core. 3)
  There is preferential heating of the O<SUP>5+</SUP>ions over the
  protons in the streamer stalk and legs, but not in the core. 4) The
  outflow velocity of the O<SUP>5+</SUP>\ ions is determined at heights
  above 4.6 R<SUB>sun</SUB>. This work is supported by NASA under grant
  NAG5-10093 to the Smithsonian Astrophysical Observatory.

Title: The Helium Focusing Cone of the Local Interstellar Medium
    Close to the Sun
Authors: Michels, J. G.; Raymond, J. C.; Bertaux, J. L.; Quémerais,
   E.; Lallement, R.; Ko, Y. -K.; Spadaro, D.; Gardner, L. D.; Giordano,
   S.; O'Neal, R.; Fineschi, S.; Kohl, J. L.; Benna, C.; Ciaravella,
   A.; Romoli, M.; Judge, D.
Bibcode: 2002ApJ...568..385M
Altcode:
  The Solar and Heliospheric Observatory (SOHO) Ultraviolet Coronagraph
  Spectrometer is used to observe the interplanetary He focusing cone
  within 1 AU. Taken over 2 yr and from differing orbit positions, the
  series of observations includes measurements of He I 584 Å and Lyβ
  intensities. The cone itself is spatially well defined, and the He I
  intensity within the cone was ~45 R in 1996 December, compared with
  ~1 R for lines of sight outward from 1 AU. Between 1996 December and
  1998 June, the focusing cone dimmed by a factor of 3.3 as the level of
  solar activity rose. This is the first time that interstellar helium
  is observed so near the Sun. Measured intensities are compared to a
  detailed temperature and density model of interstellar helium in the
  solar system. The model includes EUV ionization but does not include
  ionization by electron impact from solar wind electrons. There are
  several features in the data model comparison that we attribute to
  the absence of electron impact ionization in the model. The absolute
  maximum intensity of 45 R first measured in 1996 December calls for
  an ionization 45% more intense than the EUV photoionization alone as
  measured by the Solar EUV Monitor/Charge, Element, and Isotope Analysis
  System (SEM/CELIAS) on SOHO. Important day-to-day variations of the
  intensity are observed, as well as a general decrease as the solar
  activity rises (both absolute and divided by a model with a constant
  ionization). This general decrease is even larger than predicted by a
  model run with the SEM/CELIAS photoionization rate alone, in spite of a
  factor of 1.5 increase of this rate from 1996 December to 1998 June. At
  this time, an additional ionization rate of 0.56×10<SUP>-7</SUP>
  s<SUP>-1</SUP> (compared with 1.00×10<SUP>-7</SUP> s<SUP>-1</SUP> from
  solar EUV) is required to fit the measured low intensity. We attribute
  this additional rate to solar wind electron impact ionization of the
  atoms. This shows that the helium intensity pattern is a very sensitive
  indicator of the electron density and temperature near the Sun.

Title: Far-Ultraviolet Observations of Comet 2P/Encke at Perihelion
Authors: Raymond, J. C.; Uzzo, M.; Ko, Y. -K.; Mancuso, S.; Wu, R.;
   Gardner, L.; Kohl, J. L.; Marsden, B.; Smith, P. L.
Bibcode: 2002ApJ...564.1054R
Altcode:
  Comet 2P/Encke was observed with UVCS/SOHO near perihelion (2000
  September 9 and 11) in the Lyman lines of hydrogen. We present a Lyα
  image reconstructed from a series of long-slit spectra, along with
  the intensity ratios of Lyα, Lyβ, and Lyγ. The narrow Lyα profile
  indicates that the observed photons are scattered from hydrogen atoms
  produced by dissociation of H<SUB>2</SUB>O and OH, though a broader
  profile far from the coma suggests a contribution from hydrogen atoms
  produced by charge transfer with solar wind protons. The outgassing rate
  derived from the Lyα intensity distribution is in excellent agreement
  with Sekanina's model of two active vents. We also present upper limits
  for the outgassing rates of the noble gases helium, neon, and argon.

Title: White Light Intercalibrations of UVCS, LASCO-C2 and Spartan
    201/WLC
Authors: Frazin, R. A.; Romoli, M.; Kohl, J. L.; Gardner, L. D.;
   Wang, D.; Howard, R. A.; Kucera, T. A.
Bibcode: 2002ISSIR...2..249F
Altcode: 2002ESASR...2..249F; 2002rcs..conf..249F
  This paper describes comparisons among white light polarized radiances
  (pB) as measured by the Ultraviolet Coronagraph Spectrometer White
  Light Channel (UVCS/WLC), the Large Angle and Spectrometric Coronagraph
  Experiment C2 instrument (LASCOC2) and the Spartan 201 White Light
  Coronagraph (Spartan 201/WLC). UVCS/WLC and LASCO-C2 are generally in
  agreement, although there are some systematic trends and discrepancies
  that still require explanation. UVCS/WLC and Spartan 201/WLC agree
  to within the measurement uncertainties. Spartan 201/WLC and LASCO-C2
  are not directly compared to each other in this paper.

Title: Empirical outflow velocities in an equatorial coronal streamer
Authors: Strachan, L.; Suleiman, R.; Panasyuk, A.; Biesecker, D.;
   Kohl, J.
Bibcode: 2002cosp...34E1120S
Altcode: 2002cosp.meetE1120S
  We use combined Ultraviolet Coronagraph Spectrometer (UVCS) and Large
  Angle Spectroscopic Coronagraph (LASCO) data to determine the O5+
  outflow velocities as a function of height along the axis of an
  equatorial streamer at solar minimum and as a function of latitude
  (at 2.3 solar radii from sun center). The results show that outflow
  increases rather abruptly in the region between 3.6 and 4.1 solar radii
  near the streamer cusp, and gradually increases to 90 km/s at about
  5 solar radii in the streamer stalk beyond the cusp. The latitudinal
  variation at 2.3 solar radii shows that there is no outflow (within
  the measurement uncertainties) in the center of the streamer called
  the core, and that a steep increase in outflow occurs just beyond
  the streamer legs, where the O VI 1032 intensity relative to H I 1216
  (Ly) is higher than in the core. Velocity variations in both height
  and latitude show that the transitions from no measurable outflow to
  positive outflow are relatively sharp and thus can be used to infer the
  location of the transition from closed to open field lines in streamer
  magnetic field topologies. Such information, including the densities
  and kinetic temperatures derived from the observations, provides hard
  constraints for realistic theoretical models of streamers and the source
  regions of the slow solar wind. This work is supported by NASA Grant
  NAG5-11420 to the Smithsonian Astrophysical Observatory, by the Italian
  Space Agency, and by the ESA PRODEX program (Swiss contribution).

Title: UVCS/SOHO observations of a CME-driven shock: Consequences
    on ion heating mechanisms behind a coronal shock
Authors: Mancuso, S.; Raymond, J. C.; Kohl, J.; Ko, Y. -K.; Uzzo,
   M.; Wu, R.
Bibcode: 2002A&A...383..267M
Altcode:
  We report the observation of a 1100 km s<SUP>-1</SUP> CME-driven
  shock with the UltraViolet Coronagraph Spectrometer (UVCS) telescope
  operating on board SOHO on March 3, 2000. The shock speed was derived
  from the type II radio burst drift rate and from UVCS observations
  that can yield the density profile just before the passage of the
  shock. A CME projected speed of 920 km s<SUP>-1</SUP> was deduced
  from the Large Angle Spectrometric Coronagraph (LASCO) white light
  images, indicating that the CME leading edge was lagging behind at
  about 20% of the shock speed. The spectral profiles of both the O VI
  and Lyalpha lines were Doppler dimmed and broadened at the passage
  of the shock by the emission from shocked material along the line of
  sight. The observed line broadening for both protons and oxygen ions
  was modeled by adopting a mechanism in which the heating is due to the
  nondeflection of the ions at the shock ramp in a quasi-perpendicular
  shock wave. This specific ion heating model was able to reproduce the
  observed spectroscopic properties of the shocked plasma.

Title: Low-latitude Coronal Holes during Solar Maximum
Authors: Miralles, M.; Cranmer, S.; Kohl, J.
Bibcode: 2002cosp...34E1125M
Altcode: 2002cosp.meetE1125M
  Analyses of in situ observations have shown that some small coronal
  holes are sources of slow solar wind near solar maximum when
  polar coronal holes become smaller and disappear. However, not all
  coronal holes at solar maximum produce slow wind. The Ultraviolet
  Coronagraph Spectrometer (UVCS) aboard SOHO has been used to observe
  large low-latitude coronal holes during solar maximum that produced
  fast solar wind. UVCS observations show that large equatorial holes
  at solar maximum have plasma properties that seem to bridge the gap
  between solar minimum polar coronal holes and streamers. The ion kinetic
  temperatures in equatorial holes are about 2 times larger than those in
  a solar minimum equatorial streamer, and about a factor of 2 smaller
  than those in polar coronal holes above 2 R . The outflow speeds for
  the large equatorial holes observed by UVCS are only about 100 km s-1
  , a factor of 4 smaller than those in polar holes, at 3 R . However,
  in situ data corresponding to these equatorial coronal holes showed
  asymptotic wind speeds of 600-700 km s-1 . These wind speeds are similar
  to those observed over polar coronal holes at solar minimum. In contrast
  to the polar coronal holes, the bulk of the solar wind acceleration
  in large equatorial coronal holes at solar maximum must occur above
  3 R . Thus, the combination of spectroscopic measurements in the
  extended corona, where the primary solar wind acceleration occurs, and
  in situ measurements made in the solar wind can be used to obtain the
  solar wind acceleration as a function of heliocentric distance. These
  observations provide detailed empirical constraints for theoretical
  models and may be key to understanding how the various types of solar
  wind plasma are heated and accelerated. This work is supported by NASA
  under Grant NAG5-11420 to the Smithsonian Astrophysical Observatory,
  by the Italian Space Agency and by PRODEX (Swiss contribution).

Title: In-flight Calibration of the UVCS White Light Channel
Authors: Romoli, M.; Frazin, R. A.; Kohl, J. L.; Gardner, L. D.;
   Cranmer, S. R.; Reardon, K.; Fineschi, S.
Bibcode: 2002ISSIR...2..181R
Altcode: 2002ESASR...2..181R; 2002rcs..conf..181R
  The UVCS White Light Channel (WLC) is designed to measure the linearly
  polarized radiance (pB) of the corona, in the wavelength band from 450
  nm to 600 nm, in order to derive one of the fundamental parameters of
  the solar corona: the electron density. This paper gives a thorough
  description of the in-flight radiometric calibration of the WLC, which
  uses the star α Leo and the planet Jupiter as transfer standards
  and is based on calibrations of ground-based instruments. The
  method for computing the polarized radiance from the measurements
  is also described, together with the stray light and polarization
  characterizations obtained from dedicated, in-flight measurements.

Title: UV Radiometric Calibration of UVCS
Authors: Gardner, L. D.; Smith, P. L.; Kohl, J. L.; Atkins, N.;
   Ciaravella, A.; Miralles, M. P.; Panasyuk, A.; Raymond, J. C.;
   Strachan, L., Jr.; Suleiman, R. M.; Romoli, M.; Fineschi, S.
Bibcode: 2002ISSIR...2..161G
Altcode: 2002ESASR...2..161G; 2002rcs..conf..161G
  The Ultraviolet Coronagraph Spectrometer (UVCS) was characterized
  and radiometrically calibrated in the laboratory as a system at the
  Harvard-Smithsonian Center for Astrophysics in June of 1995. Component
  level calibrations of optical components and detectors were also
  performed. After launch, an in-flight calibration activity was carried
  out that extended the laboratory calibration, compared UVCS measurements
  of stars to those of other instruments and monitored the radiometric
  stability of UVCS through repeated measurements of stars that are
  believed to have nearly constant ultraviolet irradiance. In-flight
  measurements have, in general, confirmed the laboratory radiometric
  calibration. Comparisons to Spartan 201 observations of the same coronal
  structures agree within 10 %. The system responsivity, although it has
  changed somewhat during the six years of operation, is well behaved
  and characterizable. This paper describes the UVCS calibration and
  its results.

Title: UVCS/SOHO Observations of Coronal Holes from Solar Minimum
    to Solar Maximum
Authors: Miralles, M. P.; Cranmer, S. R.; Esser, R.; Kohl, J. L.
Bibcode: 2001AGUFMSH32A0721M
Altcode:
  Coronal holes are open field, low-density source regions of the solar
  wind. At solar minimum, large coronal holes are present at the poles
  and are the dominant source of the solar wind flow for this part of
  the solar cycle. At solar maximum, coronal holes of varying sizes and
  shapes appear at all latitudes and last for several rotations. During
  this stage of the cycle, the dominant component is mainly slow wind,
  but fast wind streams are generated by large coronal holes. UVCS/SOHO
  has been used to measure the plasma properties in several types
  of coronal holes from 1996 to 2001. Spectroscopic diagnostics of
  O<SUP>5+</SUP> velocity distributions and outflow velocities are
  derived from measurements of intensities and line widths for O~VI
  103.2 and 103.7 nm as a function of height. We compare the plasma
  properties of coronal holes from solar minimum to solar maximum and
  discuss the evolution of coronal holes during the solar cycle. We
  also study the compatibility between the growing database of coronal
  hole plasma properties and theoretical models of extended coronal
  heating via ion cyclotron resonance. This work is supported by NASA
  under Grant NAG5-10093 to the Smithsonian Astrophysical Observatory,
  by the Italian Space Agency and by PRODEX (Swiss contribution).

Title: Modelling of a CME-driven Shock Detected by UVCS/SoHO on
    March 3, 2000
Authors: Mancuso, S.; Raymond, J. C.; Kohl, J. L.; Ko, Y.; Uzzo, M.;
   Wu, R.
Bibcode: 2001AGUFMSH21B..05M
Altcode:
  We report the observation of a 1100 km/s CME-driven shock with the
  UltraViolet Coronagraph Spectrometer (UVCS) telescope operating on
  board SoHO on March 3, 2000. The CME was observed by the Large Angle
  Spectroscopic Coronagraph (LASCO), and the radio signature of the
  shock was detected by the Hiraiso and Culgoora radio spectrographs as
  an intense type II radio burst. We derived the density profile just
  before the passage of the shock from UVCS observations and obtained
  a reliable estimate of the shock speed from the type II radio burst
  drift rate. The spectral profiles of both the O VI and Lyman alpha
  lines were Doppler dimmed at the passage of the shock and showed broad
  wings caused by the emission from shocked material along the line
  of sight. By estimating a compression ratio of 1.8 from the observed
  splitting of the radio emission bands in the spectrographs and assuming
  perpendicular propagation of the shock we derive a magnetic field
  strength of 1 Gauss at 1.8 solar radii and an Alfvenic Mach number of
  1.7. The observed line broadening for both the protons and the Oxygen
  ions was modeled by adopting a mechanism in which the heating is due
  to the nondeflection of the ions at the shock ramp.

Title: The Advanced Spectroscopic and Coronagraphic Explorer Mission
Authors: Kohl, J. L.; Howard, R.; Davila, J.; Noci, G.; Esser, R.;
   Ciaravella, A.; Cranmer, S.; Fineschi, S.; Gardner, L.; Raymond, J.;
   Romoli, M.; Smith, P.; Socker, D.; Strachan, L.; Van Ballegooijen, A.
Bibcode: 2001AGUFMSH31B0711K
Altcode:
  SOHO has provided profound insights into the physics of solar wind
  acceleration and coronal mass ejections. Although significant
  progress has been made, most of the dominant physical processes
  controlling these phenomena are still not identified. The Advanced
  Spectroscopic and Coronagraphic Explorer Mission provides next
  generation spectroscopic and polarimetric instrumentation aimed at
  identifying these processes. The launch is planned for March 2007 with
  mission operations and data analysis continuing for 5 years. The data
  will be unrestricted and available to the community. The envisioned
  program includes a Guest Investigator Program with an average of 15
  grants to be awarded in response to proposals submitted during the
  first year of the mission. Information about the proposed scientific
  goals and instrumentation will be presented.

Title: Polarized Intensity Measurements of the Corona during the 21
    June 2001 Total Solar Eclipse
Authors: Habbal, S. R.; Arnaud, J.; Johnson, J.; Hegwer, S.; Ene, A.;
   Hale, J.; Esser, R.; Arndt, M.; Kohl, J. L.; Daw, A.; Faurobert, M.;
   Woo, R.; Habbal, F.; Havasy, R.; Alford, J. N.
Bibcode: 2001AGUFMSH11C0716H
Altcode:
  We report on the first successful simultaneous polarimetric measurements
  of the brightness of the Thompson-scattered white light and intensity
  of the near-infrared Fe XIII 10747 Å line, the strongest of the
  coronal iron forbidden lines. These observations which extended out
  to 3 R<SUB>s</SUB> in the corona were obtained during the total solar
  eclipse of 21 June 2001. The novel technique used to acquire these
  measurements will be presented. Polarized intensity measurements of the
  resonantly scattered component of coronal emission lines are the only
  tools to date that can yield the direction of the coronal magnetic
  field. Through these simultaneous measurements, we show how the
  direction of the coronal magnetic field can be placed in the context
  of coronal density structures. We also discuss the implications of
  these simultaneous measurements for the source of the solar wind.

Title: SOHO Ultraviolet Coronagraph Spectrometer (UVCS) Mission
    Operations and Data Analysis
Authors: Kohl, John L.
Bibcode: 2001STIN...0212280K
Altcode:
  The scientific goal of Ultraviolet Coronagraph Spectrometer (UVCS)
  is to obtain detailed empirical descriptions of the extended
  solar corona as it evolves through the solar activity cycle and
  to use those descriptions to identify and understand the physical
  processes responsible for coronal heating, solar wind acceleration,
  coronal mass ejections (CMEs), and the phenomena that establish the
  plasma properties of the solar wind as measured by 'in situ' solar
  wind instruments. The UVCS on the Solar and Heliospheric Observatory
  (SOHO) has made major advances in identifying the physical processes
  responsible for solar wind acceleration, and it has made the first
  high resolution ultraviolet spectroscopic measurements of CMEs. The
  UVCS has resulted in over 220 scientific publications.

Title: Ultraviolet Coronagraph Spectrometer Observations of a
    High-Latitude Coronal Hole with High Oxygen Temperatures and the
    Next Solar Cycle Polarity
Authors: Miralles, M. P.; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2001ApJ...560L.193M
Altcode:
  We announce the resurgence of extreme ion properties in a large,
  high-latitude coronal hole observed above the north heliographic pole
  in 2001 February at solar maximum. The observations were taken with
  the Ultraviolet Coronagraph Spectrometer on the Solar and Heliospheric
  Observatory. These observations are part of an ongoing campaign to
  determine the plasma properties of coronal holes during the current
  solar cycle. In this Letter, we compare the observations and analysis
  of O VI λλ1032, 1037 spectral lines of a high-latitude coronal hole
  in 2001 with observations of an equatorial solar maximum hole in 1999
  and polar coronal holes observed near solar minimum (1996-1997). These
  lines provide spectroscopic diagnostics of O<SUP>+5</SUP> velocity
  distributions and outflow velocities. The O VI line profiles show
  a narrow core and broad wings. The narrow core is attributed to
  foreground and background streamers and, possibly, dense polar plumes
  at the lowest observed heights. The broad wings are attributed to the
  coronal hole. The comparison of the coronal hole line widths shows
  that the O<SUP>+5</SUP> perpendicular kinetic temperatures in the 2001
  high-latitude hole are similar to those observed in polar coronal holes
  at solar minimum. These observations of extremely high ion kinetic
  temperatures (exceeding 10<SUP>8</SUP> K) at the north pole in 2001
  occurred nearly simultaneously with the polarity change of the Sun's
  magnetic field, as seen in recent magnetogram data. This coronal hole
  in 2001 may represent the first manifestation of the negative polarity
  polar coronal holes that will dominate the Sun's open magnetic flux
  tubes at the next solar minimum. The reappearance of broad O VI
  profiles at a time when not all of the ``new polarity'' magnetic
  flux has migrated to the poles was an interesting development. The
  variations in coronal hole parameters with the solar cycle provide
  constraints on models of extended coronal heating.

Title: Solar Cycle 23: Variation of the Solar Corona in the
    Ultraviolet from Solar Minimum to Solar Maximum
Authors: Miralles, M. P.; Panasyuk, A. V.; Strachan, L.; Gardner,
   L. D.; Suleiman, R.; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2001iscs.symp...59M
Altcode:
  UVCS/SOHO measurements of H I Ly-alpha and O VI (103.2 nm and 103.7 nm)
  intensities in the solar corona have been made from solar Cycle 23's
  minimum in 1996 to its current maximum. At solar minimum, the corona
  consisted of large coronal holes at the poles and quiescent streamers at
  the equator. During the approach to solar maximum, equatorial coronal
  holes and high latitude streamers became more conspicuous. Recently,
  coronal holes at higher latitudes have reappeared, allowing a comparison
  to be made of O VI intensities and line widths of coronal holes at
  different latitudes. We also characterize the variation of coronal
  hole properties with height, and location over the solar cycle. This
  work is supported by NASA under Grant NAG5-10093 to the Smithsonian
  Astrophysical Observatory, by the Italian Space Agency and by PRODEX
  (Swiss contribution)

Title: Observations of a High-latitude Coronal Hole at Solar Maximum
Authors: Miralles, M.; Cranmer, S. R.; Kohl, J. L.
Bibcode: 2001AGUSM..SH21B07M
Altcode:
  A large coronal hole at a latitude of about 60 degrees was observed
  above the north pole with the Ultraviolet Coronagraph Spectrometer
  (UVCS) aboard SOHO during 10--19 February 2001. These observations
  are part of an ongoing campaign to characterize equatorial and
  mid-latitude coronal holes during the active phase of the current
  solar cycle. Observations in H~I Lyα and O~VI 103.2 and 103.7 nm
  provided spectroscopic diagnostics of proton and O<SUP>5+</SUP>
  velocity distributions. The O~VI line profiles show a narrow core
  and broad wings. The narrow core is attributed to the foreground and
  background streamers. The broad wings are attributed to the coronal
  hole. We compare the observed line intensities and widths of this
  high-latitude hole with those of other solar maximum (lower latitude)
  holes and solar minimum polar coronal holes. The comparison of the
  line widths shows that the O~VI line widths of this solar maximum
  hole are similar to those observed in polar coronal holes at solar
  minimum. The observation of extremely high ion kinetic temperatures at
  the north pole occurs simultaneously with the polarity change of the
  Sun's magnetic field, as seen in recent magnetogram data. This coronal
  hole may represent the first manifestation of the stable polar coronal
  holes that will dominate the Sun's open magnetic flux tubes at the next
  solar minimum. The re-appearance of broad O~VI profiles at a time when
  not all of the ``new polarity'' magnetic flux has migrated to the poles
  is an interesting development that may provide a crucial constraint
  on models of extended coronal heating. This work is supported by NASA
  under Grant NAG5-10093 to the Smithsonian Astrophysical Observatory,
  by the Italian Space Agency and by PRODEX (Swiss contribution).

Title: Observed Variations of O<SUP>5+</SUP> Velocity Distributions
    with Electron Density
Authors: Kohl, J. L.; Cranmer, S. R.; Frazin, R. A.; Miralles, M.;
   Strachan, L.
Bibcode: 2001AGUSM..SH21B08K
Altcode:
  The Ultraviolet Coronagraph Spectrometer (UVCS) on the SOHO satellite
  has been used to measure the line profiles of O~VI 103.2 and 103.7
  nm versus heliographic height in a variety of coronal holes and
  streamers during the period from 1996 to 2001. Those observations
  have been used to derive velocity distributions in the line-of-sight
  direction, which is typically perpendicular to the apparent magnetic
  field direction. In the case of polar coronal holes at solar minimum,
  the electron density is the smallest observed and the most-probable
  speed is the largest observed reaching values as high as 500 km/s at the
  largest heights. The O<SUP>5+</SUP> most-probable speed is much larger
  than the hydrogen speed in those structures. The ratio of O<SUP>5+</SUP>
  to hydrogen most-probable speeds increases with height. In contrast,
  the O<SUP>5+</SUP> values are much smaller than those of hydrogen at
  the base of high-latitude streamers and never reach the hydrogen values
  at any observed height. The electron density in those structures is
  much greater than in the solar minimum coronal holes. Other structures
  have intermediate values of the electron density and O<SUP>5+</SUP>
  most-probable speeds. In general, the O<SUP>5+</SUP> most-probable speed
  and its ratio to the hydrogen value seem to decrease with increasing
  density. This apparent observational correlation may be related to
  thermalization from higher collision rates or it might be related to the
  physical process that causes the extreme O<SUP>5+</SUP> perpendicular
  heating. This work is supported by NASA under Grant NAG5-10093 to the
  Smithsonian Astrophysical Observatory, by the Italian Space Agency,
  and by PRODEX (Swiss Contribution).

Title: Where in the Streamer Belt does the Slow Speed Wind Originate?
Authors: Strachan, L.; Suleiman, R.; Panasyuk, A. V.; Biesecker,
   D. A.; Kohl, J. L.
Bibcode: 2001AGUSM..SH41B07S
Altcode:
  The Ulysses high latitude mission showed that the slow speed wind at
  solar minimum appears to come from equatorial regions in the heliosphere
  that are dominated by helmet streamers. However, there are few coronal
  measurements of the detailed latitudinal variation of the outflow
  velocity across a streamer. Such measurements are needed to identify the
  region of the streamer that gives rise to the slow speed wind. For this
  study we use UVCS and LASCO observations of a solar minimum streamer to
  make a detailed model of the outflow velocities for O<SUP>+5</SUP> as
  a function of position angle from the streamer axis. This new work goes
  beyond using the OVI line ratios to define the boundaries between fast
  and slow wind. We constrain the coronal plasma parameters (velocities,
  temperature anisotropies, densities, etc.) using OVI and Ly-alpha line
  profiles, and white light polarized brightness data. We will discuss
  various possibilities for the latitudinal profile for the coronal
  outflow in the streamer belt. This work is supported by NASA Grant
  NAG5-7822 to the Smithsonian Astrophysical Observatory, by the Italian
  Space Agency, and by the ESA PRODEX program (Swiss contribution).

Title: Coordinated UVCS/LASCO/EIT Observations of a High Latitude CME
Authors: Karovska, M.; Esser, R.; Dobrzycka, D.; Kohl, J.
Bibcode: 2001AGUSM..SH22A10K
Altcode:
  We present here the results of our coordinated UVCS/LASCO/EIT
  observations of a CME on 2000 March 5. The northern polar region of
  the Sun at a position angle 270 degrees was monitored with UVCS at 2
  solar radii for about 8 hours. During that time interval a spectacular
  CME developed in the northern hemisphere. This event was also detected
  and monitored with LASCO C2 and C3 and the EIT for several hours. We
  compare the edge-enhanced LASCO and EIT images of this event with the
  increased intensities of the H I Lyman-alpha spectral line and the line
  pair O VI 1031.91 A and 1037.61 A seen in the UVCS observations. LASCO
  and EIT images are essential in providing the larger scale context for
  this event and for correlating the small-scale sub-structure observed
  in white light with the the plasma morphology as observed with the UVCS.

Title: Plasma Conditions in Polar Plumes and Interplume Regions in
    Polar Coronal Holes
Authors: Cranmer, S. R.; Kohl, J. L.; Miralles, M.; Panasyuk, A. V.
Bibcode: 2001AGUSM..SH41B08C
Altcode:
  During times of low solar activity, large polar coronal holes are
  observed to contain bright raylike polar plumes that appear to follow
  open magnetic field lines. Plumes are believed to be flux tubes that
  are heated impulsively at their base, which leads to a higher density,
  a lower outflow speed, and a lower overall temperature in the extended
  corona, compared to the surrounding interplume regions. Despite years
  of white light and spectroscopic observations, though, the differences
  in mass, momentum, and energy flux in plumes and between plumes are not
  known precisely. This poster presents an updated survey of data from the
  Ultraviolet Coronagraph Spectrometer (UVCS), aboard SOHO, that attempts
  to sort out the local plume and interplume conditions. These results
  will be compared with previous analyses that characterized the ``mean''
  plume/interplume coronal hole, averaged over many lines of sight through
  varying concentrations of plumes. Limits on the relative contributions
  of plumes and interplume regions to the high-speed solar wind will be
  determined, with emphasis on the proton outflow speed in the corona
  and at 1 AU. Implications for theoretical models of coronal heating and
  solar wind acceleration will be discussed. This work is supported by the
  National Aeronautics and Space Administration under grant NAG5-10093 to
  the Smithsonian Astrophysical Observatory, by Agenzia Spaziale Italiana,
  and by the Swiss contribution to the ESA PRODEX program.

Title: Comparison of Empirical Models for Polar and Equatorial
    Coronal Holes
Authors: Miralles, M. P.; Cranmer, S. R.; Panasyuk, A. V.; Romoli,
   M.; Kohl, J. L.
Bibcode: 2001ApJ...549L.257M
Altcode:
  We present a self-consistent empirical model for several plasma
  parameters of a large equatorial coronal hole observed on 1999 November
  12 near solar maximum. The model was derived from observations with
  the Ultraviolet Coronagraph Spectrometer on the Solar and Heliospheric
  Observatory. In this Letter, we compare the observations of O VI
  λλ1032, 1037 emission lines with previous observations of a polar
  coronal hole observed near solar minimum. At the time of the 1999
  observations, there was no evidence of large polar coronal holes. The
  resulting empirical model for the equatorial coronal hole describes
  the outflow velocities and most probable speeds for O<SUP>5+</SUP>, and
  we compared the derived ion properties with the empirical model for a
  solar minimum polar coronal hole. The comparison of the empirical models
  shows that the 1999 equatorial hole has lower O<SUP>5+</SUP> outflow
  speeds and perpendicular temperatures than its polar counterpart from
  1996 to 1997 at heights between 2 and 3 R<SUB>solar</SUB>. However,
  in situ asymptotic speeds of the wind streams coming from the
  1996-1997 polar hole and from the 1999 equatorial hole are only ~15%
  different. Thus, the bulk of the solar wind acceleration must occur
  above 3 R<SUB>solar</SUB> for the equatorial coronal hole. The
  equatorial hole also has a higher density than the polar hole at
  similar heights. It is not yet known whether the higher densities
  are responsible for the seeming inhibition of the fast ion outflow
  speeds and extremely large perpendicular temperatures that occur in
  polar coronal holes at solar minimum. We discuss the constraints
  and implications on various theoretical models of coronal heating
  and acceleration.

Title: Efficiency variations of UVCS/SOHO based on laboratory
    measurements of replica gratings
Authors: Gardner, Larry D.; Atkins, Nigel; Fineschi, Silvano; Smith,
   Peter L.; Kohl, John L.; Maccari, L.; Romoli, Marco
Bibcode: 2000SPIE.4139..362G
Altcode:
  We have carried out measurements of efficiency as functions of position
  across the surfaces of replica grating made from the same masters
  as the UVCS/SOHO flight units. Variations in first order efficiency
  which significantly affect the interpretation of UVCS data are found
  along the direction perpendicular to the grooves. Variations are also
  found along the direction parallel to the grooves, but these do not
  seriously affect UVCS data interpretation. The measurements and their
  application to the radiometric calibration of UVCS/SOHO are discussed.

Title: Corongraphic Observations and Analyses of The Ultraviolet
    Solar Corona
Authors: Kohl, John L.
Bibcode: 2000STIN...0014831K
Altcode:
  The activities supported under NASA Grant NAG5-613 included
  the following: 1) reduction and scientific analysis of data from
  three sounding rocket flights of the Rocket Ultraviolet Coronagraph
  Spectrometer, 2) development of ultraviolet spectroscopic diagnostic
  techniques to provide a detailed empirical description of the extended
  solar corona, 3) extensive upgrade of the rocket instrument to
  become the Ultraviolet Coronal Spectrometer (UVCS) for Spartan 201,4)
  instrument scientific calibration and characterization, 5) observation
  planning and mission support for a series of five Spartan 201 missions
  (fully successful except for STS 87 where the Spartan spacecraft was
  not successfully deployed and the instruments were not activated),
  and 6) reduction and scientific analysis of the UVCS/Spartan 201
  observational data. The Ultraviolet Coronal Spectrometer for Spartan
  201 was one unit of a joint payload and the other unit was a White
  Light Coronagraph (WLC) provided by the High Altitude Observatory
  and the Goddard Space Flight Center. The two instruments were used
  in concert to determine plasma parameters describing structures in
  the extended solar corona. They provided data that could be used
  individually or jointly in scientific analyses. The WLC provided
  electron column densities in high spatial resolution and high time
  resolution. UVCS/Spartan provided hydrogen velocity distributions, and
  line of sight hydrogen velocities. The hydrogen intensities from UVCS
  together with the electron densities from WLC were used to determine
  hydrogen outflow velocities. The UVCS also provided O VI intensities
  which were used to develop diagnostics for velocity distributions and
  outflow velocities of minor ions.

Title: UVCS/SOHO Observations of Equatorial and Polar Coronal Holes
Authors: Kohl, J. L.; Miralles, M. P.; Cranmer, S. R.; Suleiman, R. M.
Bibcode: 2000SPD....31.0232K
Altcode: 2000BAAS...32..816K
  A large equatorial coronal hole was observed above the west limb with
  the Ultraviolet Coronagraph Spectrometer (UVCS) on SOHO from November
  1999 to March 2000. Observations in H I Lyα and O VI 103.2, 103.7
  nm provided spectroscopic diagnostics of proton and O<SUP>5+</SUP>
  velocity distributions and outflow velocities. These properties will be
  compared to those of the large polar coronal holes observed near solar
  minimum. The equatorial coronal hole corresponded to a high-speed
  solar wind stream at 1 AU, but there were significant differences
  between the interplanetary properties of this stream and the steady
  high-speed wind seen over the poles at solar minimum. The several
  obvious differences between the two structures in the extended corona
  may be associated with the different densities and magnetic field
  configurations and flux tube expansion factors. Preliminary results
  from a detailed empirical model of the equatorial coronal hole will
  be presented. This work is supported by NASA under Grant NAG5-7822 to
  the Smithsonian Astrophysical Observatory, by the Italian Space Agency
  and by PRODEX (Swiss contribution).

Title: Solar Cycle Variations of O VI and H I Lyman Alpha Intensities
    in the Solar Corona
Authors: Miralles, M. P.; Panasyuk, A. V.; Strachan, L.; Gardner,
   L. D.; Suleiman, R. M.; Smith, P. L.; Kohl, J. L.
Bibcode: 2000SPD....31.0229M
Altcode: 2000BAAS...32..815M
  UVCS/SOHO measurements of O VI (103.2 and 103.7 nm) and H I Lyman alpha
  intensities in the solar corona have been made from 1996 to the present
  spanning the rising phase of cycle 23. During solar minimum the corona
  consisted of large coronal holes at the poles and quiescent streamers
  at the equator. During the ascending phase of the cycle, the corona
  presented high latitude streamers and finally polar streamers as the
  Sun approached solar maximum. Recent observations of the solar corona
  show the presence of coronal holes at the equator and streamers at
  the poles. Our observations provide descriptions of these structures
  over the rising phase of the solar cycle. We compare the properties
  of quiescent equatorial streamers which occurred at solar minimum to
  high latitude and polar streamers observed toward solar maximum. We
  also compare solar minimum polar coronal holes to equatorial coronal
  holes present at solar maximum. We discuss how these results are
  related to the plasma properties. This work is supported by NASA
  under Grant NAG5-7822 to the Smithsonian Astrophysical Observatory,
  by the Italian Space Agency and by PRODEX (Swiss contribution).

Title: Comparison of UVCS and EISCAT observations of a mid- and
    high-latitude streamer during the Third Whole Sun Month Campaign
Authors: Strachan, L.; Panasyuk, A. V.; Kohl, J. L.; Breen, A.
Bibcode: 2000SPD....31.0237S
Altcode: 2000BAAS...32..817S
  We compare the plasma properties of two different streamer regions in
  the extended corona (1.5 to 6 solar radii) with solar wind velocity
  measurements made at larger distances during the Third Whole Sun Month
  Campaign. Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) measurements
  were made of H Ly-alpha intensities and profiles and O VI 1032/1037
  intensities in order to put constraints on the plasma conditions in
  these regions. The UVCS/SOHO measurements were centered at position
  angles 70 deg (CCW from NHP) during 12-21 Sept. 1999 and 190 deg during
  22-25 Sept. 1999. Streamer kinetic temperatures and outflow velocities
  are compared with measurements of outflow velocities determined by
  EISCAT interplanetary scintillation observations at the same position
  angles. The EISCAT measurements showed slow flow above the streamers
  at 25 to 80 solar radii, with steep gradients on the boundaries as
  flow speeds increased above the inter-streamer regions. Comparisons
  of EISCAT measurements from 25-35 solar radii and UVCS/SOHO coronal
  measurements should cast light on the acceleration of the slow solar
  wind. This work is supported by NASA under Grant NAG5-7822 to the
  Smithsonian Astrophysical Observatory, by the Italian Space Agency
  and by PRODEX (Swiss contribution).

Title: UVCS Observations of a High Latitude Streamer From 2-11
    November 1999
Authors: Strachan, L.; Miralles, M. P.; Frazin, R.; Kohl, J. L.
Bibcode: 2000AGUSM..SH42A04S
Altcode:
  A high latitude coronal streamer was observed with the Ultraviolet
  Coronagraph Spectrometer UVCS on SOHO for ten days during the period 2 -
  11 November 1999. The streamer was formed above a filament channel on
  the disk and, at the start of the observations, was located on the east
  limb at a position angle of about 150 deg. During the following ten
  days the streamer moved across the face of the Sun andand presented
  different aspect angles to the observed line of sight. We compare
  UVCS measurements of intensities and line widths of H Ly-alpha and
  O VI profiles obtained from 1.5 to 3.0 solar radii with equatorial
  streamer observations made near solar minimum. This work demonstrates
  that geometry effects are important when interpreting spectroscopic
  observations of coronal structures. In the future these observations
  will be used to model ion velocity distributions and outflow velocities
  in these high latitude streamer structures. This work is supported in
  part by NASA under grant NAG5-7822 to the Smithsonian Astrophysical
  Observatory, by the Italian Space Agency, and by Swiss funding agencies.

Title: New Diagnostics of Coronal Heating and Solar Wind Acceleration
    Processes Achievable With The Advanced Solar Coronal Explorer (ASCE)
Authors: Cranmer, S. R.; Kohl, J. L.; Gardner, L. D.; Raymond, J. C.;
   Strachan, L.; Smith, P. L.; Howard, R. A.; Davila, J. M.; Fisher,
   R. R.; Noci, G.; Tondello, G.; Socker, D. G.; Moses, D.
Bibcode: 2000SPD....31.0297C
Altcode: 2000BAAS...32..828C
  The Advanced Solar Coronal Explorer (ASCE) is a proposed NASA
  Medium-class Explorer (MIDEX) mission that underwent a detailed
  Concept Study in 1999. The science payload includes large aperture EUV
  and visible light coronagraphs. ASCE's unprecedented spectral range,
  spatial resolution, and sensitivity (30 to 100 times the EUV sensitivity
  of UVCS/SOHO) provide measurements needed to investigate the role of
  high-frequency and low-frequency waves in heating and accelerating
  the fast and slow speed solar wind. This presentation will outline
  the advanced capabilities of ASCE for obtaining detailed empirical
  descriptions of solar wind acceleration regions, specifying coronal
  temperatures, flow speeds, densities, and elemental abundances. Velocity
  distributions for electrons and more than 10 to 20 ion species with
  mass-to-charge ratios from 4 to 1 (including singly ionized helium) can
  be measured by ASCE in coronal holes and streamers. This information
  is sufficient to derive the wavenumber power spectrum of magnetic
  fluctuations that affect the primary electron/proton plasma. The main
  goal is to identify the physical processes responsible for heating
  and acceleration of the primary particles and minor ions in the fast
  and slow speed solar wind.

Title: Surf's Still Up: UVCS/SOHO Observations as Strong Constraints
    on Coronal Heating Theories
Authors: Cranmer, S. R.; Kohl, J. L.
Bibcode: 2000SPD....31.1502C
Altcode: 2000BAAS...32..848C
  In 1996, the Ultraviolet Coronagraph Spectrometer (UVCS) instrument
  aboard SOHO observed surprisingly broad line profiles of the O VI 1032,
  1037 doublet in polar coronal holes. These measurements indicated
  perpendicular ion temperatures of at least 100--200 million K above
  two solar radii in the nascent high-speed solar wind. Since then,
  these observations have been supplemented by profiles of other ions,
  Doppler dimming measurements made possible by Spartan 201, and a
  great deal of theoretical work. This talk outlines the current state of
  understanding about coronal heating and solar wind acceleration that has
  been facilitated by UVCS. The most promising mechanism for heating and
  accelerating minor ions remains the dissipation of high-frequency (10 to
  10,000 Hz) ion cyclotron waves, but heating the protons is a more open
  question. The physics of the ion cyclotron interaction in the corona has
  only begun to be explored, and we will discuss recent insights into the
  generation and damping of these waves. A self-consistent theory of wave
  damping and turbulent cascade ``replenishment'' would allow the question
  of proton heating to be answered more definitively. Also, a kinetic
  approach to ion cyclotron heating yields non-bi-Maxwellian ``resonant
  shell'' velocity distributions that could produce emission line profiles
  narrower than expected from their most probable speeds. Thus, the UVCS
  measurements of 100--200 million K ion temperatures may only be lower
  limits. This work is supported by the National Aeronautics and Space
  Administration under grant NAG5-7822 to the Smithsonian Astrophysical
  Observatory, by Agenzia Spaziale Italiana, and by the ESA PRODEX program
  (Swiss contribution).

Title: Identification of the Coronal Sources of the Fast Solar Wind
Authors: Giordano, S.; Antonucci, E.; Noci, G.; Romoli, M.; Kohl, J. L.
Bibcode: 2000ApJ...531L..79G
Altcode: 2000astro.ph..1257G
  The present spectroscopic study of the ultraviolet coronal emission in a
  polar hole, detected on 1996 April 6-9 with the Ultraviolet Coronagraph
  Spectrometer aboard the Solar and Heliospheric Observatory spacecraft,
  identifies the interplume lanes and background coronal hole regions
  as the channels in which the fast solar wind is preferentially
  accelerated. In interplume lanes, at heliocentric distance 1.7
  R<SUB>solar</SUB>, the corona expands at a rate between 105 and 150 km
  s<SUP>-1</SUP>, that is, much faster than in plumes in which the outflow
  velocity is between 0 and 65 km s<SUP>-1</SUP>. The wind velocity is
  inferred from the Doppler dimming of the O VI λλ1032, 1037 lines,
  within a range of values, whose lower and upper limit corresponds to
  anisotropic and isotropic velocity distribution of the oxygen coronal
  ions, respectively.

Title: Latitudinal dependence of outflow velocities from O VI Doppler
    dimming observations during the Whole Sun Month
Authors: Strachan, Leonard; Panasyuk, Alexander V.; Dobrzycka, Danuta;
   Kohl, John L.; Noci, Giancarlo; Gibson, Sarah E.; Biesecker, Douglas A.
Bibcode: 2000JGR...105.2345S
Altcode:
  Empirical determinations of outflow velocities in the solar corona
  provide a much needed constraint, along with density and temperature
  determinations, of the acceleration and heating mechanisms in the
  extended corona. Much progress has been made on density determinations
  from white light polarized brightness observations but outflow
  velocities have been more difficult to determine. We present the
  first determinations of outflow velocities versus height and latitude
  based on a three-dimensional (3-D) reconstruction of the O VI 1032
  and 1037 Å emissivities. The Doppler dimming (and pumping) of the
  local emissivities give true localized outflow velocities at the
  selected locations in the extended corona from ~ 1.75 to 2.75 solar
  radii. The velocities are based on an empirical model of the corona
  which is constrained by the reconstructed O VI emissivities derived
  from the SOHO Ultraviolet Coronagraph Spectrometer (UVCS) synoptic
  observations and by electron density determinations based on white
  light measurements from the SOHO Large Angle Spectroscopic Coronagraph
  (LASCO) and Mauna Loa Solar Observatory (MLSO) Mk III coronameter.

Title: UVCS WLC Observations of Compressional Waves in the South
    Polar Coronal Hole
Authors: Ofman, L.; Romoli, M.; Poletto, G.; Noci, G.; Kohl, J. L.
Bibcode: 2000ApJ...529..592O
Altcode:
  Recent SOHO Ultraviolet Coronagraph Spectrometer (UVCS) white light
  channel (WLC) observations of the south polar coronal hole plumes and
  interplume regions produce signatures of quasi-periodic variations in
  the polarized brightness (pB) at a heliocentric distance of 1.9 solar
  radii (R<SUB>solar</SUB>). The Fourier power spectrum of the pB time
  series shows significant peaks at about 1.6-2.5 mHz and additional
  smaller peaks at longer and shorter timescales. Wavelet analysis of
  the pB time series shows that the coherence time of the fluctuations
  is about 30 minutes. The new observations strongly suggest that the
  fluctuations are compressional wave packets propagating in the coronal
  hole high above the limb. The presence of compressional waves may have
  important implications that help to explain the heating of coronal
  holes and the fast solar wind acceleration.

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: Streamer HI Ly-α Line Profiles During the Spartan 201-05/SOHO
    Coordinated Observations
Authors: Miralles, M. P.; Strachan, L.; Gardner, L. D.; Dobryzcka,
   D.; Ko, Y. -K.; Michels, J.; Panasyuk, A.; Suleiman, R.; Kohl, J. L.
Bibcode: 1999ESASP.448.1193M
Altcode: 1999mfsp.conf.1193M
  We present H I Lyalpha observations of coronal streamers obtained
  by UVCS/SOHO during the coordinated observations with UVCS/Spartan
  on 1 3 November 1998. Two different streamer regions were observed,
  one relatively stable above the Northeast limb, and a postCME streamer
  complex above the Southwest limb. H~I Lyalpha profiles and intensities
  were measured at ~1.5 and 2 Ro in the NE streamer and its boundary
  regions, and also at heights ranging from 1.5 to 2.5 Ro in the SW
  streamer complex. We analyze integrated intensities and line widths
  in each streamer structure.

Title: Polarimetry of the UV solar corona with ASCE
Authors: Fineschi, Silvano; Gardner, Larry D.; Kohl, John L.; Romoli,
   Marco; Pace, Emanuele; Corti, Gianni; Noci, Giancarlo C.
Bibcode: 1999SPIE.3764..147F
Altcode:
  The Advanced Solar Coronal Explorer (ASCE) is a mid-explorer (MidEx)
  mission selected, together with other five, for the a Phase A Concept
  Study in the 1999 round of MidEX proposal. ASCE's spacecraft bus is
  a SPARTAN 400 reusable carrier deployed in low Earth orbit by the
  Space Shuttle. ASCE's payload comprises two instrument modules,
  the Spectroscopic and Polarimetric Coronagraph (SPC) and the
  Extreme Ultraviolet Imager (EUVI). The scientific objective of the
  mission is the investigation, through spectroscopic and polarimetric
  techniques, of the physics of the coronal heating and of the solar
  wind acceleration. A critical physical parameter of the corona is the
  magnetic field. Polarimetric measurements of UV coronal radiation
  and their interpretation through the Hanle effect can be used for
  coronal magnetic field diagnostics. One of the SPC spectrometers,
  the Spectroscopy/Polarimetry channel (SPCH), includes a reflecting
  Brewster-angle polarimeter for measurements of the linear polarization
  of the HI Lyman series lines (i.e., Ly-(alpha) , -(beta) , and (gamma)
  ) and of the O VI 1032 Angstrom line. In this paper, the optical design
  of the SPCH polarimeter is described. A relevant element of this design
  is the external occulter (EXO) that is supported on a boom, which is
  extended 10 m beyond the instrument aperture, once the instrument is in
  station. The analysis of the stray- light reduction provided by this
  occulting system is described in this paper. The principal source of
  stray light is solar disk light that is diffracted from the edge of the
  EXO and scattered from the telescope mirror. The analysis shows that the
  stray-light is less than 10<SUP>-2</SUP> the coronal signal. This level
  of stray-light rejection minimizes the polarized stray light that may
  be introduced by the EXO's straight edge. The most appropriate material
  for the polarizer has been found to be CaF<SUB>2</SUB>. The material
  selection criteria are described. Finally, the paper illustrates with
  an example that if the linear polarization can be measured better than
  1%, then the instrumental sensitivity to magnetic fields may reach a
  few gauss (greater than 2 gauss), in coronal active regions.

Title: Flat field of UVCS detectors for early part of SOHO mission
Authors: Cosmo, Mario L.; Smith, Peter L.; Atkins, Nigel; Suleiman,
   R. M.; Gardner, Larry D.; Kohl, John L.
Bibcode: 1999SPIE.3764..161C
Altcode:
  The Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and
  Heliospheric Observatory (SOHO) comprises two telescopes and two
  spectrometer channels for spatially resolved ultraviolet spectral
  diagnostics of the solar corona. The principal lines for which the
  two channels are optimized are the H I 'Lyman-(alpha) ' line at 121.5
  nm and the O VI (O<SUP>5+</SUP>) doublet at 103.2 and 103.7 nm. An
  'in-flight' method, using observations of stars and scattered solar
  disk light, has been devised to determine the flat field function,
  i.e., the relative detection efficiency of the detector pixels. We
  present the details and results of this process. Local pixel-to-pixel
  efficiency variation is found to be, typically, about plus or minus 9%
  to plus or minus 17% (1 (sigma) ) for the H I Lyman-(alpha) channel
  and plus or minus 9% for the O VI channel.

Title: Coronal Magnetic Field Diagnostics with UV Spectropolarimetry
Authors: Fineschi, S.; van Ballegoijen, A.; Kohl, J. L.
Bibcode: 1999ESASP.446..317F
Altcode: 1999soho....8..317F
  No abstract at ADS

Title: The impact of ion-cyclotron wave dissipation on heating and
    accelerating the fast solar wind
Authors: Cranmer, Steven R.; Field, George B.; Kohl, John L.
Bibcode: 1999AIPC..471...35C
Altcode: 1999sowi.conf...35C
  Using empirical ion velocity distributions derived from UVCS and
  SUMER ultraviolet spectroscopy, we construct theoretical models of
  the nonequilibrium plasma state of the polar solar corona. The primary
  energy deposition mechanism we investigate is the dissipation of high
  frequency (10-10000 Hz) ion-cyclotron resonant Alfvén waves which
  can heat and accelerate ions differently depending on their charge
  and mass. We find that it is possible to explain many of the kinetic
  properties of the plasma with relatively small amplitudes for the
  resonant waves. There is evidence for steepening of the Alfvén wave
  spectrum between the coronal base and the largest heights observed
  spectroscopically, and it is important to take Coulomb collisions into
  account to understand observations at the lowest heights. Because the
  ion-cyclotron wave dissipation is rapid, the extended heating seems to
  demand a constantly replenished population of waves over several solar
  radii. This indicates that the waves are probably generated throughout
  the wind rather than propagated up from the base of the corona.

Title: UVCS/SOHO observations of coronal streamers
Authors: Frazin, R. A.; Modigliani, A.; Ciaravella, A.; Dennis, E.;
   Fineschi, S.; Gardner, L. D.; Michels, J.; O'Neal, R.; Raymond, J. C.;
   Wu, C. -R.; Noci, G.; Kohl, J. L.
Bibcode: 1999AIPC..471..235F
Altcode: 1999sowi.conf..235F
  We used the Ultraviolet Coronagraph Spectrometer (UVCS) on the
  Solar and Heliospheric Observatory (SOHO) to obtain line profiles
  in mid-latitude coronal streamers between 1.3 R<SUB>solar</SUB> and
  5.5 R<SUB>solar</SUB> during a period of moderate solar activity. We
  present a summary of the preliminary results. These results clearly
  indicate that the mid-latitude streamers observed during this time
  period have very different spectral properties than the equatorial
  streamers observed near solar minimum.

Title: Physical properties of coronal streamers as observed by
    Spartan 201
Authors: Miralles, M. P.; Strachan, L.; Gardner, L. D.; Smith, P. L.;
   Kohl, J. L.; Guhathakurta, M.; Fisher, R. R.
Bibcode: 1999AIPC..471..239M
Altcode: 1999sowi.conf..239M
  The three Spartan 201 flights from 1993 to 1995 provided us with
  observations in HI Lyman-α of several streamers in the declining
  phase of the current solar cycle. Analysis of the heliocentric height
  dependence of the HI Ly-α LOS velocity distribution width clearly show
  that there is a maximum in the proton 1/e velocities at heights ranging
  from 2.1 to 2.5 R<SUB>solar</SUB> for all of the observed streamers. We
  compare UVCS/Spartan results with proton velocity distributions from
  UVCS/SOHO during solar minimum. We also discuss differences in the
  proton velocity distributions for different types of streamers over
  the three year period of Spartan 201 observations.

Title: Spectroscopic Constraints on Models of Ion Cyclotron Resonance
    Heating in the Polar Solar Corona and High-Speed Solar Wind
Authors: Cranmer, Steven R.; Field, George B.; Kohl, John L.
Bibcode: 1999ApJ...518..937C
Altcode:
  Using empirical ion velocity distributions derived from Ultraviolet
  Coronagraph Spectrometer (UVCS) and Solar Ultraviolet Measurements
  of Emitted Radiation (SUMER) ultraviolet spectroscopy, we construct
  theoretical models of the nonequilibrium plasma state of the polar solar
  corona. The primary energy deposition mechanism we investigate is the
  dissipation of high-frequency (10-10,000 Hz) ion cyclotron resonant
  Alfvén waves which can heat and accelerate ions differently depending
  on their charge and mass. We solve the internal energy conservation
  equations for the ion temperature components parallel and perpendicular
  to the superradially expanding magnetic field lines and use empirical
  constraints for the remaining parameters. We find that it is possible
  to explain many of the kinetic properties of the plasma (such as high
  perpendicular ion temperatures and strong temperature anisotropies)
  with relatively small amplitudes for the resonant waves. There is
  suggestive evidence for steepening of the Alfvén wave spectrum between
  the coronal base and the largest heights observed spectroscopically, and
  it is important to take Coulomb collisions into account to understand
  observations at the lowest heights. Because the ion cyclotron wave
  dissipation is rapid, the extended heating seems to demand a constantly
  replenished population of waves over several solar radii. This indicates
  that the waves are generated gradually throughout the wind rather than
  propagated up from the base of the corona.

Title: Comparison of outflow velocity determinations with UVCS and
    LASCO for the coronal mass ejection of 13-14 August 1997
Authors: Strachan, L.; Ciaravella, A.; Raymond, J. C.; Fineschi, S.;
   O'Neal, R.; Kohl, J. L.; Modigliani, A.; Noci, G.; Andrews, M. D.
Bibcode: 1999AIPC..471..637S
Altcode: 1999sowi.conf..637S
  The Ultraviolet Coronagraph Spectrometer (UVCS) on SOHO observed
  a Coronal Mass Ejection (CME) on 13-14 August 1997. The event was
  observed simultaneously with the LASCO white light coronagraphs. This
  paper describes the results from a comparison of outflow velocities
  determined from UVCS Doppler dimming studies with the velocities
  determined by examining the proper motions of the CME as measured by
  LASCO. In addition, estimates for line of sight velocities, densities
  and kinetic temperatures are discussed.

Title: Geometry, physical properties and outflow velocities from
    the polar and equatorial coronal holes-UVCS/SOHO observations
Authors: Dobrzycka, Danuta; Panasyuk, Alexander V.; Strachan, Leonard;
   Kohl, John L.
Bibcode: 1999AIPC..471..305D
Altcode: 1999sowi.conf..305D
  We analyzed the UVCS/SOHO data obtained during the Whole Sun
  Month campaign in 1996 and compared the H I Lyα (1216Å) and O VI
  (1032Å,1037Å) emission in the polar and equatorial coronal holes. We
  found that the emission lines have similar characteristics in these
  two types of coronal holes. Both types show evidence for superradially
  diverging boundaries. We used the O VI (1032Å) and O VI (1037Å) local
  emissivities, determined from the 3D tomographic reconstruction of
  the solar corona, to investigate the outflow velocities from the polar
  and equatorial coronal holes. The latitudinal distribution of the O VI
  ratio at 2.21 R<SUB>solar</SUB>, free from the line-of-sight effect,
  shows evidence that the equatorial coronal hole may have O<SUP>+5</SUP>
  outflow velocities lower than in the polar coronal holes.

Title: Whole Sun Month at solar minimum: An introduction
Authors: Galvin, Antoinette B.; Kohl, John L.
Bibcode: 1999JGR...104.9673G
Altcode:
  The Whole Sun Month was a collaborative project of the IACG Campaign
  4 and the SOHO Joint Observing Programs to characterize and model the
  structure of the global corona during solar minimum conditions. This
  introduction provides a brief description of the campaign objectives,
  the missions, and observatories involved and highlights some of the
  scientific results reported elsewhere in this special section.

Title: Study of the latitudinal dependence of H I Lyman α and O VI
emission in the solar corona: Evidence for the superradial geometry
    of the outflow in the polar coronal holes
Authors: Dobrzycka, Danuta; Cranmer, Steven R.; Panasyuk, Alexander
   V.; Strachan, Leonard; Kohl, John L.
Bibcode: 1999JGR...104.9791D
Altcode:
  We study the latitudinal distribution of the H I Lyman α and O VI
  (103.2 nm and 103.7 nm) line emission during the period of the Whole
  Sun Month campaign (August 10 to September 8, 1996) when the Sun was
  close to the minimum of its activity. The H I Lyman α and O VI line
  intensities appeared to be almost constant with latitude within the
  polar coronal holes and have abrupt increases toward the streamer
  region. We found that both north and south polar coronal holes had
  similar line intensities and line-of-sight velocities, as well as
  kinetic temperatures of H<SUP>0</SUP> and O<SUP>5+</SUP>. The dependence
  of these parameters on latitude and radius is provided. We derived
  boundaries of the polar coronal holes based on the H I Lyman α and O VI
  line intensity distributions for several days during the Whole Sun Month
  campaign. We found that the polar coronal hole boundaries clearly have
  a superradial geometry with diverging factor f<SUB>max</SUB> ranging
  from 6.0 to 7.5, and they are consistent with boundaries previously
  derived from the electron density distributions. We also found that,
  in general, they are not symmetric with respect to the heliographic
  poles, and their size and geometry change over periods of days. The H
  I Lyman α, O VI (103.2 nm), and the O VI (103.7 nm) line intensities
  showed similar boundaries within the uncertainties of our data. We
  modeled the latitudinal distribution of the H I Lyman α and O VI
  (103.2 nm and 103.7 nm) line intensities in the south polar coronal
  hole on August 17, 1996, assuming the coronal plasma outflow along
  either purely radial or nonradial flux tubes. A comparison of model
  predictions with the observed distributions shows evidence that the
  outflow velocity vectors follow nonradial intensity pattern.

Title: The Advanced Solar Coronal Explorer Mission (ASCE)
Authors: Kohl, J.; Cranmer, S.; Gardner, L.; Golub, L.; Raymond, J.;
   Smith, P. L.; Strachan, L.; Howard, R.; Moses, D.; Socker, D.; Wang,
   D.; Fisher, R. R.; Davila, J.; St. Cyr, C.; Noci, G.; Tondello, G.
Bibcode: 1999AAS...194.6506K
Altcode: 1999BAAS...31Q.928K
  The Advanced Solar Coronal Explorer (ASCE) mission was selected
  for a Phase A Concept Study in the current round of proposed MIDEX
  missions. It addresses three fundamental problems: 1) What physical
  processes heat coronal holes and drive the fast solar wind? 2) What
  physical processes heat streamers and drive the slow solar wind? and 3)
  How are coronal mass ejections (CMEs) heated and accelerated, and what
  role to they play in the evolution of the solar magnetic field. ASCE
  has two instruments, the Spectroscopic and Polarimetric Coronagraph
  (SPC) and the Extreme Ultraviolet Imager (EUVI). A deployable boom
  supports a distant external occulter that allows large aperture optics
  for the SPC coronagraphic channels. SPC's EUV channels will provide
  spectroscopy of the extended solar corona with 30 - 200 times the
  sensitivity of UVCS/SOHO and the first He II 30.4 nm spectroscopy of
  the extended corona. SPC's Large Aperture Spectroscopic Coronagraph
  channel will provide two orders of magnitude improvement in stray
  light suppression for wide field visible spectroscopy and 2 arcsec
  resolution elements for imaging and polarimetry. EUVI provides full
  disk imaging with 0.9 arcsec resolution elements and extremely high
  cadence. ASCE is designed to determine the thermal, kinetic, and
  wave energy densities in coronal structures, determine the rates of
  transformation among these forms of energy, their flow in space, and
  their loss to radiation, and determine the composition and ionization
  state of the corona in static and transient conditions.

Title: Joint H I Lyalpha Observations with UVCS/Spartan and UVCS/SOHO
    During the STS-95 Mission
Authors: Dobrzycka, D.; Kohl, J. L.; Gardner, L. D.; Strachan, L.;
   Miralles, M. P.; Smith, P. L.; Suleiman, R.; Panasyuk, A.; Michels,
   J.; Ko, Y. -K.
Bibcode: 1999AAS...194.1609D
Altcode: 1999BAAS...31..851D
  The Spartan 201 Ultraviolet Coronal Spectrometer (UVCS/Spartan)
  is an instrument developed to conduct spectroscopic studies of the
  extended solar corona and its expansion into the solar wind. It was
  designed to be Shuttle deployed and retrieved and has already flown in
  1993, 1994, 1995, 1997, and 1998 providing a consistent set of data
  that span several years of the declining and rising phases of the
  solar cycle. The advantage of this instrument is that its inflight
  performance characteristics can be determined from the preflight and
  postflight laboratory calibration. The last, Spartan 201-5 mission was
  launched aboard the Space Shuttle Discovery (STS-95) on 29 October 1998
  at 2:19:20 PM (EST). Spartan 201 made autonomous observations of the
  Sun and its corona for approximately 43 hours during 26 orbits around
  the Earth. These observations were coordinated with the Ultraviolet
  Coronagraph Spectrometer on board the Solar and Heliospheric Observatory
  (UVCS/SOHO). One of the main goals of the Spartan 201-5 mission was
  to update calibration of the UVCS/SOHO and to provide continuity of
  measurements from the period before and after solar minimum. We review
  the successfully accomplished goals of the UVCS/Spartan on the Spartan
  201-5 flight and describe the radiometric and spectrometric comparison
  of the streamer data to that of UVCS/SOHO. This work is supported by
  NASA under Grant NAG 5-613 to the Smithsonian Astrophysical Observatory
  and by NASA under Grant NAG5-3192 to the Smithsonian Astrophysical
  Observatory, by the Italian Space Agency, and by Swiss Funding Agencies.

Title: SOHO/Spartan 201 Coordinated Observations
Authors: Kohl, J. L.; Gardner, L. D.; Strachan, L.; Miralles, M. P.;
   Smith, P. L.; Suleiman, R.; Dobrzycka, D.
Bibcode: 1999EOSTr..80..263K
Altcode:
  We present preliminary results from the simultaneous H I Lyman alpha
  observations carried out during 1-3 November 1998 with the UVCS/SOHO
  and UVCS/Spartan instruments. The main objective of this mission was
  to provide information on the physical conditions of the solar corona
  during the rising phase of the solar activity cycle. The analysis of
  the H I Lyman alpha profile measurements made with both instruments
  provides us with hydrogen kinetic temperatures. These observations are
  also used to update the calibration of the UVCS/SOHO instrument. This
  cross-calibration provides continuity between the earlier results of
  Spartan 201 and more recent results from SOHO, and consequently it
  provides information on how the corona varies from the period before
  the activity minimum to the period approaching the time of maximum
  solar activity. This work is supported by NASA under Grants NAG 5-613
  and NAG5-3192 to the Smithsonian Astrophysical Observatory.

Title: UVCS/Spartan Observations of Coronal Streamers
Authors: Miralles, M. P.; Strachan, L.; Gardner, L. D.; Smith, P. L.;
   Kohl, J. L.; Guhathakurta, M.; Fisher, R. R.
Bibcode: 1999EOSTr..80..263M
Altcode:
  We present H I Lyman alpha observations of coronal streamers obtained
  by the UVCS instrument aboard Spartan 201 satellite during four
  flights between 1993 and 1998. The analysis of the data allows us to
  study the velocity structure of various streamer regions at different
  phases of the solar activity cycle. We compare physical properties of
  streamers derived from the UVCS/Spartan H I Lyman alpha measurements
  before solar minimum with results from UVCS/SOHO and UVCS/Spartan
  after solar minimum. This work is supported by NASA under Grants NAG
  5-613 and 5-3192 to the Smithsonian Astrophysical Observatory.

Title: Latitudinal properties of the Lyman alpha and O VI profiles
    in the extended solar corona
Authors: Zangrilli, L.; Nicolosi, P.; Poletto, G.; Noci, G.; Romoli,
   M.; Kohl, J. L.
Bibcode: 1999A&A...342..592Z
Altcode:
  We have analysed the latitudinal properties of the profiles of the H I
  Lyman alpha line at 1215.6 protect Angstroms and of the O VI doublet at
  1031.9 protect Angstroms and 1037.6 protect Angstroms in the extended
  solar corona, between 1.5 R_sun and 2.0 R_sun. Observations have
  been performed with the UltraViolet Coronagraph Spectrometer (UVCS)
  on board the ESA-NASA solar satellite SOHO (SOlar and Heliospheric
  Observatory). The results show that these lines have quite a different
  behaviour with latitude: the Ly alpha line has larger full width at
  half maximum (FWHM) values in the streamer region and narrower ones
  towards polar latitudes, while the O VI lines have a minimum FWHM at
  the center of the streamer, which almost steadily increases towards
  polar regions. The observations have been analysed looking also
  for an interpretation in terms of selective heating mechanisms. The
  implications of our results for coronal heating theories are also
  examined. In particular we discuss the possibility for the presence
  of the ion-cyclotron coronal heating mechanism. Moreover, we point out
  an interesting correlation between the intensity of the coronal lines
  and their widths, which may be relevant to the open question of the
  different morphological features visible in the Ly alpha and O VI lines.

Title: An Empirical Model of a Polar Coronal Hole at Solar Minimum
Authors: Cranmer, S. R.; Kohl, J. L.; Noci, G.; Antonucci, E.;
   Tondello, G.; Huber, M. C. E.; Strachan, L.; Panasyuk, A. V.;
   Gardner, L. D.; Romoli, M.; Fineschi, S.; Dobrzycka, D.; Raymond,
   J. C.; Nicolosi, P.; Siegmund, O. H. W.; Spadaro, D.; Benna, C.;
   Ciaravella, A.; Giordano, S.; Habbal, S. R.; Karovska, M.; Li, X.;
   Martin, R.; Michels, J. G.; Modigliani, A.; Naletto, G.; O'Neal,
   R. H.; Pernechele, C.; Poletto, G.; Smith, P. L.; Suleiman, R. M.
Bibcode: 1999ApJ...511..481C
Altcode:
  We present a comprehensive and self-consistent empirical model
  for several plasma parameters in the extended solar corona above
  a polar coronal hole. The model is derived from observations
  with the SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO)
  during the period between 1996 November and 1997 April. We compare
  observations of H I Lyα and O VI λλ1032, 1037 emission lines
  with detailed three-dimensional models of the plasma parameters and
  iterate for optimal consistency between measured and synthesized
  observable quantities. Empirical constraints are obtained for
  the radial and latitudinal distribution of density for electrons,
  H<SUP>0</SUP>, and O<SUP>5+</SUP>, as well as the outflow velocity
  and unresolved anisotropic most probable speeds for H<SUP>0</SUP> and
  O<SUP>5+</SUP>. The electron density measured by UVCS/SOHO is consistent
  with previous solar minimum determinations of the white-light coronal
  structure; we also perform a statistical analysis of the distribution
  of polar plumes using a long time series. From the emission lines we
  find that the unexpectedly large line widths of H<SUP>0</SUP> atoms
  and O<SUP>5+</SUP> ions at most heights are the result of anisotropic
  velocity distributions. These distributions are not consistent with
  purely thermal motions or the expected motions from a combination of
  thermal and transverse wave velocities. Above 2 R<SUB>solar</SUB>,
  the observed transverse most probable speeds for O<SUP>5+</SUP> are
  significantly larger than the corresponding motions for H<SUP>0</SUP>,
  and the outflow velocities of O<SUP>5+</SUP> are also significantly
  larger than the corresponding velocities of H<SUP>0</SUP>. Also, the
  latitudinal dependence of intensity constrains the geometry of the
  wind velocity vectors, and superradial expansion is more consistent
  with observations than radial flow. We discuss the constraints and
  implications on various theoretical models of coronal heating and
  acceleration.

Title: EUV Spectral Line Profiles in Polar Coronal Holes from 1.3
    to 3.0 R<SUB>solar</SUB>
Authors: Kohl, J. L.; Esser, R.; Cranmer, S. R.; Fineschi, S.; Gardner,
   L. D.; Panasyuk, A. V.; Strachan, L.; Suleiman, R. M.; Frazin, R. A.;
   Noci, G.
Bibcode: 1999ApJ...510L..59K
Altcode:
  Spectral line profiles have been measured for H I λ1216, O VI λλ1032,
  1037, and Mg X λ625 in a polar coronal hole observed during 1997
  September 15-29, at projected heliographic heights ρ between 1.34
  and 2.0 R<SUB>solar</SUB>. Observations of H I λ1216 and the O
  VI doublet from 1997 January for ρ=1.5-3.0 R<SUB>solar</SUB> are
  provided for comparison. The O VI lines are well fit to a narrow and
  broad component which appear to be associated with regions of higher
  and lower spectral radiance, respectively. The narrow components
  dominate at low heights and become a small fraction of the lines at
  higher heights. Mg X λ625 is observed to have a narrow component at
  ρ=1.34 R<SUB>solar</SUB> which accounts for only a small fraction of
  the observed spectral radiance. In the case of the broad components,
  the values of v<SUB>1/e</SUB> for O VI are only slightly larger than
  those for H I at ρ=1.34 R<SUB>solar</SUB> but are significantly
  larger at ρ=1.5 R<SUB>solar</SUB> and much larger for ρ&gt;1.75
  R<SUB>solar</SUB>. In contrast, the Mg X values are less than those
  of H I up to 1.75 and then increase rapidly up to at least ρ=2.0
  R<SUB>solar</SUB> but never reach the values of O VI.

Title: Properties of Coronal Hole/Streamer Boundaries and Adjacent
    Regions as Observed by SPARTAN 201
Authors: Miralles, M. P.; Strachan, L.; Gardner, L. D.; Smith, P. L.;
   Kohl, J. L.; Guhathakurta, M.; Fisher, R. R.
Bibcode: 1999SSRv...87..277M
Altcode:
  The Spartan 201 flights from 1993 to 1995 provided us with
  observations in H I Lyman-α of several coronal hole/streamer
  boundaries and adjacent streamers during the declining phase of the
  current solar cycle: Analysis of the latitudinal dependence of the
  line intensities clearly shows that there is a boundary region at
  the coronal hole/streamer interface where the H I Lyman-α intensity
  reaches a minimum value. Similar results are also found in UVCS/SOHO
  observations. We also discuss differences in the coronal hole/streamer
  boundaries for different types of streamers and their changes over
  the three year period of Spartan 201 observations.

Title: Variation of Polar Coronal Hole Profiles with Solar Cycle
Authors: Dobrzycka, D.; Strachan, L.; Miralles, M. P.; Kohl, J. L.;
   Gardner, L. D.; Smith, P.; Guhathakurta, M.; Fisher, R.
Bibcode: 1999SSRv...87..177D
Altcode:
  We compared the H I Lyα polar coronal hole profiles obtained during
  the three Spartan 201 flights (in 1993, 1994, and 1995) and during the
  more recent UVCS/SOHO mission. We found that at 2.1 R<SUB>⊙</SUB>
  there are no significant variations of the line shape over the several
  years of the descending phase of the solar cycle. However, there may be
  some evidence for the 1.8 R<SUB>⊙</SUB> profiles being broader towards
  solar minimum. The profiles at 2.1 R<SUB>⊙</SUB> are different from
  profiles obtained at 1.8 R<SUB>⊙</SUB>; they have clearly narrower
  cores and wide wings. We fitted the profiles with single and/or multiple
  Gaussian functions and calculated their typical 1/e half widths.

Title: Plasma Properties in Coronal Holes Derived from Measurements
    of Minor Ion Spectral Lines and Polarized White Light Intensity
Authors: Esser, Ruth; Fineschi, Silvano; Dobrzycka, Danuta; Habbal,
   Shadia R.; Edgar, Richard J.; Raymond, John C.; Kohl, John L.;
   Guhathakurta, Madhulika
Bibcode: 1999ApJ...510L..63E
Altcode:
  Recent observations of the Lyα λ1216, Mg X λ625, and O VI λ1038
  spectral lines carried out with the Ultraviolet Coronagraph Spectrometer
  (UVCS) on board SOHO at distances in the range 1.35-2.1 R<SUB>S</SUB> in
  the northern coronal hole are used to place limits on the turbulent wave
  motions of the background plasma and the thermal motions of the protons
  and Mg<SUP>+9</SUP> and O<SUP>+5</SUP> ions. Limits on the turbulent
  wave motion are estimated from the measured line widths and electron
  densities derived from white light coronagraph observations, assuming
  WKB approximation at radial distances covered by the observations. It
  is shown that the contribution of the turbulent wave motion to the
  widths of the measured spectral lines is small compared to thermal
  broadening. The observations show that the proton temperature slowly
  increases between 1.35 and 2.7 R<SUB>S</SUB> and does not exceed
  3×10<SUP>6</SUP> K in that region. The temperature of the minor ions
  exceeds the proton temperature at all distances, but the temperatures
  are neither mass proportional nor mass-to -charge proportional. It is
  shown, for the first time, that collision times between protons and
  minor ions are small compared to the solar wind expansion times in
  the inner corona. At 1.35 R<SUB>S</SUB> the expansion time exceeds
  the proton Mg<SUP>+9</SUP> collision time by more than an order of
  magnitude. Nevertheless, the temperature of the Mg ions is significantly
  larger than the proton temperature, which indicates that the heating
  mechanism has to act on timescales faster than minutes. When the
  expansion time starts to exceed the collision times a rapid increase
  of the O<SUP>+5</SUP> ion spectral line width is seen. This indicates
  that the heavier and hotter ions lose energy to the protons as long as
  collision frequencies are high, and that the ion spectral line width
  increases rapidly as soon as this energy loss stops.

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: Ulysses-UVCS Coordinated Observations
Authors: Suess, S. T.; Poletto, G.; Corti, G.; Simnett, G.; Noci,
   G.; Romoli, M.; Kohl, J.; Goldstein, B.
Bibcode: 1999SSRv...87..319S
Altcode:
  We present results from SOHO/UVCS measurements of the density and
  flow speed of plasma at the Sun and again of the same plasma by
  Ulysses/SWOOPS in the solar wind. UVCS made measurements at 3.5 and
  4.5 solar radii and Ulysses was at 5.1 AU. Data were taken for nearly
  2 weeks in May June 1997 at 9 10 degrees north of the equator in the
  streamer belt on the east limb. Density and flow speed were compared
  to see if near Sun characteristics are preserved in the interplanetary
  medium. By chance, Ulysses was at the very northern edge of the streamer
  belt. Nevertheless, no evidence was found of fast wind or mixing of slow
  wind with fast wind coming from the northern polar coronal hole. The
  morphology of the streamer belt was similar at the beginning and end
  of the observing period, but was markedly different during the middle
  of the period. A corresponding change in density (but not flow speed)
  was noted at Ulysses.

Title: UVCS/SOHO Observations of H I Lyman Alpha Line Profiles in
    Coronal Holes at Heliocentric Heights Above 3.0 R⊙
Authors: Suleiman, R. M.; Kohl, J. L.; Panasyuk, A. V.; Ciaravella,
   A.; Cranmer, S. R.; Gardner, L. D.; Frazin, R.; Hauck, R.; Smith,
   P. L.; Noci, G.
Bibcode: 1999SSRv...87..327S
Altcode:
  The Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and
  Heliospheric Observatory (SOHO) has been used to measure spectral line
  profiles for H I Lyα in the south polar coronal hole at projected
  heliocentric heights from 3.5 to 6.0 R<SUB>⊙</SUB> during 1998
  January 5 11. Observations from 1.5 to 2.5 R<SUB>⊙</SUB> were made
  for comparison. The H I Lyα profile is the only one observable with
  UVCS above 3.5 R<SUB>⊙</SUB> in coronal holes. Within this region
  the outflowing coronal plasma becomes nearly collisionless and the
  ionization balance is believed to become frozen.

Title: Comparison of Polar and Equatorial Coronal Holes Observed by
UVCS/SOHO: Geometry and Physical Properties
Authors: Dobrzycka, D.; Panasyuk, A.; Strachan, L.; Kohl, J.
Bibcode: 1999SSRv...87..173D
Altcode:
  We analyzed UVCS/SOHO data and compared the H I Lyα (121.6 nm) and O
  VI (103.2 nm, 103.7 nm) emission in the polar and equatorial coronal
  holes. We found that the emission lines have similar characteristics
  in these two types of coronal holes. Both types show evidence for
  superradially diverging boundaries. The latitudinal distribution of
  the O VI line ratio may indicate that the equatorial coronal hole has
  O<SUP>+5</SUP> outflow velocities lower than in the polar coronal holes.

Title: Constraints on Coronal Outflow Velocities Derived from UVCS
    Doppler Dimming Measurements and in-Situ Charge State Data
Authors: Strachan, L.; Ko, Y. -K.; Panasyuk, A. V.; Dobrzycka, D.;
   Kohl, J. L.; Romoli, M.; Noci, G.; Gibson, S. E.; Biesecker, D. A.
Bibcode: 1999SSRv...87..311S
Altcode:
  We constrain coronal outflow velocity solutions, resolved along the
  line-of-sight, by using Doppler dimming models of H I Lyman alpha and
  O VI 1032/1037 Å emissivities obtained with data from the Ultraviolet
  Coronagraph Spectrometer (UVCS) on SOHO. The local emissivities, from
  heliocentric heights of 1.5 to 3.0 solar radii, were determined from 3-D
  reconstructions of line-of-sight intensities obtained during the first
  Whole Sun Month Campaign (10 August to 8 September 1996). The models use
  electron densities derived from polarized brightness measurements made
  with the visible light coronagraphs on UVCS and LASCO, supplemented
  with data from Mark III at NCAR/MLSO. Electron temperature profiles
  are derived from 'freezing-in' temperatures obtained from an analysis
  of charge state data from SWICS/Ulysses. The work concentrates on
  neutral hydrogen outflow velocities which depend on modeling the
  absolute coronal H I Lyα emissivities. We use an iterative method to
  determine the neutral hydrogen outflow velocity with consistent values
  for the electron temperatures derived from a freezing-in model.

Title: Coronal Holes and Solar Wind Acceleration, Proceedings of
    the SOHO-7 Workshop.
Authors: Kohl, John L.; Cranmer, Steven R.
Bibcode: 1999soho....7.....K
Altcode:
  No abstract at ADS

Title: UVCS/SOHO Ion Kinetics in Coronal Streamers
Authors: Frazin, R. A.; Ciaravella, A.; Dennis, E.; Fineschi, S.;
   Gardner, L. D.; Michels, J.; O'Neal, R.; Raymond, J. C.; Wu, C. -R.;
   Kohl, J. L.; Modigliani, A.; Noci, G.
Bibcode: 1999SSRv...87..189F
Altcode:
  We made streamer observations with the Ultraviolet Coronagraph
  Spectrometer (UVCS) on the Solar and Heliospheric Observatory (SOHO)
  during the early part of 1998, which was a time of moderate solar
  activity. We present an empirical study of coronal ion kinetics using
  the line profiles from these observations. Our first and most striking
  result is that the mid-latitude (ML) streamers have much narrower
  O VI 1032 Å line profiles than the solar minimum equatorial (SME)
  streamers. Our second result is that the line profiles from a small
  collection of ions in ML streamers do not seem to be consistent with
  the ions having a single temperature and turbulent velocity. We discuss
  several interpretations, including line of sight (LOS) effects. This
  work is supported by the National Aeronautics and Space Administration
  under grant NAG-3192 to the Smithsonian Astrophysical Observatory.

Title: Ly-α Observation of a Coronal Streamer with UVCS/SOHO
Authors: Maccari, L.; Noci, G.; Modigliani, A.; Romoli, M.; Fineschi,
   S.; Kohl, J. L.
Bibcode: 1999SSRv...87..265M
Altcode:
  In this paper we discuss some characteristics of an equatorial streamer
  observed by UVCS in July 1997. We determine the height distribution
  of the Ly-α total intensity and of its width. We focus our attention,
  in particular, on the time variability of these parameters.

Title: Foreword
Authors: Kohl, John L.; Cranmer, Steven R.
Bibcode: 1999SSRv...87....9K
Altcode:
  No abstract at ADS

Title: UVCS/SOHO Observations of Spectral Line Profiles in Polar
    Coronal Holes
Authors: Kohl, J. L.; Fineschi, S.; Esser, R.; Ciaravella, A.; Cranmer,
   S. R.; Gardner, L. D.; Suleiman, R.; Noci, G.; Modigliani, A.
Bibcode: 1999SSRv...87..233K
Altcode:
  Ultraviolet emission line profiles have been measured on 15-29 September
  1997 for H I 1216 Å, O VI 1032, 1037 Å and Mg X 625 Å in a polar
  coronal hole, at heliographic heights ϱ (in solar radii) between 1.34
  and 2.0. Observations of H I 1216 Å and the O VI doublet from January
  1997 for ϱ = 1.5 to 3.0 are provided for comparison. Mg X 625 Å is
  observed to have a narrow component at ϱ = 1.34 which accounts for
  only a small fraction of the observed spectral radiance, and a broad
  component that exists at all observed heights. The widths of O VI broad
  components are only slightly larger than those for H I at ϱ = 1.34,
  but are significantly larger at ϱ = 1.5 and much larger for ϱ &gt;
  1.75. In contrast, the Mg X values are less than those of H I up to
  1.75 and then increase rapidly up to at least ϱ = 2.0, but never
  reach the values of O VI.

Title: What Can UVCS Observations Tell Us about Coronal Mass Ejections
Authors: Strachan, L.; Ciaravella, A.; Raymond, J. C.; Kohl, J. L.
Bibcode: 1999EOSTr..80..254S
Altcode:
  The Ultraviolet Coronagraph Spectrometer (UVCS) on SOHO has observed a
  number of Coronal Mass Ejections at various heights and heliographic
  latitudes. We will focus on the changes in the physical conditions
  of the coronal plasma that can be observed with uv spectroscopic
  techniques. These changes may provide a clue to the origin of the
  material ejected by the CME. This work is supported in part by NASA
  under grant NAG-3192 to the Smithsonian Astrophysical Observatory,
  by the Italian Space Agency and by Swiss funding agencies.

Title: Coronal holes and solar wind acceleration. Proceedings. SOHO-7
    Workshop, Northeast Harbor, ME (USA), 28 Sep - 1 Oct 1998.
Authors: Kohl, J. L.; Cranmer, S. R.
Bibcode: 1999SSRv...87.....K
Altcode:
  The following topics were dealt with: solar coronal holes, solar wind
  acceleration, solar wind models, high speed solar wind, compositional
  variations, coronal loops, solar magnetic fields, plasma waves, solar
  polar region, coronal heating, streamers.

Title: Variation of H I Lyman Alpha Profiles in the Solar Corona
    from 1993 to 1998
Authors: Miralles, M. P.; Strachan, L.; Gardner, L. D.; Dobryzcka,
   D.; Smith, P. L.; Kohl, J. L.
Bibcode: 1999EOSTr..80..818M
Altcode:
  UVCS/Spartan and UVCS/SOHO Lyman alpha intensity and profile
  measurements of the solar corona have been made from 1993 to the
  present, spanning the declining phase of cycle 22 through the rising
  phase of cycle 23. These measurements can be used to characterize
  the plasma in the regions where solar wind acceleration and heating
  mechanisms are important. The H I Lyman alpha intensity observations
  provide information about electron temperature and outflow velocity as
  well as density. The analysis of the line profile provides information
  about the line of sight velocity distribution of the protons. The recent
  coordinated SOHO/Spartan 201-5 mission confirmed the UVCS/SOHO spectral
  characterization and radiometric calibration an allows a continuity of
  measurements from the period before minimum to the present rising phase
  toward solar maximum. We show how streamer and coronal hole profiles
  change over this period. This work is supported by NASA under Grants
  NAG 5-613 and 5-3192 to the Smithsonian Astrophysical Observatory.

Title: SOHO Observations of Density Fluctuations in Coronal Holes
Authors: Ofman, L.; Romoli, M.; Noci, G.; Poletto, G.; Kohl, J. L.;
   Howard, R. A.; Cyr, C. St.; Deforest, C. E.
Bibcode: 1999SSRv...87..287O
Altcode:
  In recent UVCS/SOHO White Light Channel (WLC) observations we found
  quasi-periodic variations in the polarized brightness (pB) in the
  polar coronal holes at heliocentric distances of 1.9 to 2.45 solar
  radii. The motivation for the observation is the 2.5D MHD model of
  solar wind acceleration by nonlinear waves, that predicts compressive
  fluctuations in coronal holes. In February 1998 we performed new
  observations using the UVCS/WLC in the coronal hole and obtained
  additional data. The new data corroborate our earlier findings with
  higher statistical significance. The new longer observations show that
  the power spectrum peaks in the 10 12 minute range. These timescales
  agree with EIT observations of brightness fluctuations in polar
  plumes. We performed preliminary LASCO/C2 observations in an effort
  to further establish the coronal origin of the fluctuations.

Title: Spectroscopic Constraints on Models of Ion-cyclotron Resonance
    Heating in the Polar Solar Corona
Authors: Cranmer, S. R.; Field, G. B.; Kohl, J. L.
Bibcode: 1999SSRv...87..149C
Altcode:
  Using empirical velocity distributions derived from UVCS and
  SUMER ultraviolet spectroscopy, we construct theoretical models of
  anisotropic ion temperatures in the polar solar corona. The primary
  energy deposition mechanism we investigate is the dissipation of high
  frequency (10-10000 Hz) ion-cyclotron resonant Alfvén waves which
  can heat and accelerate ions differently depending on their charge
  and mass. We find that it is possible to explain the observed high
  perpendicular temperatures and strong anisotropies with relatively small
  amplitudes for the resonant waves. There is suggestive evidence for
  steepening of the Alfvén wave spectrum between the coronal base and the
  largest heights observed spectroscopically. Because the ion-cyclotron
  wave dissipation is rapid, even for minor ions like O<SUP>5+</SUP>,
  the observed extended heating seems to demand a constantly replenished
  population of waves over several solar radii. This indicates that
  the waves are generated gradually throughout the wind rather than
  propagated up from the base of the corona.

Title: Spectroscopic Constraints on Models of Ion-Cyclotron Resonance
    Heating in the Polar Solar Corona and Fast Solar Wind
Authors: Cranmer, S. R.; Field, G. B.; Kohl, J. L.
Bibcode: 1998EOSTr..79..722C
Altcode:
  We present preliminary results from a theoretical model of the heating
  of minor ions in the fast solar wind. We examine the compatibility
  between these models and spectroscopic determinations of velocity
  distribution functions from the UVCS and SUMER instruments aboard
  SOHO. By examining the dependence of line shapes (which probe
  the perpendicular velocity distribution) on ion charge and mass,
  detailed information can be extracted about the preferential heating
  and the Coulomb collisional coupling. The primary momentum and energy
  deposition mechanism we investigate is the dissipation of high-frequency
  (ion-cyclotron resonant) Alfven waves, which can accelerate and heat
  ions differently depending on their charge and mass. Minor ions which
  do not appreciably damp the resonant wave amplitudes can be used to
  constrain the slope of the fluctuation spectrum. SUMER measurements of
  several ions at heliocentric heights between 1.02 and 1.07 solar radii
  allow the ``base'' spectrum to be analyzed, and UVCS O VI line widths
  measured between 1.5 and 3.5 solar radii provide information about
  the radial evolution of the spectrum. This work is supported by the
  National Aeronautics and Space Administration under grant NAG5-3192 to
  the Smithsonian Astrophysical Observatory, by Agenzia Spaziale Italiana,
  and by the ESA PRODEX program (Swiss contribution).

Title: White-light stray light test of the SOHO UVCS
Authors: Leviton, Douglas B.; Gardner, Larry D.; Fineschi, Silvano;
   Jhabvala, Murzy D.; Kohl, John L.; Romoli, Marco; Noci, Giancarlo C.
Bibcode: 1998SPIE.3443...50L
Altcode:
  During the late stages of integration at MATRA-Marconi in Toulouse,
  France of the Ultraviolet Coronagraph Spectrometer (UVCS) for the joint
  NASA/ESA (European Space Agency) Solar and Heliospheric Observatory
  (SOHO), project management for the International Solar and Terrestrial
  Physics Project (ISTP) at Goddard Space Flight Center (GSFC) became
  concerned that the instrument's elaborate stray light rejection system
  had not been tested and might possibly be misaligned such that the
  instrument could not deliver promised scientific returns. A white light
  stray light test, which would place an upper bound on UVCS's stray
  light rejection capability, was commissioned, conceived, and carried
  out. This upper bound value would be indicative of the weakest coronal
  features the spectrometer would be capable of discerning. The test was
  rapidly developed at GSFC, in parallel with spacecraft integration,
  in coordination with science team members from Harvard- Smithsonian
  Center for Astrophysics (CFA) and was carried out at MATRA in late
  February 1995. The outcome of this test helped justify later impact
  to integration schedule to conduct similar much needed testing with
  visible and far ultraviolet light at CFA in a facility specifically
  designed to perform such tests.

Title: Grating stray light analysis and control in the UVCS/SOHO
Authors: Fineschi, Silvano; Gardner, Larry D.; Kohl, John L.; Romoli,
   Marco; Noci, Giancarlo C.
Bibcode: 1998SPIE.3443...67F
Altcode:
  The Ultraviolet Coronagraph Spectrometer (UVCS) of the Solar and
  Heliospheric (SOHO) mission has been developed for spectroscopic
  and polarimetric determinations of temperatures, densities and
  flow velocities in the extended solar corona. The instrument
  consists of a visible light (VL) polarimeter, and two ultraviolet
  (UV) spectrometers, optimized for the H I Lyman (alpha) (Ly-(alpha)
  ) line ((lambda) 1216 angstrom) and for the O VI doublet ((lambda)
  (lambda) 1032/1037 angstrom). The stray-light profile of the Ly-(alpha)
  holographic grating has been measured, in a laboratory set-up, in
  both the spatial and spectral directions. The observed profile has
  been found to be a combination of two components: the scattering
  from the grating surface, and the Fraunhofer diffraction due to the
  vignetting of the grating. An analytical expression for the scattering
  component of the grating point spread function (PSF) has been derived
  from a simple model of the grating surface roughness. The stray-light
  profile generated by the analytical expression of the grating PSF gives
  a good fit of stray-light profile measured in the laboratory. This
  instrument function has been used in the analysis of in-flight UVCS
  observations of the profile of electron scattered Ly- (alpha) from the
  solar corona. These observations have resulted, for the first time,
  in the most direct measurement of the coronal electron temperature.

Title: Solar Wind at 6.8 Solar Radii from UVCS Observation of Comet
    C/1996Y1
Authors: Raymond, John C.; Fineschi, S.; Smith, P. L.; Gardner, L.;
   O'Neal, R.; Ciaravella, A.; Kohl, J. L.; Marsden, B.; Williams, G. V.;
   Benna, C.; Giordano, S.; Noci, G.; Jewitt, D.
Bibcode: 1998ApJ...508..410R
Altcode:
  The comet C/1996Y1, a member of the Kreutz family of Sun-grazing comets,
  was observed with the Ultraviolet Coronagraph Spectrometer (UVCS)
  aboard the Solar and Heliospheric Observatory (SOHO) satellite. The
  Lyα line profile and spatial distribution are interpreted in terms
  of the theory of bow shocks driven by mass-loading. At the time of
  the observation, the comet was 6.8 R<SUB>⊙</SUB> from the Sun in
  a region of high-speed wind, a region difficult to observe directly
  with the SOHO instruments but an important region for testing models
  of solar wind acceleration and heating. We find a solar wind speed
  below 640 km s<SUP>-1</SUP> and a constraint on the combination of
  solar wind speed and proton temperature. The total energy per proton at
  6.8 R<SUB>⊙</SUB> is 50%-75% of the energy at 1 AU, indicating that
  significant heating occurs at larger radii. The centroid and width
  of the Lyα line generally confirm the predictions of models of the
  cometary bow shock driven by mass-loading as cometary molecules are
  ionized and swept up in the solar wind. We estimate an outgassing rate
  of 20 kg s<SUP>-1</SUP>, which implies an active area of the nucleus
  only about 6.7 m in diameter at 6.8 R<SUB>⊙</SUB>. This is likely
  to be the size of the nucleus, because any inert mantle would have
  probably been blown off during the approach to the Sun.

Title: Ultraviolet Coronagraph Spectrometer Observations of Density
    Fluctuations in the Solar Wind
Authors: Ofman, L.; Romoli, M.; Poletto, G.; Noci, G.; Kohl, J. L.
Bibcode: 1998ApJ...507L.189O
Altcode:
  In the Letter ``Ultraviolet Coronagraph Spectrometer
  Observations of Density Fluctuations in the Solar Wind'' by
  L. Ofman, M. Romoli, G. Poletto, G. Noci, and J. L. Kohl (<A
  href="/abs/1997ApJ...491L.111">ApJ, 491, L111 [1997]</A>), there was
  an error in the data reduction of the polarized brightness (pB). It
  was assumed that the cadence of the data and the exposure time are
  equal. However, the correct cadence is30 s longer than the exposure
  time because of the time it takes the polarizer to change orientation
  between exposures. This error does not affect the main result of the
  Letter, i.e., the detection of quasi-periodic density fluctuations in
  the solar wind. However, the correct cadences of the data in Table 1
  are 30 s longer. This correction can be taken into account in Figure
  1 by multiplying the times by 1.5 and dividing the frequencies by
  the same factor. Thus, the highest peak in the power spectrum is at
  1.8+/-0.07 mHz (the corresponding period is 9.3+/-0.4 minutes). The
  correction factor is 1.1 in Figure 2 because of the longer exposure
  time in this observation.

Title: Physical Structure of a Coronal Streamer in the Closed-Field
    Region as Observed from UVCS/SOHO and SXT/Yohkoh
Authors: Li, J.; Raymond, J. C.; Acton, L. W.; Kohl, J. L.; Romoli,
   M.; Noci, G.; Naletto, G.
Bibcode: 1998ApJ...506..431L
Altcode:
  We analyze a coronal helmet streamer observed on 1996 July 25 using
  instruments aboard two solar spacecraft, the Ultraviolet Coronagraph
  Spectrometer (UVCS) on board Solar and Heliospheric Observatory
  (SOHO) and the Soft X-Ray Telescope (SXT) on board Yohkoh. We derive
  temperatures and electron densities at 1.15 R<SUB>⊙</SUB> from
  SXT/Yohkoh observations. At this height, the streamer temperature is
  about log T (K) = 6.28 +/- 0.05, and the electron density is about
  log n<SUB>e</SUB>(cm<SUP>-3</SUP>) = 8.09 +/- 0.26, while at 1.5
  R<SUB>⊙</SUB> a temperature of log T (K) = 6.2 and a density of log
  n<SUB>e</SUB>(cm<SUP>-3</SUP>) = 7.1 are obtained by UVCS/SOHO. Within
  the measurement uncertainty this suggests a constant temperature from
  the base of the streamer to 1.5 R<SUB>⊙</SUB>. Electron density
  measurements suggest that the gas in the streamer core is close to
  hydrostatic equilibrium. Comparison with potential field models for the
  magnetic field suggests a plasma β larger than 1 in the closed-field
  region in the streamer. In deriving electron densities and temperatures
  from the SXT/Yohkoh data, we include the effects of abundance anomalies
  on the SXT filter response. We use the elemental abundances derived from
  the UVCS/SOHO observations to estimate the first ionization potential
  and gravitational settling effects. We then give the set of abundances
  for the solar corona, which agrees with our observations. In addition,
  we analyzed the SXT data from 6 consecutive days. We found that from
  1996 July 22 to July 27, the physical properties of the streamer are
  nearly constant. We conclude that we may be observing the same loop
  system over 6 days.

Title: The Effect of Temperature Anisotropy on Observations of
    Doppler Dimming and Pumping in the Inner Corona
Authors: Li, Xing; Habbal, Shadia Rifai; Kohl, John L.; Noci, Giancarlo
Bibcode: 1998ApJ...501L.133L
Altcode: 1998astro.ph..5021L
  Recent observations of the spectral line profiles and intensity ratio
  of the O VI λλ1032 and 1037.6 doublet by the Ultraviolet Coronagraph
  Spectrometer (UVCS) on the Solar and Heliospheric Observatory (SOHO),
  made in coronal holes below 3.5 R<SUB>S</SUB>, provide evidence
  for Doppler dimming of the O VI λ1037.6 line and pumping by the
  chromospheric C II λ1037.0182 line. Evidence for a significant kinetic
  temperature anisotropy of O<SUP>5+</SUP> ions was also derived from
  these observations. We show in this Letter how the component of the
  kinetic temperature in the direction perpendicular to the magnetic
  field, for both isotropic and anisotropic temperature distributions,
  affects both the amount of Doppler dimming and pumping. Taking this
  component into account, we further show that the observation of the O
  VI doublet intensity ratio less than unity can be accounted for only
  if pumping by C II λ1036.3367 in addition to C II λ1037.0182 is in
  effect. The inclusion of the C II λ1036.3367 pumping implies that the
  speed of the O<SUP>5+</SUP> ions can reach 400 km s<SUP>-1</SUP> around
  3 R<SUB>S</SUB>, which is significantly higher than the reported UVCS
  values for atomic hydrogen in polar coronal holes. These results imply
  that oxygen ions flow much faster than protons at that heliocentric
  distance.

Title: UVCS/SOHO Empirical Determinations of Anisotropic Velocity
    Distributions in the Solar Corona
Authors: Kohl, J. L.; Noci, G.; Antonucci, E.; Tondello, G.; Huber,
   M. C. E.; Cranmer, S. R.; Strachan, L.; Panasyuk, A. V.; Gardner,
   L. D.; Romoli, M.; Fineschi, S.; Dobrzycka, D.; Raymond, J. C.;
   Nicolosi, P.; Siegmund, O. H. W.; Spadaro, D.; Benna, C.; Ciaravella,
   A.; Giordano, S.; Habbal, S. R.; Karovska, M.; Li, X.; Martin, R.;
   Michels, J. G.; Modigliani, A.; Naletto, G.; O'Neal, R. H.; Pernechele,
   C.; Poletto, G.; Smith, P. L.; Suleiman, R. M.
Bibcode: 1998ApJ...501L.127K
Altcode:
  We present a self-consistent empirical model for several plasma
  parameters of a polar coronal hole near solar minimum, derived from
  observations with the Solar and Heliospheric Observatory Ultraviolet
  Coronagraph Spectrometer. The model describes the radial distribution of
  density for electrons, H<SUP>0</SUP>, and O<SUP>5+</SUP> and the outflow
  velocity and unresolved most probable velocities for H<SUP>0</SUP>
  and O<SUP>5+</SUP> during the period between 1996 November and 1997
  April. In this Letter, we compare observations of H I Lyα and O
  VI λλ1032, 1037 emission lines with spatial models of the plasma
  parameters, and we iterate for optimal consistency between measured and
  synthesized observable quantities. The unexpectedly large line widths
  of H<SUP>0</SUP> atoms and O<SUP>5+</SUP> ions at most radii are the
  result of anisotropic velocity distributions, which are not consistent
  with purely thermal motions or the expected motions from a combination
  of thermal and transverse wave velocities. Above 2 R<SUB>solar</SUB>,
  the observed transverse, most probable speeds for O<SUP>5+</SUP> are
  significantly larger than the corresponding motions for H<SUP>0</SUP>,
  and the outflow velocities of O<SUP>5+</SUP> are also significantly
  larger than the corresponding velocities of H<SUP>0</SUP>. We discuss
  the constraints and implications on various theoretical models of
  coronal heating and acceleration.

Title: Elemental Abundances in Coronal Structures
Authors: Raymond, John C.; Suleiman, Raid; Kohl, John L.; Noci,
   Giancarlo
Bibcode: 1998SSRv...85..283R
Altcode:
  A great deal of evidence for elemental abundance variations among
  different structures in the solar corona has accumulated over the
  years. Many of the observations show changes in the relative abundances
  of high- and low-First Ionization Potential elements, but relatively
  few show the absolute elemental abundances. Recent observations from the
  SOHO satellite give absolute abundances in coronal streamers. Along the
  streamer edges, and at low heights in the streamer, they show roughly
  photospheric abundances for the low-FIP elements, and a factor of 3
  depletion of high-FIP elements. In the streamer core at 1.5 R·, both
  high- and low-FIP elements are depleted by an additional factor of 3,
  which appears to result from gravitational settling.

Title: UVCS/SOHO: The First Two Years
Authors: Cranmer, S. R.; Kohl, J. L.; Noci, G.
Bibcode: 1998SSRv...85..341C
Altcode:
  The SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) has observed
  the extended solar corona between 1 and 10 R· for more than two
  years. We review spectroscopic and polarimetric measurements made
  in coronal holes, equatorial streamers, and coronal mass ejections,
  as well as selected non-solar targets. UVCS/SOHO has provided a great
  amount of empirical information about the physical processes that heat
  and accelerate the solar wind, and about detailed coronal structure
  and evolution.

Title: Absolute Cross Section for Electron Impact Excitation of
    Metastable Si^2+
Authors: Janzen, P. H.; Reisenfeld, D. B.; Gardner, L. D.; Kohl, J. L.
Bibcode: 1998APS..DMP..LP31J
Altcode:
  We have measured the absolute cross section for electron impact
  excitation (EIE) of Si^2+(3s3p ^3P^o - 3s3p ^1P) for energies near
  threshold. A beams modulation technique with inclined electron and ion
  beams was used. The radiation from the excited ions at λ120.6 nm was
  detected using an absolutely calibrated optical system that subtends
  slightly over π steradians. The population of the Si^2+(3s3p ^3P^o)
  metastable state in the incident ion beam was determined using a
  beam attenuation method and by making an absolute measurement of the
  intensity of the λ189.2 nm light from the beam due to radiative decay
  of the metastable state. A metastable fraction of 22.4 ± 2.5% was
  measured. Because of the small metastable fraction, the EIE signal
  is rather small. Nevertheless, the complex resonance structure of
  the cross section is clearly resolved. Research progress and the
  experimental apparatus will be described. This work was supported by
  NASA Supporting Research and Technology Program in Solar Physics grant
  NAG5-5059 and the Smithsonian Astrophysical Observatory.

Title: Absolute Cross Section for Electron Impact Excitation of
    Ground State Si^2+
Authors: Reisenfeld, D. B.; Janzen, P. H.; Gardner, L. D.; Savin,
   D. W.; Kohl, J. L.
Bibcode: 1998APS..DMP..K608R
Altcode:
  We have measured the absolute cross section for electron impact
  excitation (EIE) of Si^2+(3s^2 ^1S - 3s3p ^1P) for energies below
  threshold to 11 eV above. A beams modulation technique with inclined
  electron and ion beams was used, where the radiation from the excited
  ions at λ120.6 nm was detected using an absolutely calibrated optical
  system. The population of the Si^2+(3s3p ^3P^o) metastable state in
  the incident ion beam was determined to be 22.4 ± 2.5%. The data
  have been corrected for contributions to the signal from excitation
  of the metastable state, and for higher energies, from excitation of
  the ground state to levels above the 3s3p ^1P level. The experimental
  0.5 ± 0.05 eV energy spread allowed us to resolve complex resonance
  structure throughout the studied energy range. At the reported 15%
  uncertainty level (90% confidence limit), the measured structure
  and absolute scale of the cross section are in good agreement with
  12-state close-coupling R-matrix calculations(D. C. Griffin et al).,
  Phys. Rev. A 47, 2871 (1993).^,(P. L. Dufton &amp; A. E. Kingston,
  MNRAS 241), 209 (1989).. This work was supported by NASA Supporting
  Research and Technology Program in Solar Physics grants NAGW-1687
  and NAG5-5059, NASA Training Grant NGT-51081 and the Smithsonian
  Astrophysical Observatory.

Title: Ultraviolet Spectroscopy of the Extended Solar Corona with
    UVCS/SOHO
Authors: Kohl, John
Bibcode: 1998APS..DMP..K104K
Altcode:
  The Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and
  Heliospheric Observatory (SOHO) is designed to obtain an empirical
  description of the extended solar corona and its expansion into the
  solar wind. During its first two years of operation, UVCS has been
  used to determine velocity distributions and bulk motions of protons,
  electrons and minor ions; particle densities, and elemental abundances
  from near the base of the solar corona to heliocentric heights up to 10
  solar radii. Measurements of spectral line profiles and comparisons of
  observed intensities with self consistent coronal models are used to
  derive values for the coronal plasma parameters. The measurements are
  challenging the current theories on the composition and acceleration of
  the solar wind. The velocity distributions for coronal ions are found
  to be anisotropic by as much as a factor of 15 and the most probable
  speeds in the direction perpendicular to the coronal magnetic field are
  extremely large reaching values corresponding to temperatures of over
  2 × 10^8 K in a thermalized plasma. Elemental abundances in specific
  coronal structures can be an order of magnitude smaller than in the
  solar photosphere. Similarities between abundances in the corona and
  abundances in fast and slow wind streams provide clues about the coronal
  source regions of the wind. The physical processes and atomic parameters
  required to derive the coronal parameters from the observations will
  be discussed. Current ideas about the theoretical explanation for the
  derived empirical description of the corona will also be described
  briefly. This work is supported by the National Aeronautics and Space
  Administration under grant NAG5-3192 to the Smithsonian Astrophysical
  Observatory, by Agenzia Spaziale Italiana and by Swiss funding agencies.

Title: Study of the Latitudinal Dependence of HI Lyman alpha and OVI
    Emission - Evidence for the Super-Radial Geometry of the Outflow in
    the Polar Coronal Holes
Authors: Dobrzycka, D.; Strachan, L.; Panasyuk, A.; Cranmer, S. R.;
   Kohl, J. L.; Romoli, M.
Bibcode: 1998EOSTr..79..283D
Altcode:
  The observations obtained during the Whole Sun Month (WSM) campaign
  (Aug.10 - Sept.08, 1996) provide us with detailed information about
  the Sun and solar corona near the minimum of solar activity. This data
  set is especially important for analysis of the latitudinal dependence
  of the emission from the solar corona, since at solar minimum the
  polar coronal holes are large, stable structures and streamers are
  long lasting features occupying a narrow region in the equatorial
  plane. We present our analysis of the UVCS/SOHO data acquired during
  the period of the WSM campaign. We describe the distribution of the
  HI Lyman alpha and O VI (1032,1037 A) emission as a function of both
  latitude and radius and derive characteristic plasma parameters like
  velocities along the line of sight and kinetic temperatures. We put
  constraints on the boundaries of the polar coronal holes by modeling
  them with flow tubes that expand radially or super-radially and
  compare our results with constraints from other instruments. We also
  model the latitudinal distribution of the Lyman alpha and O VI line
  intensities assuming outflow either along purely radial or non-radial
  flux tubes. This work was supported by NASA under Grant NAG5-3192 to
  the Smithsonian Astrophysical Observatory, by the Italian Space Agency,
  and by Swiss Funding Agencies.

Title: Acceleration and Heating of the Fast Solar Wind: Diagnostics
    and Theory
Authors: Cranmer, S. R.; Field, G. B.; Noci, G.; Kohl, J. L.
Bibcode: 1998EOSTr..79..278C
Altcode:
  We present empirical models based on UVCS/SOHO observational data
  for several plasma parameters in the fast solar wind emerging
  from near-solar-minimum polar coronal holes. We also discuss the
  constraints on various theoretical processes of coronal heating and
  acceleration, and present preliminary kinetic models of the velocity
  distributions. UVCS/SOHO has measured hydrogen kinetic temperatures
  in polar coronal holes in excess of 3 million K, and O<SUP>5+</SUP>
  ion kinetic temperatures of at least 200 million K. The velocity
  distributions parallel to the open magnetic field are smaller than
  those perpendicular to the field, possibly implying temperature
  anisotropy ratios of order 100 for minor ions. In addition, Doppler
  dimming and pumping of the emission line intensities indicates that the
  O<SUP>5+</SUP> ions may have higher outflow velocities than the protons;
  the ions may reach 500 km/s by a radius of 4 solar radii. We examine
  various features of plasma heating by the dissipation of high-frequency
  ion-cyclotron resonance Alfven waves, which may be the most natural
  physical mechanism to produce the observed plasma conditions. This
  resonant wave damping produces anisotropic velocity-space diffusion and
  a significant outward acceleration in addition to that provided to ions
  by the magnetic mirror force. Because different ions have different
  resonant frequencies, they receive different amounts of heating and
  acceleration as a function of radius. Thus, the more ionic species
  that are observed, the greater the extent in frequency space the wave
  spectrum can be inferred and spatially mapped.

Title: Tomographic Reconstructions of the Corona from UVCS/SOHO
    Synoptic Observations
Authors: Panasyuk, A. V.; Strachan, L.; Finesehi, S.; Gardner, L. D.;
   Raymond, J.; Kohl, J. L.; Antonucci, E.; Giordano, S.; Romoli, M.
Bibcode: 1998ASPC..140..407P
Altcode: 1998ssp..conf..407P
  No abstract at ADS

Title: UVCS/SOHO: The First Two Years
Authors: Cranmer, S. R.; Kohl, J. L.; Noci, G.
Bibcode: 1998sce..conf..341C
Altcode:
  No abstract at ADS

Title: UVCS observations of polar regions
Authors: Poletto, G.; Corti, G.; Romoli, M.; Kohl, J. L.; Noci, G.
Bibcode: 1998ESASP.421...69P
Altcode: 1998sjcp.conf...69P
  In order to facilitate the interpretation of UVCS data, the first
  section of this paper gives a short summary of the mechanisms of line
  formation in the extended corona and of the diagnostic techniques
  adopted to analyze UVCS observations. This allows us to interpret, in
  a semiqualitative way, the morphology of polar regions, as revealed
  by UVCS, which are next illustrated. Results of data analysis,
  i.e. densities, kinetic temperatures and flow speeds at heliocentric
  distances between 1.5 and 3.5 R<SUB>sun</SUB> are then discussed. The
  ensuing scenario has a strong impact on the theories of heating
  and acceleration of the solar wind plasma: we briefly outline the
  theoretical implications emerging from UVCS results and the theories
  which may comply with the observational requirements.

Title: The Impact of UVCS/SOHO Observations on Models of Ion-Cyclotron
    Resonance Heating of the Solar Corona
Authors: Cranmer, Steven R.; Field, George B.; Kohl, John L.
Bibcode: 1998ASPC..154..592C
Altcode: 1998csss...10..592C
  We examine the compatibility between theoretical models and observations
  of the temperatures and anisotropic velocity distributions of hydrogen
  and minor ions in the solar corona. The UVCS instrument on board SOHO
  has measured hydrogen kinetic temperatures along lines of sight in
  coronal holes in excess of 3 x 10<SUP>6</SUP> K, and O^{+5} ion kinetic
  temperatures of at least 2 x 10<SUP>8</SUP> K. In addition, the velocity
  distributions in the radial direction (mainly perpendicular to the
  line of sight) are smaller, possibly implying temperature anisotropies
  of order T<SUB>perp</SUB> / T<SUB>parallel</SUB> ~ 100 for the oxygen
  ions. These properties can be understood only in terms of a mechanism
  which heats and/or accelerates heavier ions more than lighter ones
  (possibly proportionally to m<SUB>ion</SUB><SUP>alpha</SUP>, where
  alpha &gt;~ 1), and preferentially in directions perpendicular to the
  magnetic field. We examine various features of plasma heating by the
  dissipation of high-frequency ion-cyclotron resonance Alfven waves,
  which may be the most natural physical mechanism to produce such
  plasma conditions. We show that a quantitative model should predict
  the spectrum of waves required to reproduce the observations.

Title: Absolute Cross Section for Electron Impact Excitation of
    Ground State Si2+
Authors: Reisenfeld, D. B.; Janzen, P. H.; Gardner, L. D.; Savin,
   D. W.; Kohl, J. L.
Bibcode: 1998lss..work..219R
Altcode:
  No abstract at ADS

Title: The white light polarimeter of SOHO/UVCS
Authors: Romoli, M.; Benna, C.; Fineschi, S.; Gardner, L. D.; Kohl,
   J. L.; Noci, G.
Bibcode: 1998MmSAI..69..703R
Altcode:
  No abstract at ADS

Title: Comparison of SPARTAN and UVCS/SOHO observations.
Authors: Dobrzycka, D.; Strachan, L.; Miralles, M. P.; Kohl, J. L.;
   Gardner, L. D.; Smith, P. L.; Cranmer, S. R.; Guhathakurta, M.;
   Fisher, R.
Bibcode: 1998ASPC..154..601D
Altcode:
  The authors present a comparison of the H I Lyα Spartan Ultraviolet
  Coronal Spectrometer observations of the north and south polar coronal
  holes in 1993 - 1995 with SOHO Ultraviolet Coronograph Spectrometer
  data obtained near solar minimum. These data span several years of
  the declining phase of the current solar cycle. Detailed analysis of
  the data revealed that the average H I Lyα intensities at similar
  heights decreased towards solar minimum in both polar coronal hole
  regions. In 1993 the authors observed a 15% - 40% scatter in the
  intensities measured at the same height but different position angles
  within the same coronal hole. Towards solar minimum the scatter was
  clearly reduced. Also the shape of the Lyα profile changed over
  the last four years. The narrow component present in 1993 data being
  attributed to the contribution from streamers along the line-of-sight
  disappeared in 1996/97. They interpret these effects as mainly due to
  a decrease in the number of high latitude streamers. At solar minimum
  streamers occupy mostly the equatorial region and do not contribute
  to the line-of-sight intensity as much as in 1993.

Title: Ultraviolet Spectroscopy of a Coronal Mass Ejection
Authors: Ciaravella, A.; Raymond, J. C.; Fineschi, S.; Romoli,
   M.; Benna, C.; Gardner, L.; Giordano, S.; Michels, J.; O'Neal, R.;
   Antonucci, E.; Kohl, J.; Noci, G.
Bibcode: 1998ASPC..150..370C
Altcode: 1998npsp.conf..370C; 1998IAUCo.167..370C
  No abstract at ADS

Title: Absolute Cross Section for Electron Impact Excitation of
    Metastable Si2+
Authors: Janzen, P. H.; Reisenfeld, D. B.; Gardner, L. D.; Kohl, J. L.
Bibcode: 1998lss..work..169J
Altcode:
  No abstract at ADS

Title: Comparison of SPARTAN and UVCS/SOHO Observations
Authors: Dobrzycka, D.; Strachan, L.; Miralles, M. P.; Kohl, J. L.;
   Gardner, L. D.; Smith, P. L.; Cranmer, S. R.; Guhathakurta, M.;
   Fisher, R.
Bibcode: 1998ASPC..154..607D
Altcode: 1998csss...10..607D
  We present a comparison of the H 1 Lyalpha Spartan Ultraviolet Coronal
  Spectrometer observations of the north and south polar coronal holes in
  1993-1995 with SOHO Ultraviolet Coronograph Spectrometer data obtained
  near solar minimum. These data span several years of the declining phase
  of the current solar cycle. Detailed analysis of the data revealed that
  the average H 1 Lyalpha intensities at similar heights decreased towards
  solar minimum in both polar coronal hole regions. In 1993 we observed
  a 15% - 40% scatter in the intensities measured at the same height but
  different position angles within the same coronal hole. Towards solar
  minimum the scatter was clearly reduced. Also the shape of the Lyalpha
  profile changed over the last four years. The narrow component present
  in 1993 data being attributed to the contribution from streamers along
  the line-of-sight disappeared in 1996/97. We interpret these effects as
  mainly due to a decrease in the number of high latitude streamers. At
  solar minimum streamers occupy mostly the equatorial region and do
  not contribute to the line-of-sight intensity as much as in 1993.

Title: Elemental Abundances in Coronal Structures
Authors: Raymond, J.; Suleiman, R.; Kohl, J. L.; Noci, G.
Bibcode: 1998sce..conf..283R
Altcode:
  No abstract at ADS

Title: Velocity Fields in the Solar Corona during Mass Ejections as
    Observed with UVCS-SOHO
Authors: Antonucci, E.; Kohl, J. L.; Noci, G.; Tondello, G.; Huber,
   M. C. E.; Gardner, L. D.; Nicolosi, P.; Giordano, S.; Spadaro, D.;
   Ciaravella, A.; Raymond, C. J.; Naletto, G.; Fineschi, S.; Romoli, M.;
   Siegmund, O. H. W.; Benna, C.; Michels, J.; Modigliani, A.; Panasyuk,
   A.; Pernechele, C.; Smith, P. L.; Strachan, L.; Ventura, R.
Bibcode: 1997ApJ...490L.183A
Altcode:
  This Letter presents the observations of the first two coronal mass
  ejections (CMEs) obtained with the Ultraviolet Coronagraph Spectrometer
  of SOHO. Both CMEs were observed at high spectral resolution in the
  ultraviolet domain. The first event on 1996 June 6-7 was observed in H I
  Lyα λ1216 and Lyβ λ1026, O VI λλ1032 and 1037, Si XII λλ499 and
  521 and imaged within 1.5 and 5 R<SUB>solar</SUB>. The second event on
  1996 December 23 was observed in several H I lines and cool lines such
  as C III λ977, N III λλ990-992, and O V λ630. The analysis of line
  profiles has allowed us to determine the line-of-sight velocities of the
  extended corona during a mass ejection. In particular there is evidence
  for mass motions consistent with untwisting magnetic fields around an
  erupted flux tube in one of the events and line of sight velocities of
  200 km s<SUP>-1</SUP> in the early phase of the second event presumably
  related to the expansion of the leading arch of the transient.

Title: Solar Wind Acceleration in the Solar Corona
Authors: Giordano, S.; Antonucci, E.; Benna, C.; Kohl, J. L.; Noci,
   G.; Michels, J.; Fineschi, S.
Bibcode: 1997ESASP.415..327G
Altcode: 1997cpsh.conf..327G
  No abstract at ADS

Title: Determination of 3D Coronal Structures from UVCS/SOHO Synoptic
    Observations
Authors: Strachan, L.; Panasyuk, A. V.; Fineschi, S.; Gardner, L. D.;
   Raymond, J. C.; ANtonucci, E.; Giordano, S.; Romoli, M.; Noci, G.;
   Kohl, J. L.
Bibcode: 1997ESASP.415..539S
Altcode: 1997cpsh.conf..539S
  No abstract at ADS

Title: Ultraviolet Coronagraph Spectrometer Observations of Density
    Fluctuations in the Solar Wind
Authors: Ofman, L.; Romoli, M.; Poletto, G.; Noci, G.; Kohl, J. L.
Bibcode: 1997ApJ...491L.111O
Altcode:
  Recent Ultraviolet Coronagraph Spectrometer (UVCS) white-light
  channel (WLC) observations on board the Solar and Heliospheric
  Observatory (SOHO) indicate quasi-periodic variations in the
  polarized brightness (pB) in the polar coronal holes. This is
  the first observation of possible signatures of compressional
  waves high above the limb (at heliocentric distances in the range
  1.9-2.45 R<SUB>solar</SUB>). The Fourier power spectrum of the
  pB time series at 1.9 R<SUB>solar</SUB> shows significant peak
  at about 6 minutes and possible fluctuations on longer timescales
  (20-50 minutes). The observation at 1.9 R<SUB>solar</SUB> is the only
  currently available WLC data set with sufficient cadence to resolve
  the 6 minute period. These preliminary observations may result from
  density fluctuations caused by compressional waves propagating in
  polar coronal holes. We stress that our results are preliminary, and
  we plan future high-cadence observations in both plume and interplume
  regions of coronal holes. Recently, Ofman &amp; Davila used a 2.5 D
  MHD model and found that Alfvén waves with an amplitude of 20-70 km
  s<SUP>-1</SUP> at the base of the coronal hole can generate nonlinear,
  high-amplitude compressional waves that can contribute significantly to
  the acceleration of the fast solar wind. The nonlinear solitary-like
  waves appear as fluctuations in the density and the radial outflow
  velocity and contribute significantly to solar wind acceleration
  in open magnetic field structures. The motivation for the reported
  observations is the MHD model prediction.

Title: A User's Guide to UVCS/SOHO
Authors: Kohl, J. L.; Noci, G.; Cranmer, S. R.; Fineschi, S.; Gardner,
   L. D.; Halas, C. D.; Smith, P. L.; Strachan, L.; Suleiman, R. M.
Bibcode: 1997AAS...191.7309K
Altcode: 1997BAAS...29Q1322K
  The SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) is currently
  being used to observe the extended solar corona between 1 and 10
  heliocentric radii. In its first two years of operation, UVCS/SOHO
  has made spectroscopic measurements leading to the determination of
  densities, velocities, temperatures, and elemental abundances in coronal
  holes, equatorial streamers, and coronal mass ejections. Observations
  of selected non-solar targets, such as near-ecliptic stars, planets,
  comets, and interplanetary hydrogen and helium, have also produced
  interesting astronomical results. This poster presents a brief
  review of the UVCS/SOHO spectroscopic and polarimetric diagnostic
  capabilities, highlighted by pertinent observational data. Most
  importantly, we summarize the procedures that have been designed
  to allow UVCS/SOHO data to be used by a wide array of researchers,
  and invite participation in this unique investigation. Scientists
  interested in UVCS/SOHO observations are encouraged to fill
  out the ``Get Involved'' questionnaire located on the WWW at:
  http://cfa-www.harvard.edu/uvcs/ This work is supported by the National
  Aeronautics and Space Administration under grant NAG5-3192 to the
  Smithsonian Astrophysical Observatory, by Agenzia Spaziale Italiana,
  and by Swiss funding agencies.

Title: Ultraviolet Observations of Coronal Mass Ejections
Authors: Ciaravella, A.; Raymond, J. C.; Benna, C.; Fineschi, S.;
   Gardner, L. D.; Giordano, S.; O'Neal, R. H.; Reale, F.; Romoli, M.;
   Michels, J.; Antonucci, E.; Kohl, J. L.; Noci, G.
Bibcode: 1997ESASP.415..543C
Altcode: 1997cpsh.conf..543C
  No abstract at ADS

Title: Ultraviolet Coronagraph Spectrometer Observation of the 1996
    December 23 Coronal Mass Ejection
Authors: Ciaravella, A.; Raymond, J. C.; Fineschi, S.; Romoli,
   M.; Benna, C.; Gardner, L.; Giordano, S.; Michels, J.; O'Neal, R.;
   Antonucci, E.; Kohl, J.; Noci, G.
Bibcode: 1997ApJ...491L..59C
Altcode:
  The Ultraviolet Coronagraph Spectrometer (UVCS) aboard the Solar
  and Heliospheric Observatory (SOHO) observed a spectacular coronal
  mass ejection (CME) caused by a prominence eruption on 1996 December
  23. The evolution of the ejected prominence material was followed for
  1 hr and 50 minutes. The observation consists of a series of 5 minute
  exposures, at a fixed heliocentric distance of 1.5 R<SUB>solar</SUB>
  in several spectral ranges. The Lyman lines of hydrogen brighten
  more than 2 orders of magnitude during the CME. The C III 977.02 Å
  line is very bright, and many other low-temperature lines have been
  detected. Line intensities and profiles provide important diagnostics
  for the physical and dynamical parameters of the ejected plasma. Lines
  widths show nonthermal line broadening due to a plasma expansion with
  velocity larger than 50 km s<SUP>-1</SUP>. The Lyα inside the CME
  region shows red and blue shifts, up to 0.2 Å (50 km s<SUP>-1</SUP>)
  and 0.8 Å (200 km s<SUP>-1</SUP>), respectively. A preliminary estimate
  shows a flat emission measure distribution 3 or 4 orders of magnitude
  smaller than typical prominence emission measures. Essentially the same
  structure in space and velocity is seen in the Lyman lines, in C III
  (10<SUP>5</SUP> K) and in O VI (3×10<SUP>5</SUP> K).

Title: Absolute Abundances in Streamers from UVCS
Authors: Raymond, J. C.; Suleiman, R. M.; van Ballegooijen, A. A.;
   Kohl, J. L.
Bibcode: 1997ESASP.415..383R
Altcode: 1997cpsh.conf..383R
  The Ultraviolet Coronagraph Spectrometer on SOHO covers the 940-1350
  Angstrom range as well as the 470-630 Angstrom range in second
  order. It has detected coronal emission lines of H, N, O, Mg, Al, Si,
  S, Ar, Ca, Fe and Ni in coronal streamers. We are able to determine
  the ionization state and the absolute elemental abundances in the
  gas. There is a strong First Ionization Potential (FIP) dependence in
  the abundances. Oxygen is depleted relative to hydrogen, by a full order
  of magnitude for oxygen in the center of a quiescent streamer. Here, we
  extend the earlier work by considering greater heights in the streamer
  and by estimating the projection effects (the line of sight passing
  through the streamer edges). We suggest that the FIP fractionation
  occurs in the chromosphere, but that in addition gravitational settling
  produces an overall depletion at large heights in the closed-field
  region. We present numerical results of diffusion models.

Title: The Impact of UVCS/SOHO Observations on Models of Ion-Cyclotron
    Resonance Heating of the Solar Corona
Authors: Cranmer, S. R.; Field, G. B.; Noci, G.; Kohl, J. L.
Bibcode: 1997ESASP.415...89C
Altcode: 1997cpsh.conf...89C
  No abstract at ADS

Title: The Impact of Ion-Cyclotron Wave Dissipation on Minor Ion
    Velocity Distributions in the Solar Corona
Authors: Cranmer, S. R.; Field, G. B.; Noci, G.; Kohl, J. L.
Bibcode: 1997AAS...191.7411C
Altcode: 1997BAAS...29.1325C
  We present theoretical models of the acceleration and heating
  of minor ions in the solar wind, as well as detailed anisotropic
  velocity distribution functions computed numerically by solving the
  Boltzmann transport equation. We examine the compatibility between
  these models and spectroscopic measurements of the velocities
  and kinetic temperatures of various particle species in the solar
  corona. The SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO)
  has measured hydrogen kinetic temperatures in polar coronal holes in
  excess of 3 million K, and O VI ion kinetic temperatures of at least
  200 million K. In addition, the velocity distributions parallel to
  the open magnetic field are smaller than those perpendicular to the
  field, possibly implying temperature anisotropy ratios of order 100
  for minor ions. We examine various features of plasma heating by the
  dissipation of high-frequency ion-cyclotron resonance Alfven waves,
  which may be the most natural physical mechanism to produce the
  observed plasma conditions. The modeled ion velocity distributions
  depend sensitively on the assumed amplitudes and frequencies of the
  waves, and these computations can be used to accurately predict many
  quantitative features of the wave power spectrum. Indeed, the more
  ionic species that are observed spectroscopically, the greater the
  extent in frequency space the wave spectrum can be inferred. This work
  is supported by the National Aeronautics and Space Administration
  under grant NAG5-3192 to the Smithsonian Astrophysical Observatory,
  by Agenzia Spaziale Italiana, and by Swiss funding agencies.

Title: Origins of the Slow and the Ubiquitous Fast Solar Wind
Authors: Habbal, S. R.; Woo, R.; Fineschi, S.; O'Neal, R.; Kohl, J.;
   Noci, G.; Korendyke, C.
Bibcode: 1997ApJ...489L.103H
Altcode: 1997astro.ph..9021H
  We present in this Letter the first coordinated radio occultation
  measurements and ultraviolet observations of the inner corona below
  5.5R<SUB>s</SUB>, obtained during the Galileo solar conjunction in
  1997 January, to establish the origin of the slow solar wind. Limits
  on the flow speed are derived from the Doppler dimming of the
  resonantly scattered component of the oxygen 1032 and 1037.6 Å
  lines as measured with the ultraviolet coronagraph spectrometer
  (UVCS) on the Solar and Heliospheric Observatory (SOHO). White light
  images of the corona from the large-angle spectroscopic coronagraph
  (LASCO) on SOHO taken simultaneously are used to place the Doppler
  radio scintillation and ultraviolet measurements in the context of
  coronal structures. These combined observations provide the first
  direct confirmation of the view recently proposed by Woo &amp; Martin
  that the slow solar wind is associated with the axes, also known as
  stalks, of streamers. Furthermore, the ultraviolet observations also
  show how the fast solar wind is ubiquitous in the inner corona and
  that a velocity shear between the fast and slow solar wind develops
  along the streamer stalks.

Title: Composition of Coronal Streamers from the SOHO Ultraviolet
    Coronagraph Spectrometer
Authors: Raymond, J. C.; Kohl, J. L.; Noci, G.; Antonucci, E.;
   Tondello, G.; Huber, M. C. E.; Gardner, L. D.; Nicolosi, P.; Fineschi,
   S.; Romoli, M.; Spadaro, D.; Siegmund, O. H. W.; Benna, C.; Ciaravella,
   A.; Cranmer, S.; Giordano, S.; Karovska, M.; Martin, R.; Michels, J.;
   Modigliani, A.; Naletto, G.; Panasyuk, A.; Pernechele, C.; Poletto,
   G.; Smith, Peter L.; Suleiman, R. M.; Strachan, L.
Bibcode: 1997SoPh..175..645R
Altcode:
  The Ultraviolet Coronagraph Spectrometer on the SOHO satellite covers
  the 940-1350 Å range as well as the 470-630 Å range in second
  order. It has detected coronal emission lines of H, N, O, Mg, Al, Si,
  S, Ar, Ca, Fe, and Ni, particularly in coronal streamers. Resonance
  scattering of emission lines from the solar disk dominates the
  intensities of a few lines, but electron collisional excitation produces
  most of the lines observed. Resonance, intercombination and forbidden
  lines are seen, and their relative line intensities are diagnostics
  for the ionization state and elemental abundances of the coronal gas.

Title: First Results from the SOHO Ultraviolet Coronagraph
    Spectrometer
Authors: Kohl, J. L.; Noci, G.; Antonucci, E.; Tondello, G.; Huber,
   M. C. E.; Gardner, L. D.; Nicolosi, P.; Strachan, L.; Fineschi, S.;
   Raymond, J. C.; Romoli, M.; Spadaro, D.; Panasyuk, A.; Siegmund,
   O. H. W.; Benna, C.; Ciaravella, A.; Cranmer, S. R.; Giordano, S.;
   Karovska, M.; Martin, R.; Michels, J.; Modigliani, A.; Naletto, G.;
   Pernechele, C.; Poletto, G.; Smith, P. L.
Bibcode: 1997SoPh..175..613K
Altcode:
  The SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) is being
  used to observe the extended solar corona from 1.25 to 10 R⊙ from
  Sun center. Initial observations of polar coronal holes and equatorial
  streamers are described. The observations include measurements of
  spectral line profiles for HI Lα and Lβ, Ovi 1032 Å and 1037 Å,
  Mgx 625 Å, Fexii 1242 Å and several others. Intensities for Mgx
  610 Å, Sixii 499 Å, and 520 Å, Sx 1196 Å, and 22 others have been
  observed. Preliminary results for derived H<SUP>0</SUP>, O<SUP>5+</SUP>,
  Mg<SUB>9+</SUB>, and Fe<SUP>11+</SUP> velocity distributions and initial
  indications of outflow velocities for O<SUP>5+</SUP> are described. In
  streamers, the H<SUP>0</SUP> velocity distribution along the line of
  sight (specified by the value at e<SUP>-1</SUP>, along the line of
  sight) decreases from a maximum value of about 180 km s<SUP>-1</SUP>
  at 2 R⊙ to about 140 km s<SUP>-1</SUP> at 8 R⊙. The value for
  O<SUP>5+</SUP> increases with height reaching a value of 150 km
  s<SUP>-1</SUP> at 4.7 R⊙. In polar coronal holes, the O<SUP>5+</SUP>
  velocity at e<SUP>-1</SUP> is about equal to that of H<SUP>0</SUP>
  at 1.7 R⊙ and significantly larger at 2.1 R⊙. The O<SUP>5+</SUP>
  in both streamers and coronal holes were found to have anisotropic
  velocity distributions with the smaller values in the radial direction.

Title: Empirical Models of the Extended Solar Corona
Authors: Kohl, J. L.; Noci, G.; Antonucci, E.; Ciaravella, A.;
   Cranmer, S.; Dobrzycka, D.; Fineschi, S.; Gardner, L. D.; Huber,
   M. C. E.; Panasyuk, A.; Raymond, J. C.; Strachan, L.
Bibcode: 1997SPD....28.0303K
Altcode: 1997BAAS...29..907K
  Ultraviolet spectroscopy is being used to produce self consistent
  empirical models of polar coronal holes and equatorial streamers in the
  extended solar corona. The models are intended to provide experimental
  values for many of the primary plasma parameters of the extended corona,
  which can then be used to constrain theoretical coronal and solar
  wind models. The empirical models are based on synoptic observations
  and other measurements of spectral line profiles and intensities of
  H I Lyalpha , O VI 1032 Angstroms and 1037 Angstroms, Fe XII 1242
  Angstroms, Mg X 625 Angstroms and several others. Information about
  velocity distributions, outflow velocities, densities and elemental
  abundances as derived from the observations are specified in the
  models. The models used to specify the empirically derived parameters
  include a description of well established theoretical processes such
  as those controlling ionization balance, collisional excitation,
  and resonant scattering. They do not include any descriptions of
  less well established processes such as heating functions, transverse
  wave motions or direct momentum deposition by waves. The intent is to
  provide, to the maximum extent possible, empirical descriptions that
  can be used, together with theoretical models, to help identify the
  dominant physical processes responsible for coronal heating, solar wind
  acceleration and the chemical composition of the solar wind. This work
  is supported by NASA Grant NAG5-3192 to the Smithsonian Astrophysical
  Observatory, the Italian Space Agency and Swiss funding sources.

Title: UVCS/SOHO Synoptic Observations of the Extended Corona during
    the Whole Sun Month Campaign
Authors: Strachan, L.; Fineschi, S.; Gardner, L. D.; Panasyuk, A. V.;
   Kohl, J. L.; Antonucci, E.; Giordano, S.; Romoli, M.
Bibcode: 1997SPD....28.0122S
Altcode: 1997BAAS...29..883S
  Daily synoptic observations were made with UVCS/SOHO during the Whole
  Sun Month (10 August to 8 September 1996) in order to characterize
  the large-scale spatial distributions of plasma parameters in the
  solar corona from 1.5 to 3 solar radii. We use observed line profiles
  and intensities of H I Lyman alpha and O VI 1032/1037 Angstroms,
  and white light polarized brightness measurements to derive physical
  properties of the plasma in the solar wind acceleration region. Line of
  sight velocity distributions and bulk outflow velocities for neutral
  hydrogen and for O({5) +}, and electron densities can be derived from
  these measurements. We show some results from the on-going effort and
  present some of these data as synoptic maps. The ultimate goal of this
  work is to produce a data set that can be used in developing empirical
  models that describe the solar minimum conditions of the extended
  corona. This work is supported by NASA under Grant NAG5-3192 to the
  Smithsonian Astrophysical Observatory, by the Italian Space Agency,
  and by Swiss funding sources.

Title: Absolute Elemental Abundances in Streamers
Authors: Raymond, J. C.; Kohl, J.; Suleiman, R.; Ciaravella, A.;
   Fineschi, S.; Gardner, L.; Panasyuk, A.; Strachan, L.; Noci, G.;
   Antonucci, E.; Nicolosi, P.; Naletto, G.; Giordano, S.; Benna, C.
Bibcode: 1997SPD....28.0114R
Altcode: 1997BAAS...29..881R
  The UVCS instrument aboard the SOHO satellite has measured the
  intensities of emission lines of H, N, O, Mg, Al, S, Ar, Ca ,Fe and Ni
  at 1.5 solar radii in a quiescent equatorial helmet streamer and in an
  active region streamer. The First Ionization Potential (FIP) effect is
  clearly seen. Low FIP elements show nearly photospheric abundances above
  the active region and along the edges of the equatorial streamer, while
  high FIP elements are depleted by a factor of 2-3. Near the center of
  the streamer, presumably the closed field region, the low-FIP elements
  are at about 1/3 photospheric abundances, and the high FIP elements
  are near 1/10 their photospheric values.

Title: Expansion Factors in Coronal Holes and Plume/Interplume
    UVCS Observations
Authors: Poletto, G.; Corti, G.; Noci, G.; Kohl, J.; Suess, S.
Bibcode: 1997SPD....28.0108P
Altcode: 1997BAAS...29..880P
  We show that expansion factors in plumes and coronal hole areas devoid
  of plumes are nearly equal because the plasma beta is &lt;&lt;1. Hence,
  the overall coronal hole expansion factor is equal to the expansion
  factors of its densest structures. UVCS plume and interplume
  observations of coronal holes are illustrated, with the purpose of
  showing the data capabilities. Integration along the line of sight,
  through a medium containing high and low pressure regions, and the
  rapid decrease with heliocentric distance of plume intensity, presently
  hinder an observational determination of the expansion factors between
  1.5 and 2 solar radii.

Title: Comparison of SPARTAN and UVCS/SOHO Observations
Authors: Dobrzycka, D.; Strachan, L.; Kohl, J. L.; Gardner, L. D.;
   Smith, P. L.; Cranmer, S. R.; Guhathakurta, M.; Fisher, R.
Bibcode: 1997EOSTr..78..242D
Altcode:
  Three SPARTAN flights in 1993, 1994, and 1995 provided us with
  observations of HI Lyman alpha in the south and north polar coronal
  hole regions. These data span several years of the declining phase of
  the current solar cycle. We analyzed the data using various diagnostic
  techniques and obtained strong constraints on the geometry of coronal
  holes, electron density distributions, hydrogen velocity distributions
  and outflow velocities. We compare SPARTAN HI Lyman alpha observations
  with UVCS/SOHO data obtained in solar minimum to characterize changes
  of the plasma parameters in the polar coronal holes over a four year
  period. This work is supported by NASA under Grant NAG 5-613 to the
  Smithsonian Astrophysical Observatory and by NASA under Grant NAG5-3192
  to the Smithsonian Astrophysical Observatory, by the Italian Space
  Agency, and by Swiss Funding Agencies.

Title: Evidence for Nonradial Solar Wind Acceleration in Magnetostatic
    Coronal Holes
Authors: Cranmer, S. R.; Strachan, L.; Romoli, M.; Dobrzycka, D.;
   Panasyuk, A. V.; Kohl, J. L.
Bibcode: 1997EOSTr..78..258C
Altcode:
  We compare UVCS/SOHO observations of densities and outflow velocities
  in polar coronal holes with theoretical mass-conservation models of an
  idealized force-free magnetostatic geometry. Open flux tubes bordering
  the closed-field streamer belt initially expand much more rapidly than
  flux tubes over the poles, then turn nearly radial and expandless
  rapidly. In the past, this variation in the super radial expansion
  factor has been inversely correlated with solar wind velocity at 1 AU,
  but we find an even stronger inverse correlation in the acceleration
  region of the solar wind (1 to 10 solar radii). A considerable
  reduction in the wind speed of low-latitude flux tubes, compared with
  those over the poles, results in a geometry-dependent variation in the
  Doppler dimming of UV resonance lines such as H I Lyman alpha. Thus,
  we are able to use these emission diagnostics not only to infer the
  magnitude of the solar wind velocity, but also to map out the geometry
  of the solar wind emerging from large polar coronal holes. This work is
  supported by NASA under Grant NAG5-3192 to the Smithsonian Astrophysical
  Observatory, by the Italian Space Agency, and by Switzerland.

Title: Optical performances of the Ultraviolet Coronagraph
    Spectrometer of the Solar Heliospheric Observatory
Authors: Pernechele, Claudio; Naletto, Giampiero; Nicolosi,
   Piergiorgio; Tondello, Giuseppe; Fineschi, Silvano; Romoli, Marco;
   Noci, Giancarlo; Spadaro, Daniele; Kohl, John L.
Bibcode: 1997ApOpt..36..813P
Altcode:
  No abstract at ADS

Title: Plume and interplume regions and solar wind acceleration in
    polar coronal holes between 1.5 and 3.5 R
Authors: Giordano, S.; Antonucci, E.; Benna, C.; Romoli, M.; Noci,
   G.; Kohl, J. L.; Fineschi, S.; Michels, J.; Naletto, G.
Bibcode: 1997ESASP.404..413G
Altcode: 1997cswn.conf..413G
  No abstract at ADS

Title: Ultraviolet spectroscopy of a coronal mass ejection with UVCS
Authors: Ciaravella, A.; Raymond, J.; Fineschi, S.; Romoli, M.; Benna,
   C.; Gardner, L.; Giordano, S.; O'Neal, R.; Michels, J.; Antonucci,
   E.; Noci, G.; Kohl, J.
Bibcode: 1997ESASP.404..279C
Altcode: 1997cswn.conf..279C
  No abstract at ADS

Title: Intercomparison between UVCS/WLC and LASCO/C2 measured
    polarized brightness
Authors: Romoli, M.; Biesecker, D.; Benna, C.; Fineschi, S.; Lamy,
   P. L.; Llebaria, A.; Kohl, J. L.; Noci, G.
Bibcode: 1997ESASP.404..637R
Altcode: 1997cswn.conf..637R
  No abstract at ADS

Title: Signature of open magnetic field lines in the extended solar
    corona and of solar wind acceleration
Authors: Antonucci, E.; Giordano, S.; Benna, C.; Kohl, J. L.; Noci,
   G.; Michels, J.; Fineschi, S.
Bibcode: 1997ESASP.404..175A
Altcode: 1997cswn.conf..175A
  No abstract at ADS

Title: KCorona polarized brightness and electron density measurement
    with the visible light polarimeter of UVCS
Authors: Romoli, M.; Benna, C.; Cranmer, S.; Fineschi, S.; Gardner,
   L. D.; Strachan, L.; Kohl, J. L.; Noci, G.
Bibcode: 1997ESASP.404..633R
Altcode: 1997cswn.conf..633R
  No abstract at ADS

Title: UVCS/SOHO empirical models of solar coronal holes
Authors: Cranmer, S. R.; Kohl, J. L.; Noci, G.; Strachan, L.;
   Panasyuk, A. V.; Romoli, M.; Fineschi, S.; Dobrzycka, D.; Raymond,
   J. C.; Suleiman, R. M.; O'Neal, R. H.
Bibcode: 1997ESASP.404..295C
Altcode: 1997cswn.conf..295C
  No abstract at ADS

Title: Possible Signatures of Nonlinear MHD Waves in the Solar Wind:
    UVCS Observatio ns and Models
Authors: Ofman, L.; Romoli, M.; Davila, J. M.; Poletto, G.; Kohl,
   J.; Noci, G.
Bibcode: 1997ESASP.404..571O
Altcode: 1997cswn.conf..571O
  No abstract at ADS

Title: Spectroscopic observations of the extended corona during the
    SOHO whole sun month
Authors: Strachan, L.; Raymond, J. C.; Panasyuk, A. V.; Fineschi,
   S.; Gardner, L. D.; Antonucci, E.; Giordano, S.; Romoli, M.; Noci,
   G.; Kohl, J. L.
Bibcode: 1997ESASP.404..691S
Altcode: 1997cswn.conf..691S
  No abstract at ADS

Title: First Results from UVCS: Dynamics of the Extended Corona
Authors: Antonucci, E.; Noci, G.; Kohl, J. L.; Tondello, G.; Huber,
   M. C. E.; Giordano, S.; Benna, C.; Ciaravella, A.; Fineschi, S.;
   Gardner, L. D.; Martin, R.; Michels, J.; Naletto, G.; Nicolosi, P.;
   Panasyuk, A.; Raymond, C. J.; Romoli, M.; Spadaro, D.; Strachan, L.;
   van Ballegooijen, A.
Bibcode: 1997ASPC..118..273A
Altcode: 1997fasp.conf..273A
  The Ultraviolet Coronagraph Spectrometer (UVCS) started to observe
  the Sun at the end of January 1996. Here we present a selection of
  results obtained with the UVCS in the first months of operation. UV
  spectral line profiles in coronal holes, and in general in regions
  with open magnetic field lines, are much broader than in closed
  field line regions; that is, line-of-sight velocities are much
  larger in open field lines . Polar plumes have narrower profiles
  than interplume regions. The O VI ratio diagnostics indicates that in
  polar coronal holes the outflow velocity is progressively increasing
  with heliodistance and exceeds 100 km/sec near 2--2.5 solar radii. A
  coronal mass ejection observation has revealed line--of--sight plasma
  motions of 100 km/sec and a complex dynamics.

Title: SOHO observations of the north polar solar wind
Authors: Peres, G.; Ciaravella, A.; Betta, R.; Orlando, S.; Reale,
   F.; Kohl, J.; Noci, G.; Fineschi, S.; Romoli, M.; Brekke, P.; Fludra,
   A.; Gurman, J. B.; Lemaire, P.; Schuhle, U.
Bibcode: 1997ESASP.404..587P
Altcode: 1997cswn.conf..587P
  No abstract at ADS

Title: First results from UVCS/SOHO
Authors: Noci, G.; Kohl, J. L.; Antonucci, E.; Tondello, G.; Huber,
   M. C. E.; Fineschi, S.; Gardner, L. D.; Naletto, G.; Nicolosi, P.;
   Raymond, J. C.; Romoli, M.; Spadaro, D.; Siegmund, O. H. W.; Benna, C.;
   Ciaravella, A.; Giordano, S.; Michels, J.; Modigliani, A.; Panasyuk,
   A.; Pernechele, C.; Poletto, G.; Smith, P. L.; Strachan, L.
Bibcode: 1997AdSpR..20.2219N
Altcode:
  We present here the first results obtained by the Ultraviolet
  Coronagraph Spectrometer (UVCS) operating on board the SOHO
  satellite. The UVCS started to observe the extended corona at the end
  of January 1996; it routinely obtains coronal spectra in the 1145 A˚ -
  1287 A˚, 984 A˚ - 1080 A˚ ranges, and intensity data in the visible
  continuum. Through the composition of slit images it also produces
  monocromatic images of the extended corona. The performance of the
  instrument is excellent and the data obtained up to now are of great
  interest. We briefly describe preliminary results concerning polar
  coronal holes, streamers and a coronal mass ejection, in particular: the
  very large r.m.s. velocities of ions in polar holes (hundreds km/sec
  for OVI and MgX); the puzzling difference between the HI Ly-alpha
  image and that in the OVI resonance doublet, for most streamers; the
  different signatures of the core and external layers of the streamers
  in the width of the ion lines and in the OVI doublet ratio, indicating
  larger line-of-sight (l.o.s.) and outflow velocities in the latter.

Title: Physical Parameters in Plume and Interplume Regions from
    UVCS Observations
Authors: Corti, G.; Poletto, G.; Romoli, M.; Michels, J.; Kohl, J.;
   Noci, G.
Bibcode: 1997ESASP.404..289C
Altcode: 1997cswn.conf..289C
  No abstract at ADS

Title: The quiescent corona and slow solar wind
Authors: Noci, G.; Kohl, J. L.; Antonucci, E.; Tondello, G.; Huber,
   M. C. E.; Fineschi, S.; Gardner, L. D.; Korendyke, C. M.; Nicolosi,
   P.; Romoli, M.; Spadaro, D.; Maccari, L.; Raymond, J. C.; Siegmund,
   O. H. W.; Benna, C.; Ciaravella, A.; Giordano, S.; Michels, J.;
   Modigliani, A.; Naletto, G.; Panasyuk, A.; Pernechele, C.; Poletto,
   G.; Smith, P. L.; Strachan, L.
Bibcode: 1997ESASP.404...75N
Altcode: 1997cswn.conf...75N; 1997soho....5...75N
  No abstract at ADS

Title: UV spectroscopy of the extended solar corona: Results from
    UVCS/Spartan
Authors: Strachan, Leonard; Gardner, Larry D.; Smith, Peter L.; Kohl,
   John L.
Bibcode: 1997AIPC..385..113S
Altcode: 1997recs.conf..113S
  Remote sensing of the solar corona using ultraviolet spectroscopy can
  be used to characterize the physical state of the plasma along a wide
  region around the trajectory of a near-Sun flyby spacecraft (solar
  probe). Data from such an instrument can be used to separate spatial
  from temporal variations in the data received from in situ instruments
  aboard the probe. We present results from the UVCS/Spartan space
  shuttle missions in order to show examples of diagnostic techniques
  that can be used to determine velocity distributions and bulk outflow
  velocities of protons and minor ions in the solar wind.

Title: Stray light, radiometric, and spectral characterization of
UVCS/SOHO: laboratory calibration and flight performance
Authors: Gardner, Larry D.; Kohl, J. L.; Daigneau, P. S.; Dennis,
   E. F.; Fineschi, Silvano; Michels, J.; Nystrom, George U.;
   Panasyuk, Alexander; Raymond, John C.; Reisenfeld, D. J.; Smith,
   Peter L.; Strachan, Leonard; Suleiman, R.; Noci, G. C.; Romoli, Marco;
   Ciaravella, A.; Modigliani, A.; Huber, Martin C.; Antonucci, E.; Benna,
   C.; Giordano, S.; Tondello, Giuseppe; Nicolosi, Piergiorgio; Naletto,
   Giampiero; Pernechele, Claudio; Spadaro, D.; Siegmund, Oswald H.;
   Allegra, A.; Carosso, Paolo A.; Jhabvala, Murzy D.
Bibcode: 1996SPIE.2831....2G
Altcode:
  The Ultraviolet Coronagraph Spectrometer is one of the instruments
  on board the Solar and Heliospheric Observatory spacecraft, which
  was launched in December, 1995. The instrument is designed to make
  ultraviolet spectrometric measurements and visible polarimetric
  measurements of the extended solar corona. Prior to launch laboratory
  measurements were carried out to determine system level values for
  many of the key performance parameters. Further measurements on
  instrument performance have been carried out since launch. Presented
  are descriptions of measurement techniques and representative results.

Title: Measurement of Hydrogen Velocity Distributions in the Extended
    Solar Corona
Authors: Kohl, J. L.; Strachan, L.; Gardner, L. D.
Bibcode: 1996ApJ...465L.141K
Altcode:
  H I Ly alpha spectral line profiles have been measured in polar
  regions of the solar corona at projected heliocentric heights of
  1.8--3.5 Rsolar. Observations were made with the Ultraviolet Coronal
  Spectrometer on the Spartan 201 satellite from 16:52 to 04:04 UT on
  1993 April 11--12 (south pole) and from 12:28 to 22:09 UT on 1993
  April 12 (north pole). In general, the coronal profiles cannot be
  accurately curve-fitted with a single-Gaussian function. The fits
  with two Gaussians yield most probable velocities of 158 and 322 km
  s-1 (south) and 98 and 266 km s-1 (north). These parameters vary by
  less than 10% (1 sigma ) over the observed heights. The observations
  are consistent with a line-of-sight model that attributes the narrow
  component to background streamers and to sites within polar coronal
  holes or a surrounding diffuse corona, and the broad component to
  the polar coronal holes and/or plumes. This interpretation suggests
  that there are regions within the observed coronal holes that have
  hydrogen and proton kinetic temperatures of (4--6) x 106 K, which is
  4--10 times higher than the expected electron temperatures at the same
  heights. However, other models with, for example, local non-Maxwellian
  velocity distributions are also consistent with the observations.

Title: Coordinated SOHO Observations of Polar Plumes
Authors: Deforest, C. E.; Scherrer, P. H.; Tarbell, T.; Harrison,
   R. A.; Fludra, A.; Delaboudiniere, J. P.; Gurman, J. B.; Wilhelm,
   K.; Lemaire, P.; Hassler, D. M.; Kohl, J. L.; Noci, G.; Fineschi,
   S.; Brueckner, G. E.; Howard, R. A.; Cyr, O. C. St.
Bibcode: 1996AAS...188.4909D
Altcode: 1996BAAS...28R.898D
  On 7 and 8 March 1996, SOHO instruments engaged in their first
  joint science operation, a 12-hr observation of polar plumes
  over the South polar coronal hole. The observing mini-campaign
  included observations from SOHO, other spacecraft, and ground-based
  observatories. Contributing SOHO instruments -- in order of altitude,
  MDI, CDS, SUMER, EIT, UVCS, and LASCO -- made overlapping, simultaneous
  observations of plume structures from the photosphere out to the
  LASCO C3 limit of 32 solar radii. MDI provided line-of-sight surface
  magnetograms with a one-min cadence and 0.6 arcsec resolution;
  CDS, SUMER, and EIT supplied temperature-sensitive images of the
  lower corona with varying cadences and resolutions; UVCS measured
  fluctuations in Ly B intensity across the coronal hole with a one-min
  cadence at 1.4 R0; and LASCO imaged the entire corona out to 30 R0 in
  various visible passbands. Plume footpoints in the lower corona are
  observed by EIT and CDS to vary by a factor of two in EUV brightness
  with a timescale of tens of minutes, while the structures above are
  (as as been previously observed) quiescent on at least a ten-hr time
  scale. We present preliminary results of cross-instrument analysis
  of the observed plumes, and suggest how this and similar future data
  sets can be used to constrain quiet-sun wind acceleration and coronal
  heating models for the coronal hole. This research is supported by
  the SOI-MDI NASA contract NAG5-3077 at Stanford University. SOHO is
  project of international cooperation between NASA and ESA.

Title: In-Flight Performance of the SOHO Ultraviolet Coronagraph
    Spectrometer
Authors: Gardner, L. D.; Kohl, J. L.; Noci, G.; Antonucci, E.;
   Tondello, G.; Huber, M. C. E.; Ciaravella, A.; Fineschi, S.; Giordano,
   S.; Moran, T.; Naletto, G.; Nicolosi, P.; Romoli, M.; Strachan,
   L.; Benna, C.; Pernechele, C.; Raymond, J. C.; Siegmund, O. H. W.;
   Spadaro, D.; Smith, P. L.
Bibcode: 1996AAS...188.3705G
Altcode: 1996BAAS...28..878G
  The in-flight performance of the SOHO Ultraviolet Coronagraph
  Spectrometer (UVCS/SOHO) is consistent with the pre-launch
  characterization and meets all planned observational
  requirements. Measurements of the key UVCS/SOHO performance
  characteristics have been performed. This paper describes the
  measurement techniques and the results. In-flight values for the
  spectral and spatial resolutions, wavelength scales, the flat
  fields, the geometric distortions, radiometric calibrations,
  and stray light levels for the two ultraviolet channels have been
  determined. Comparisons will be made to pre-flight measurements at both
  the component level and system level. This work is supported by NASA
  under contract NAS5-31250 to the Smithsonian Astrophysical Observatory,
  by the Italian Space Agency and by Switzerland.

Title: Spectroscopic Diagnostic Techniques with the SOHO Ultraviolet
    Coronagraph Spectrometer
Authors: Romoli, M.; Kohl, J. L.; Noci, G.; Antonucci, E.; Tondello,
   G.; Huber, M. C. E.; Fineschi, S.; Karovska, M.; Moran, T.; Strachan,
   L.; Ciaravella, A.; Benna, C.; Gardner, L. D.; Giordano, S.; Naletto,
   G.; Nicolosi, P.; Raymond, J. C.; Siegmund, O. H. W.; Spadaro, D.;
   Smith, P. L.
Bibcode: 1996AAS...188.3703R
Altcode: 1996BAAS...28R.877R
  The SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) uses
  spectroscopic diagnostic techniques and polarimetry to determine
  velocity distributions, temperatures, outflow velocities and densities
  of protons, electrons, and several minor ions in the extended solar
  corona. This paper describes the initial use of these techniques with
  UVCS/SOHO. Velocity distributions are derived from the observed spectral
  line profiles. In some cases, grating scans are used to improve the
  spectral resolution. The Doppler dimming method is used to determine
  radial outflow velocities and spectral line shifts are used for line of
  sight velocity measurements. The electron densities are derived from
  visible polarized radiance measurements. The status of attempts to
  derive electron temperatures from observations of electron scattered
  HI Lyman-alpha will be presented. This research is supported by NASA
  Contract NAS5-31250 to the Smithsonian Astrophysical Observatory,
  by the Italian Space Agency and by Switzerland.

Title: Ultraviolet Imaging of the Extended Solar Corona with the
    SOHO Ultraviolet Coronagraph Spectrometer
Authors: Noci, G.; Kohl, J. L.; Antonucci, E.; Tondello, G.; Huber,
   M. C. E.; Strachan, L.; Giordano, S.; Panasyuk, A.; Benna, C.;
   Ciaravella, A.; Fineschi, S.; Gardner, L. D.; Naletto, G.; Nicolosi,
   P.; Raymond, J. C.; Romoli, M.; Siegmund, O. H. W.; Spadaro, D.;
   Smith, P. L.
Bibcode: 1996AAS...188.3701N
Altcode: 1996BAAS...28..877N
  Spectroscopic observations of the extended solar corona with the SOHO
  Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) can be used to produce
  images of the extended solar corona in several ultraviolet spectral
  lines. The images are produced by scanning coronal images across the
  spectrometer entrance slits. The slits intercept a 40 arcminute slice of
  the corona parallel to the limb tangent. Telescope mirror motions can
  be used to scan from about 1.25 to 10 R_⊙. The instrument is rolled
  about its Sun-center axis to obtain images of the full corona. The
  spatial resolution depends on the selected slit width and the combined
  resolution of the spectrometer and XDL detectors. It is limited by
  diffraction for observations near the Sun where only a narrow strip of
  the telescope mirror is unvignetted by the external occulter. Images
  of equatorial streamers in HI Lyman-alpha and beta, and in O VI 103.2
  nm will be presented. Ultraviolet images of polar plumes will also be
  provided. In some cases, interpolation techniques are used to fill-in
  gaps in the raster pattern. This research is supported by NASA Contract
  NAS5-31250 to the Smithsonian Astrophysical Observatory, by the Italian
  Space Agency and by Switzerland.

Title: Coordinated SOHO Observations of Polar Plumes: Ultraviolet
    Spectroscopy with UVCS
Authors: Fineschi, S.; Kohl, J. L.; Noci, G.; Antonucci, E.;
   Tondello, G.; Huber, M. C. E.; Gardner, L. D.; Giordano, S.; Romoli,
   M.; Benna, C.; Ciaravella, A.; Naletto, G.; Nicolosi, P.; Raymond,
   J. C.; Siegmund, O. H. W.; Spadaro, D.; Smith, P. L.; Strachan, L.
Bibcode: 1996AAS...188.3704F
Altcode: 1996BAAS...28..877F
  The SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) observed polar
  plumes at the south polar coronal hole on 7 March 1996. Observations
  were made in H I Ly-alpha, Ly-beta and O VI 103.2 and 103.7
  nm. Heliocentric heights from 1.5 to 3.2 R_⊙ were observed. In
  addition, HI Ly-alpha observations with 60 sec time resolution were
  obtained at a heliocentric height of 1.6 solar radii. The polar plumes
  are clearly distinguishable in both H I Ly-alpha and O VI. These
  measurements were made in coordination with time resolved magnetograms
  by the Michelson Doppler Imager (MDI) and time resolved XUV images
  by the Extreme-Ultraviolet Imaging Telescope (EIT). This work is
  supported by NASA Contract NAS5-31250 to the Smithsonian Astrophysical
  Observatory, by the Italian Space Agency and by Switzerland.

Title: First Results from the SOHO Ultraviolet Coronagraph
    Spectrometer
Authors: Kohl, J. L.; Noci, G.; Antonucci, E.; Tondello, G.; Huber,
   M. C. E.; Benna, C.; Ciaravella, A.; Fineschi, S.; Gardner, L. D.;
   Giordano, S.; Karovska, M.; Michels, J.; Naletto, G.; Nicolosi, P.;
   Poletto, G.; Pernechele, C.; Raymond, J. C.; Romoli, M.; Siegmund,
   O. H. W.; Spadaro, D.; Smith, P. L.; Strachan, L.
Bibcode: 1996AAS...188.4906K
Altcode: 1996BAAS...28R.897K
  The SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) is being used
  to observe the extended solar corona from 1.25 to 10 R_⊙ from Sun
  center. Initial observations of polar coronal holes, polar plumes,
  equatorial streamers and the diffuse mid-latitude corona will be
  presented. The observations include measurements of spectral line
  profiles for HI Lyman alpha and beta, and O VI 103.2 and 103.7
  nm. Line intensities for Mg X 61.0 nm, Si XII 49.9 and 52.0 nm,
  S X 119.6 nm, Fe XII 124.2 nm and several other minor ions have been
  observed. Observations with moderate time resolution (about 1 minute) at
  one strip of the corona will also be presented. Preliminary results for
  derived proton and O VI velocity distributions and initial indications
  of outflow velocities for protons, and O VI will be discussed as
  well as preliminary results for other spectroscopic diagnostics
  techniques. This research is supported by NASA Contract NAS5-31250 to
  the Smithsonian Astrophysical Observatory, by the Italian Space Agency
  and by Switzerland.

Title: Coronal Emission Lines with UVCS
Authors: Raymond, J. C.; Noci, G.; Kohl, J. L.; Antonucci, E.;
   Tondello, G.; Huber, M. C. E.; Benna, C.; Ciaravella, A.; Fineschi, S.;
   Gardner, L. D.; Giordano, S.; Naletto, G.; Nicolosi, P.; Romoli, M.;
   Siegmund, O. H. W.; Spadaro, D.; Smith, P. L.; Strachan, L.; Martin, R.
Bibcode: 1996AAS...188.3702R
Altcode: 1996BAAS...28Q.877R
  The Ultraviolet Coronagraph Spectrometer aboard the SOHO satellite has
  observed the extended solar corona in H I Lyalpha and O VI lines for
  coronal diagnostics, but other, fainter, lines are also present. We
  discuss a spectral atlas obtained from emission in equatorial streamers
  and above solar active regions, pointing out lines which are especially
  useful for determining the elemental abundances, ionization state,
  and density of the emitting plasma. This work is supported by NASA
  under contract NAS5-31250 to the Smithsonian Astrophysical Observatory.

Title: Intercalibration and Co-Registration of the LASCO, UVCS and
    SUMER instruments on SOHO
Authors: Michels, J.; Kohl, J. L.; Noci, G.; Antonucci, E.; Tondello,
   G.; Huber, M. C. E.; Curdt, W.; Hollandt, J.; Lemaire, P.; Schuhle,
   U.; Wilhelm, K.; Korendyke, C.; Moran, T.; Raymond, J. C.; Romoli,
   M.; Benna, C.; Ciaravella, A.; Fineschi, S.; Gardner, L. D.; Giordano,
   S.; Naletto, G.; Nicolosi, P.; Siegmund, O. H. W.; Spadaro, D.; Smith,
   P. L.; Strachan, L.
Bibcode: 1996AAS...188.3706M
Altcode: 1996BAAS...28..878M
  Joint observations of equatorial streamers by three SOHO instruments
  have been used for radiometric intercalibration, co-registration and
  other spectroscopic comparisons. The results are used to track the
  stability of the radiometric calibrations of the Ultraviolet Coronagraph
  Spectrometer (UVCS) and the Solar Ultraviolet Measurements of Emitted
  Radiation (SUMER) experiment at overlapping wavelenghs. Observations
  of equatorial streamers at heliocentric heights from 1.25 to 1.5
  R_⊙ are used for the intercalibrations. The results are compared to
  pre-launch laboratory calibrations and to observations of stars. The
  first stellar observation was for 38 AQI. These UV observations are
  compared to coronal green line (Fe XIV) observations obtained with the
  Large Angle Spectrometric Coronagraph (LASCO) C1 coronagraph obtained
  in the same time frame. Intercomparisons of spectral line profiles
  among LASCO, SUMER, and UVCS are also planned. The LASCO research is
  supported by NASA Grant NDPR S92835D; the UVCS research is supported by
  NASA Contract NAS5-31250 to the Smithsonian Astrophysical Observatory,
  by the Italian Space Agency and by Switzerland, and SUMER is financially
  supported by BMFT/DARA, CNES, NASA and PRODEX (Swiss Contribution).

Title: New atomic data for the FeXII coronal ion
Authors: Binello, A. M.; Mason, H. E.; Storey, P. J.; Kohl, J.
Bibcode: 1996ASPC..109..251B
Altcode: 1996csss....9..251B
  No abstract at ADS

Title: Proton Temperatures, Electron Temperatures and Outflows in
    the Extended Solar Corona.
Authors: Kohl, J. L.; Gardner, L. D.; Strachan, L.; Cohen, C. M. S.;
   Galvin, A. B.; Gloeckler, G.; Guhathakurta, M.; Fisher, R. R.; Ko,
   Y. -K.; Geiss, J.; von Steiger, R.
Bibcode: 1996ASPC..109...99K
Altcode: 1996csss....9...99K
  No abstract at ADS

Title: The Ultraviolet Coronagraph Spectrometer for the Solar and
    Heliospheric Observatory
Authors: Kohl, J. L.; Esser, R.; Gardner, L. D.; Habbal, S.; Daigneau,
   P. S.; Dennis, E. F.; Nystrom, G. U.; Panasyuk, A.; Raymond, J. C.;
   Smith, P. L.; Strachan, L.; Van Ballegooijen, A. A.; Noci, G.;
   Fineschi, S.; Romoli, M.; Ciaravella, A.; Modigliani, A.; Huber,
   M. C. E.; Antonucci, E.; Benna, C.; Giordano, S.; Tondello, G.;
   Nicolosi, P.; Naletto, G.; Pernechele, C.; Spadaro, D.; Poletto, G.;
   Livi, S.; Von Der Lühe, O.; Geiss, J.; Timothy, J. G.; Gloeckler,
   G.; Allegra, A.; Basile, G.; Brusa, R.; Wood, B.; Siegmund, O. H. W.;
   Fowler, W.; Fisher, R.; Jhabvala, M.
Bibcode: 1995SoPh..162..313K
Altcode:
  The SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) is composed of
  three reflecting telescopes with external and internal occultation and
  a spectrometer assembly consisting of two toric grating spectrometers
  and a visible light polarimeter. The purpose of the UVCS instrument is
  to provide a body of data that can be used to address a broad range
  of scientific questions regarding the nature of the solar corona and
  the generation of the solar wind. The primary scientific goals are
  the following: to locate and characterize the coronal source regions
  of the solar wind, to identify and understand the dominant physical
  processes that accelerate the solar wind, to understand how the coronal
  plasma is heated in solar wind acceleration regions, and to increase the
  knowledge of coronal phenomena that control the physical properties of
  the solar wind as determined byin situ measurements. To progress toward
  these goals, the UVCS will perform ultraviolet spectroscopy and visible
  polarimetry to be combined with plasma diagnostic analysis techniques
  to provide detailed empirical descriptions of the extended solar corona
  from the coronal base to a heliocentric height of 12 solar radii.

Title: Ultraviolet Coronagraph Spectrometer for the Solar and
Heliospheric Observatory: instrument description and calibration
    overview
Authors: Kohl, J. L.; Esser, R.; Gardner, Larry D.; Habbal, S.;
   Daigneau, P. S.; Nystrom, George U.; Raymond, John C.; Strachan,
   Leonard; van Ballegooijen, A. A.; Noci, G.; Fineschi, Silvano; Romoli,
   Marco; Ciaravella, A.; Modigliani, A.; Huber, Martin C.; Antonucci, E.;
   Benna, C.; Giordano, S.; von der Luehe, Oskar; Tondello, Giuseppe;
   Nicolosi, Piergiorgio; Naletto, Giampiero; Pernechele, Claudio;
   Geiss, J.; Gloeckler, G.; Poletto, G.; Spadaro, D.; Allegra, A.;
   Basile, G.; Brusa, R.; Wood, B.; Siegmund, Oswald H.
Bibcode: 1995SPIE.2517...40K
Altcode:
  The SOHO ultraviolet coronagraph spectrometer (UVCS/SOHO) is
  composed of three reflecting telescopes with external and internal
  occultation and a spectrometer assembly consisting of two toric grating
  spectrometers and a visible light polarimeter. The UVCS will perform
  ultraviolet spectroscopy and visible polarimetry to be combined with
  plasma diagnostic analysis techniques to provide detailed empirical
  descriptions of the extended solar corona from the coronal base to a
  heliographic height of 12 R. In this paper, the salient features of
  the design of the UVCS instrument are described. An overview of the
  UVCS test and calibration activities is presented. The results from
  the calibration activity have demonstrated that the UVCS can achieve
  all its primary scientific observational goals.

Title: Determining coronal electron temperatures from observations
    with UVCS/SOHO
Authors: Fineschi, S.; Esser, R.; Habbal, S. R.; Karovska, M.; Romoli,
   M.; Strachan, L.; Kohl, J. L.; Huber, M. C. E.
Bibcode: 1995sowi.confQ..68F
Altcode:
  The electron temperature is a fundamental physical parameter of the
  coronal plasma. Currently, there are no direct measurements of this
  quantity in the extended corona. Observations with the Ultraviolet
  Coronagraph Spectrometer (UVCS) aboard the upcoming Solar and
  Heliospheric Observatory (SOHO) mission can provide the most direct
  determination of the electron kinetic temperature (or, more precisely,
  the electron velocity distribution along the line of sight). This
  measurement is based on the observation of the Thomson-scattered Lyman
  alpha (Ly-alpha) profile. This observation is made particularly
  challenging by the fact that the integrated intensity of the
  electron-scattered Ly-alpha line is about 10<SUP>3</SUP> times fainter
  than that of the resonantly-scattered Ly-alpha component. In addition,
  the former is distributed across 50 A (FWHM), unlike the latter that
  is concentrated in 1 A. These facts impose stringent requirements on
  the stray-light rejection properties of the coronagraph/spectrometer,
  and in particular on the requirements for the grating. We make use of
  laboratory measurements of the UVCS Ly-alpha grating stray-light, and of
  simulated electron-scattered Ly-alpha profiles to estimate the expected
  confidence levels of electron temperature determination. Models of
  different structures typical of the corona (e.g., streamers, coronal
  holes) are used for this parameter study.

Title: Spectroscopic diagnostics of extended corona and solar wind
    with UVCS/Spartan
Authors: Strachan, L.; Gardner, L. D.; Kohl, J. L.
Bibcode: 1995sowi.conf...29S
Altcode:
  The primary goal of the Ultraviolet Coronal Spectrometer on Spartan 201
  (UVCS/Spartan) is to make spectroscopic diagnostic measurements that can
  be used to derive plasma parameters in the extended solar corona where
  it is believed that significant heating of the corona and acceleration
  of the solar wind take place. Direct and indirect measurements of
  particle velocity distribution, thermal and non-thermal temperatures,
  and bulk outflow velocities are crucial to aid in the identification
  of physical processes that may be responsible for coronal heating
  and solar wind acceleration. UVCS/Spartan has made two flights in
  April 1993 and September 1994, the latter coinciding with the South
  Polar Passage of the Ulysses spacecraft. Observations were made of
  the large-scale structures and sub-structures of coronal holes and
  streamers at heliocentric heights between 1.5 solar radii and 3.5
  solar radii. Measurements were made of H I Lyman-alpha intensities
  and profiles, and line intensities of minor ions like O(5+) and
  Fe(11+). We will present results from the flights and discuss how
  these measurements are used to constrain values for the proton thermal
  and non-thermal kinetic temperatures, proton bulk outflow velocities,
  and minor ion temperatures and bulk outflow velocities. Plans for the
  upcoming flight in July 1995 will also be discussed.

Title: SPARTAN 201 Coronal Spectroscopy During the Polar Passes
    of ULYSSES
Authors: Kohl, J. L.; Gardner, L. D.; Strachan, L.; Fisher, R.;
   Guhathakurta, M.
Bibcode: 1995SSRv...72...29K
Altcode:
  Spartan 201 is a shuttle deployed spacecraft that is scheduled to
  perform ultraviolet spectroscopy and white light polarimetry of the
  extended solar corona during two 40 hour missions to occur in September
  1994 and August 1995. The spectroscopy is done with an ultraviolet
  coronal spectrometer which measures the intensity and spectral line
  profile of HI Lyα up to heliocentric heights of 3.5 solar radii. It
  also measures the intensities of the OVI doublet at 1032 and 1037
  Å and of Fe XII at 1242 Å. The HI Lyα line profile measurements
  are used to determine the random velocity distribution of coronal
  protons along the line-of-sight. The absolute HI Lyα intensities
  can be used together with electron densities from the white light
  coronagraph to estimate electron temperatures from hydrogen ionization
  balance calculations, and bulk outflow velocities from models of
  Doppler dimmed resonant scattering. Intensities of minor ion lines
  are used to determine coronal abundances and outflow velocities of
  O<SUP>5+</SUP>. Ultraviolet spectroscopy of extended coronal regions
  from the 11 April 1993 mission of Spartan 201 are discussed.

Title: New Results for Outflow and LOS Velocities in the Solar Wind
    Acceleration Region of the Corona
Authors: Strachan, L.; Gardner, L. D.; Kohl, J. L.; Guhathakurta,
   M.; Fisher, R. R.; Cohen, C. M. S.; Galvin, A. B.; Gloeckler, G.;
   Ko, Y. -K.; Geiss, J.; von Steiger, R.
Bibcode: 1995SPD....26..719S
Altcode: 1995BAAS...27..970S
  No abstract at ADS

Title: The Ultraviolet Coronagraph Spectrometer for the Solar and
    Hellospheric Observatory
Authors: Raymond, J. C.; Kohl, J. L.; Esser, R.; Gardner, L. D.;
   Habbal, S.; Strachan, L.; van Ballegooijen, A. A.; Noci, G.; Fineschi,
   S.; Romoli, M.; Huber, M. C. E.; Antonucci, E.; Benna, C.; von der
   Luhe, O.; Naletto, G.; Nicolosi, P.; Pernechele, C.; Tondello, G.;
   Geiss, J.; Gloeckler, G.; Spadaro, D.; Daigneau, P. S.; Nystrom,
   G. U.; Allegra, A.; Basile, G.; Brusa, R.; Wood, B.; Siegmund, O. H. W.
Bibcode: 1995SPD....26..720R
Altcode: 1995BAAS...27..970R
  No abstract at ADS

Title: Absolute-rate coefficient for C<SUP>3 + </SUP>(2s --&gt; 2p)
    electron-impact excitation
Authors: Savin, D. W.; Gardner, L. D.; Reisenfeld, D. B.; Young,
   A. R.; Kohl, J. L.
Bibcode: 1995PhRvA..51.2162S
Altcode:
  We have measured the absolute-rate coefficient for
  electron-impact excitation (EIE) of C<SUP>3+</SUP>(2s
  <SUP>2</SUP>S<SUB>1/2</SUB>--&gt;2p <SUP>2</SUP>P<SUB>1/2,3/2</SUB>)
  for energies near threshold. A delayed coincidence technique with
  inclined beams was used. Radiation from the excited ions was detected
  using an optical system that subtends slightly over π steradians. At
  an ion-rest-frame energy of 10.10 eV the measured rate coefficient
  was (7.79+/-2.10)×10<SUP>-8</SUP> cm<SUP>3</SUP> s<SUP>-1</SUP>
  and the measured cross section was (4.15+/-1.12)×10<SUP>-16</SUP>
  cm<SUP>2</SUP>. The uncertainties quoted here represent the total
  experimental uncertainty, statistical and systematic, at a confidence
  level considered to be equivalent to a statistical 90% confidence
  level. Good agreement is found with other measurements. Agreement
  is not good with Coulomb-Born with exchange and two-state
  close-coupling calculations, both of which fall outside our 90%
  confidence limits. Nine-state close-coupling calculations are in
  better agreement. However, the calculations lie at the extreme edge
  of our uncertainty limits. Taking into account previous measurements
  of EIE in C<SUP>3+</SUP> and also a measurement of EIE in Li-like
  Be<SUP>+</SUP> that falls significantly below theory at threshold, there
  is a suggestion that the C<SUP>3+</SUP>(2s--&gt;2p) EIE rate coefficient
  near threshold may fall slightly below presently accepted values.

Title: The Ultraviolet Coronagraph Spectrometer
Authors: Noci, G.; Kohl, J. L.; Huber, M. C. E.; Antonucci, E.;
   Fineschi, S.; Gardner, L. D.; Naletto, G.; Nicolosi, P.; Raymond,
   J. C.; Romoli, M.; Spadaro, D.; Strachan, L.; Tondello, G.; van
   Ballegooijen, A.
Bibcode: 1995LNP...444..261N
Altcode: 1995cmer.conf..261N
  The Ultraviolet Coronagraph Spectrometer (UVCS) is an instrument onboard
  the Solar and Heliospheric (SOHO) spacecraft, a joint ESA/NASA mission
  to be launched in 1995. The UVCS will provide ultraviolet spectroscopic
  measurements to determine the primary plasma parameters of the solar
  corona (temperatures, densities, velocities), from its base to as high
  as 10 R<SUB>⊙</SUB>. We review briefly, here, its science objectives
  and give an instrument description.

Title: SPARTAN 201 Coronal Spectroscopy During the Polar Passes
    of ULYSSES
Authors: Kohl, J. L.; Gardner, L. D.; Strachan, L.; Fisher, R.;
   Guhathakurta, M.
Bibcode: 1995hlh..conf...29K
Altcode:
  No abstract at ADS

Title: UVCS Science from SOHO
Authors: Antonucci, E.; Kohl, J. L.; Noci, G.; Huber, M. C. E.;
   Fineschi, S.; Gardner, L. D.; Naletto, G.; Nicolosi, P.; Pernechele,
   C.; Raymond, J. C.; Romoli, M.; Spadaro, Daniele; Strachan, L.;
   Tondello, G.; van Ballegooijen, A.
Bibcode: 1995jena.conf...80A
Altcode:
  The ultraviolet Coronagraph Spectrometer (UVCS), to be launched on
  board SOHO in 1995, has been designed to determine the primary plasma
  parameters in order to obtain a far more complete description of the
  coronal plasma than presently exists. This will be accomplished by
  obtaining ultraviolet spectroscopic observations in some EUV lines (HI
  Ly Alpha, O VI, Mg X, Si XII, Fe XII) and in the visible continuum,
  form the base of the solar corona to as high as 12 solar radii. The
  profiles and intensities of the measured UV lines are sensitive
  to effective temperature of protons, minor ions and electrons; ion
  densities; chemical abundances; and outflow velocities of protons and
  ions into the solar wind. The electron density is determined by means
  of white light observations. The UVCS data will be used to address a
  broad range of scientific questions concerning the nature of the solar
  corona and the generation of the solar wind. The primary scientific
  objectives are in fact those of identifying the source regions of the
  slow and fast solar wind, understanding the dominant processes that
  accelerate the solar wind, and the mechanisms for heating the coronal
  plasma in the extended corona.

Title: UVCS/SOHO capability for determining coronal conditions before,
    during and after CMEs
Authors: Strachan, L.; Raymond, J. C.; Kohl, J. L.; Noci, G.;
   Antonucci, E.; Tondello, G.; Huber, M. C. E.; Fineschi, S.; Gardner,
   L. D.; Nicolosi, P.; Romoli, M.
Bibcode: 1994ESASP.373..421S
Altcode: 1994soho....3..421S
  No abstract at ADS

Title: Ly-alpha and white light observations of a CME during the
    Spartan 201-1 mission
Authors: Hassler, D. M.; Strachan, L.; Gardner, L. D.; Kohl, J. L.;
   Guhathakurta, M.; Fisher, R. R.; Strong, K.
Bibcode: 1994ESASP.373..363H
Altcode: 1994soho....3..363H
  No abstract at ADS

Title: Polarization characterization of LY alpha holographic gratings
    with a triple-reflection polarizer
Authors: Romoli, Marco; Fineschi, Silvano; Gardner, Larry D.; Kohl,
   J. L.
Bibcode: 1994SPIE.2283..288R
Altcode:
  The diffraction efficiency of holographic gratings depends on the
  degree and orientation of the linear polarization of the incident
  light. A test has been run to measure the reflectance efficiency at Kr
  1236 angstrom of two holographic gratings in the orders +1, 0, $min1,
  as a function of the angle of the incident beam polarization plane. To
  this purpose, a triple-reflection polarizer, optimized for Ly(alpha)
  (1216 angstrom) has been fabricated and characterized. The test has
  been run to demonstrate that the coronal resonantly scattered Ly(alpha)
  can be measured using a holographic grating in the Ly(alpha) channel
  of the ultraviolet coronagraph spectrograph (UVCS) of the Solar
  and Heliospheric Observatory (SOHO) without introducing relevant
  polarization biases inside the instrument.

Title: Ultraviolet Coronagraph Spectrometer for the Solar and
Heliospheric Observatory: optical testings
Authors: Fineschi, Silvano; Romoli, Marco; Gardner, Larry D.; Kohl,
   J. L.; Noci, G.; Tondello, Giuseppe
Bibcode: 1994SPIE.2283...30F
Altcode:
  The Ultraviolet Coronagraph Spectrometer (UVCS) of the Solar and
  Heliospheric (SOHO) mission has been developed for spectroscopic
  and polarimetric determinations of temperatures, densities and flow
  velocities in the extended solar corona. The instrument consists of two
  ultraviolet (UV) spectrometers and a visible light (VL) polarimeter. The
  grating of the UV channel optimized for the HI Lyman (alpha) (Ly-(alpha)
  ) line ((lambda) 1236 angstrom) and that for the OVI doublet ((lambda)
  (lambda) 1032/1037 angstrom) have been characterized.

Title: Ultraviolet spectroscopy of the extended solar corona during
    the SPARTAN 201 mission
Authors: Kohl, J. L.; Gardner, L. D.; Strachan, L.; Hassler, D. M.
Bibcode: 1994SSRv...70..253K
Altcode:
  The instruments on the Spartan 201 spacecraft are an Ultraviolet Coronal
  Spectrometer and a White Light Coronagraph. Spartan 201 was deployed
  by the Space Shuttle on 11 April 1993 and observed the extended solar
  corona for about 40 hours. The Ultraviolet Coronal Spectrometer measured
  the intensity and spectral line profile of HI Lyα and the intensities
  of OVI 103.2 and 103.7 nm. Observations were made at heliocentric
  heights between 1.39 and 3.5 R<SUB>⊙</SUB>. Four coronal targets were
  observed, a helmet streamer at heliographic position angle 135°, the
  north and south polar coronal holes, and an active region above the west
  limb. Measurements of the HI Lyα geocorona and the solar irradiance
  were also made. The instrument performed as expected. Straylight
  suppression, spectral focus, radiometric sensitivity and background
  levels all appear to be satisfactory. The uv observations are aimed at
  determining proton temperatures and outflow velocities of hydrogen,
  protons and oxygen ions. Preliminary results from the north polar
  coronal hole observations are discussed.

Title: Preliminary results from SPARTAN 201: coronal streamer
    observations
Authors: Strachan, L.; Gardner, L. D.; Hassler, D. M.; Kohl, J. L.
Bibcode: 1994SSRv...70..263S
Altcode:
  The Ultraviolet Coronal Spectrometer on Spartan 201 obtained
  measurements of HI Ly α line profiles and O VI λ103.2/103.7 nm
  integrated intensities in a helmet streamer. Similar measurements
  were made on the solar disk to characterize the incident radiation
  which is the source for the resonantly scattered component of the
  lines. A description of the H I Ly α observations in the streamer
  will be presented. A more complete physical description of the observed
  coronal regions will become available after the analysis of additional
  data from coordinated observations made by visible coronagraphs and
  x-ray telescopes.

Title: Coronagraphic observations and analyses of the ultraviolet
    solar corona
Authors: Kohl, John L.
Bibcode: 1994sao..reptR....K
Altcode:
  This status report for the period 1 October 1992 to 30 September 1994
  covers the final preparation and first observations with the Spartan
  Ultraviolet Coronal Spectrometer on Spartan 201-1, and the preparation
  and second flight for Spartan 201-2. Both flights were fully successful
  and resulted in high quality spectroscopic observations of the extended
  solar corona out to 3.5 solar radii from Sun-center. The primary focus
  of this report is the results from Spartan 201-1. There is also a
  brief description of the evaluation of the quick look data from the
  second flight. Highlights from the first flight include a discovery
  that the proton velocity distribution in coronal holes is complex and
  consists of a central core with elevated high velocity wings compared
  to a Gaussian shape.

Title: GAUSSFIT: A Simple Way for Robust Estimate
Authors: Kohl, J. L.
Bibcode: 1994bas..conf..185K
Altcode:
  No abstract at ADS

Title: SPARTAN 201 Observations of the Ultraviolet Extended Solar
    Corona
Authors: Gardner, L. D.; Hassler, D. M.; Strachan, L.; Kohl, J. L.
Bibcode: 1994scs..conf..631G
Altcode: 1994IAUCo.144..631G
  The instruments on the Spartan 201 spacecraft are an Ultraviolet Coronal
  Spectrometer and a White Light Coronagraph. Spatan 201 observed the
  extended solar corona for about 40 hours. Four coronal targets were
  observed, a helmet streamer at heliographic position angle 135°,
  the north and south polar coronal holes, and an active region above
  the west limb. Measurements of the H I Lyα geocorona and the solar
  irradiance were also made.

Title: The SPARTAN 201 Ultraviolet Coronal Spectrometer
Authors: Gardner, L. D.; Kohl, J. L.; Strachan, L.; Hassler, D. M.
Bibcode: 1993AAS...183.0801G
Altcode: 1993BAAS...25Q1300G
  The Spartan 201 spacecraft, a free-flying autonomous satellite carried
  into orbit, released, and then recovered by the Space Shuttle, completed
  its first mission in April 1993. Spartan 201 carries two instruments:
  a UV Coronagraph (Spartan/UVCS) from the Harvard-Smithsonian Center
  for Astrophysics and a White Light Coronagraph from Goddard Space
  Flight Center and the High Altitude Observatory. The optical system
  of the Spartan/UVCS consists of an externally and internally occulted
  coronagraph with two telescope mirrors coupled to a dual spectrograph
  system, one of which makes line profile and intensity measurements
  near lambda 1216 Angstroms. The other makes intensity measurements
  of each of the OVI doublet lines at lambda lambda 1032 and 1037
  Angstroms. A summary of the observations from the first mission will be
  presented. We will also describe the Spartan/UVCS instrument and discuss
  the instrument's characterization and flight performance. Plans for the
  next mission in September 1994 will be discussed. Supported in part by
  NASA Grant no. NAG 5-613 to the Smithsonian Astrophysical Observatory.

Title: SPARTAN 201 H I Lyman-Alpha Observations of a Polar Coronal
    Region
Authors: Kohl, J. L.; Gardner, L. D.; Hassler, D. M.; Strachan, L.
Bibcode: 1993AAS...183.5906K
Altcode: 1993BAAS...25.1386K
  Measurements of H I Lyman-alpha spectral line profiles were made during
  the Spartan 201-1 Mission on 11 April 1993. The spectral resolution
  elements were 0.025 nm and the spatial elements were 0.5 arc min. by
  2.5 arc min. Observations were made between 1.35 and 3.5 solar radii
  from sun-center. The line shapes are found to be complex. Velocity
  distributions derived from the line profiles will be presented. Broad
  wings on the profiles indicate proton velocity distributions that
  deviate significantly from that expected in a purely Maxwellian thermal
  distribution. Possible explanations for the observed high velocities
  will be discussed. Supported in part by NASA Grant no. NAG 5-613 to
  the Smithsonian Astrophysical Observatory.

Title: A Doppler Dimming Determination of Coronal Outflow Velocity
Authors: Strachan, Leonard; Kohl, John L.; Weiser, Heinz; Withbroe,
   George L.; Munro, Richard H.
Bibcode: 1993ApJ...412..410S
Altcode:
  Outflow velocities in a polar coronal hole are derived from observations
  made during a 1982 sounding rocket flight. The velocity results are
  derived from a Doppler dimming analysis of resonantly scattered H I
  Ly-alpha. This analysis indicates radial outflow velocities of 217
  km/s at 2 solar radii from sun-center with an uncertainty range of
  153 to 251 km/s at a confidence level of 67 percent. These results are
  best characterized as strong evidence for supersonic outflow within 2
  solar radii of sun-center in a polar coronal hole. Several means for
  obtaining improved accuracy in future observations are discussed.

Title: Stray-light suppression in a reflecting white-light coronagraph
Authors: Romoli, Marco; Weiser, Heinz; Gardner, Larry D.; Kohl, John L.
Bibcode: 1993ApOpt..32.3559R
Altcode: 1993ApOpt..32.3559W
  An analysis of stray-light suppression in the white-light channel
  of the Ultraviolet Coronagraph Spectrometer experiment for the
  Solar and Heliospheric Observatory is reported. The white-light
  channel consists of a reflecting telescope with external and internal
  occultation and a polarimeter section. Laboratory tests and analytical
  methods are used to perform the analysis. The various stray-light
  contributions are classified in two main categories: the contribution
  from sunlight that passes directly through the entrance aperture
  and the contribution of sunlight that is diffracted by the edges of
  the entrance aperture. Values of the stray-light contributions from
  various sources and the total stray-light level for observations at
  heliocentric heights from 1.4 to 5 solar radii are derived. Anticipated
  signal-to-stray-light ratios are presented together with the effective
  stray-light rejection by the polarimeter, demonstrating the efficacy
  of the stray-light suppression design.

Title: Ultraviolet Coronal Spectrometer Observations During Spartan
    Mission 201-1
Authors: Gardner, L. D.; Fineschi, S.; Hassler, D.; Romoli, M.;
   Strachan, L.; Kohl, J. L.
Bibcode: 1993BAAS...25.1200G
Altcode:
  No abstract at ADS

Title: Ultraviolet Spectroscopic Observations of Polar Coronal Holes
    During Spartan Mission 201-1
Authors: Kohl, J. L.; Gardner, L. D.; Hassler, D.; Strachan, L.
Bibcode: 1993BAAS...25.1209K
Altcode:
  No abstract at ADS

Title: Ultraviolet Spectroscopic Observations of a Helmet Streamer
    During Spartan Mission 201-1
Authors: Strachan, L.; Gardner, L. D.; Hassler, D.; Kohl, J. L.
Bibcode: 1993BAAS...25.1209S
Altcode:
  No abstract at ADS

Title: Measuring electron temperature in the extended corona.
Authors: Hassler, Donald M.; Gardner, L. D.; Kohl, John L.
Bibcode: 1992ESASP.348..375H
Altcode: 1992cscl.work..375H
  The authors discuss a technique for measuring electron temperature in
  the extended corona from the line profile of the electron scattered
  component of coronal H I Ly-α produced by Thomson scattering of
  chromospheric Ly-α emission. They present an evaluation of this
  technique based on simulated measurements and discuss the subsequent
  instrumental requirements necessary to make a meaningful determination
  of the electron temperature. Estimates of uncertainties in the measured
  electron temperature are related to critical instrument parameters
  such as grating stray light suppression.

Title: "UVCS" - the Ultraviolet Coronagraph Spectrometer for SOHO.
Authors: Kohl, John L.; Noci, Giancarlo
Bibcode: 1992ESASP.348...23K
Altcode: 1992cscl.work...23K
  The Ultraviolet Coronagraph Spectrometer (UVCS) will provide
  spectroscopic observations of the solar corona out to 10 solar radii
  from Sun-center. This capability is expected to expand greatly the
  number of plasma parameters that can be specified by remote sensing
  techniques. UVCS plasma diagnostic techniques are expected to provide
  a sufficient number of empirically derived parameters to constrain
  significantly theories of solar wind acceleration, coronal heating,
  and solar wind composition. The measured line profiles and intensities
  are sensitive to random velocity distributions, densities, and outflow
  velocities of coronal protons, electrons, and ions.

Title: Simulated O VI Doppler dimming measurements of coronal
    outflow velocities.
Authors: Strachan, Leonard; Gardner, L. D.; Kohl, John L.
Bibcode: 1992ESASP.348..121S
Altcode: 1992cscl.work..121S
  The authors investigate the possibility of determining O<SUP>5+</SUP>
  outflow velocities by using a Doppler dimming analysis of the
  resonantly scattered intensities of O VI λ1031.9 and λ1037.6. The
  technique is sensitive to outflow velocities, W, in the range 30 &lt;
  W &lt; 250 km s<SUP>-1</SUP> and can be used for probing regions of
  the inner solar corona, where significant coronal heating and solar
  wind acceleration may be occurring. These velocity measurements,
  when combined with measurements of other plasma parameters (i.e.,
  temperatures and densities of ions and electrons), can be used to
  estimate the energy and mass flux of O<SUP>5+</SUP>. In particular,
  it may be possible to locate where the flow changes from subsonic
  to supersonic and to identify source regions for the high- and
  low-speed solar wind. The velocity diagnostic technique is discussed
  with emphasis placed on the requirements needed for accurate outflow
  velocity determinations. Model determinations of outflow velocities
  based on simulated Doppler dimming observations are presented.

Title: Measuring the Electron Scattered Component of H I Ly-α to
    Determine Te
Authors: Hassler, D. M.; Gardner, L. D.; Kohl, J. L.
Bibcode: 1992AAS...180.5205H
Altcode: 1992BAAS...24R.816H
  No abstract at ADS

Title: The SPARTAN Ultraviolet Coronagraph
Authors: Gardner, L. D.; Esser, R.; Habbal, S. R.; Hassler, D. M.;
   Raymond, J. C.; Strachan, L.; van Ballegooijen, A. A.; Kohl, J. L.;
   Fineschi, S.
Bibcode: 1992AAS...180.5202G
Altcode: 1992BAAS...24..815G
  An ultraviolet coronagraph (UVC) is being prepared for a series of
  orbital flights on NASA's Spartan 201 which is deployed and retrieved
  by Shuttle. The Spartan 201 payload consists of the UVC and a white
  light coronagraph developed by the High Altitude Observatory. Spartan
  is expected to provide 26 orbits of solar observations per flight. The
  first flight is scheduled for May 1993 and subsequent flights
  are planned to occur at each polar passage of Ulysses (1994 and
  1995). The UVC measures the intensity and spectral line profile of
  resonantly scattered H I Ly-alpha and the intensities of O VI lambda
  1032 and lambda 1037 at heliocentric heights between 1.3 and 3.5 solar
  radii. A description of the UVC instrument, its characteristics, and the
  observing program for the first flight will be presented. The initial
  scientific objective is to determine the random velocity distribution
  and bulk outflow velocity of coronal protons and the density and outflow
  velocity of O(5+) in polar coronal holes and adjoining high latitude
  streamers. This work is supported by NASA under Grant No. NAG5-613 to
  the Smithsonian Astrophysical Observatory.

Title: Experimental Dielectronic Recombination Results and their
    Implications for the Solar Transition Region
Authors: Savin, D. W.; Reisenfeld, D. B.; Gardner, L. D.; Young,
   A. R.; Raymond, J. C.; Kohl, J. L.
Bibcode: 1992AAS...180.0516S
Altcode: 1992BAAS...24..736S
  Electric and magnetic fields of the magnitudes found in the solar
  atmosphere can significantly enhance dielectronic recombination (DR)
  rate coefficients. An experiment to measure DR rates as a function of
  the external electric field strength will be described. An initial
  result for the C(3+) DR rate coefficient through the 2s-2p core
  transition indicates that the DR rate for a 12 V/cm field is a factor
  of 7.2+/-1.8 (1sigma ) larger than calculated zero field values. This
  is a field strength comparable to the plasma microfield strength
  found in the upper transition region where C(3+) is abundant. We will
  present calculations showing the implications of field enhanced DR
  rates on the carbon ionization balance and on observations of solar UV
  emission lines. In particular, we show that the field enhanced C(3+)
  DR rate could lead to as much as a factor of 4 reduction in previously
  reported C(3+) fractional abundances. This requires a corresponding
  increase in emission measures to match the C IV lambda 1550 Angstroms
  emission line intensities observed in the Sun and late-type stars. This
  work is supported by NASA under Grant NAGW-1687 to the Harvard College
  Observatory.

Title: Plans for Measuring Coronal O(5+) Outflow Velocities with
    SPARTAN 201
Authors: Strachan, L.; Gardner, L. D.; Kohl, J. L.
Bibcode: 1992AAS...180.5203S
Altcode: 1992BAAS...24..815S
  A goal of the Spartan 201 mission is to derive outflow velocities, W,
  of coronal O(5+) by using a Doppler dimming analysis of the expected
  resonantly scattered intensities of OVI lambda 1031.9 and lambda
  1037.6. The technique is sensitive to velocities in the range 30 &lt;
  W &lt; 250 km s(-1) and will be used for probing regions of the inner
  solar corona, between 1.3 and 3.5 R<SUB>sun</SUB>, where significant
  coronal heating and solar wind acceleration may be occurring. These
  velocity measurements, when combined with measurements of other plasma
  parameters (i.e., temperatures and densities of ions and electrons),
  can be used to estimate the energy and mass fluxes of coronal ions. In
  particular, it may be possible to locate where the flow changes from
  subsonic to supersonic and to identify source regions for the high- and
  low-speed solar wind. The velocity diagnostic technique is discussed
  with emphasis placed on the requirements needed for accurate outflow
  velocity determinations. Model calculations of outflow velocities
  based on expected detector count rates are also presented. This work
  is supported by NASA under Grant No. NAG5-613 to the Smithsonian
  Astrophysical Observatory.

Title: The Ultraviolet Coronagraph Spectrometer for SOHO (UVCS)
Authors: Kohl, J. L.; Noci, G.
Bibcode: 1992AAS...180.3308K
Altcode: 1992BAAS...24..781K
  The purpose of the Ultraviolet Coronagraph Spectrometer (UVCS) is to
  provide information about the behavior, in the extended corona, of
  the primary particles (protons and electrons) and several minor ions
  (O(5+) , Mg(9+) , Si(11+) , and Fe(11+) ). Spectroscopic diagnostic
  techniques will be used to determine random velocity distributions,
  densities, and bulk outflow velocities for these particles. The
  resulting empirical description of the extended corona can be used to
  address a broad range of scientific questions regarding the nature of
  the solar corona and the generation of the solar wind. The instrument
  consists of an externally and internally occulted telescope assembly
  and a spectrometer assembly. It has three channels whose purposes are
  the following: 1) VUV spectroscopy and absolute radiometry in the 1130
  to 1361 Angstroms wavelength range with spectral resolution up to 9800
  and spatial resolution elements of 7" or larger, 2) EUV spectroscopy
  and absolute radiometry in the 937 to 1127 Angstroms (first order) and
  469 to 655 Angstroms (second order) wavelength ranges with spectral
  resolution up to 12000 and the same spatial resolution as the VUV
  channel, and 3) White light polarimetry with a wavelength band pass
  of 4500 -- 6000 Angstroms and a single 14" by 14" spatial resolution
  element. MAMA detectors provide simultaneous ultraviolet observations
  of a 40' long strip (parallel to a limb tangent) of the corona. Mirror
  and instrument motions allow this instantaneous field-of-view to scan
  out to heliocentric heights of 10 R<SUB>sun</SUB> and onto the solar
  disk. This work is supported by NASA under contract NAS5-31250 to the
  Smithsonian Astrophysical Observatory.

Title: On the Density and Field Sensitivities of Dielectronic
    Recombination
Authors: Reisenfeld, Daniel B.; Raymond, John C.; Young, Albert R.;
   Kohl, John L.
Bibcode: 1992ApJ...389L..37R
Altcode:
  Dielectronic recombination dominates the recombination rates
  of most ions in coronal plasmas at their temperatures of peak
  concentration. Because dielectronic recombination goes by way of high nl
  doubly excited levels, it is susceptible to collisional excitation and
  ionization, leading to a decreased rate. On the other hand, theoretical
  studies show that Stark mixing of the nl levels by a modest electric
  field enhances the dielectronic recombination rate severalfold. The
  ionization balance is computed here as as function of density, and it
  is found that the new results require increased emission measures to
  match the C IV emission line intensities observed in the sun and in
  late-type stars. They also make it more difficult to interpret the
  overall EUV emission line spectrum of the sun.

Title: Laboratory studies in ultraviolet solar physics
Authors: Parkinson, W. H.; Kohl, J. L.; Gardner, L. D.; Raymond,
   J. C.; Smith, P. L.
Bibcode: 1991STIN...9226029P
Altcode:
  The research activity comprised the measurement of basic atomic
  processes and parameters which relate directly to the interpretation of
  solar ultraviolet observations and to the development of comprehensive
  models of the component structures of the solar atmosphere. The research
  was specifically directed towards providing the relevant atomic
  data needed to perform and to improve solar diagnostic techniques
  which probe active and quiet portions of the solar chromosphere, the
  transition zone, the inner corona, and the solar wind acceleration
  regions of the extended corona. The accuracy with which the physical
  conditions in these structures can be determined depends directly on
  the accuracy and completeness of the atomic and molecular data. These
  laboratory data are used to support the analysis programs of past and
  current solar observations (e.g., the Orbiting solar Observatories,
  the Solar Maximum Mission, the Skylab Apollo Telescope Mount, and the
  Naval Research Laboratory's rocket-borne High Resolution Telescope
  and Spectrograph). In addition, we attempted to anticipate the needs
  of future space-borne solar studies such as from the joint ESA/NASA
  Solar and Heliospheric Observatory (SOHO) spacecraft. Our laboratory
  activities stressed two categories of study: (1) the measurement of
  absolute rate coefficients for dielectronic recombination and electron
  impact excitation; and (2) the measurement of atomic transition
  probabilities for solar density diagnostics. A brief summary of the
  research activity is provided.

Title: UV observational techniques for the extended solar corona
Authors: Kohl, J. L.; Gardner, L. D.; Huber, M. C. E.; Nicolosi,
   P.; Noci, G.; Naletto, G.; Romoli, M.; Spadaro, D.; Tondello, G.;
   Weiser, H.
Bibcode: 1991AdSpR..11a.359K
Altcode: 1991AdSpR..11..359K
  The SOHO Ultraviolet Coronagraph Spectrometer is being developed for
  spectroscopic determinations of temperatures, densities and flow
  velocities in the extended solar corona. Determinations of plasma
  parameters for the primary particles (electrons and protons) and for
  several minor ions are planned. The techniques and instrumentation
  to be used must overcome the relatively low intensity levels and
  potentially high stray light levels intrinsic to observations of the
  extended corona while also providing high radiometric and spectrometric
  accuracy and relatively high spectral and spatial resolution. This
  paper concentrates on the instrument characteristics that are required
  to observe the resonantly scatter HI Lyman-alpha line at heliocentric
  heights from 1 to 10 solar radii.

Title: The Spartan 201 Mission Observations of the Extended Solar
    Corona
Authors: Gardner, L. D.; Kohl, J. L.; Strachan, L.; Weiser, H.;
   Fisher, R.; Sime, D.
Bibcode: 1990BAAS...22..852G
Altcode:
  No abstract at ADS

Title: Measurement of Dielectronic Recombination in CIV in an External
    Electric Field
Authors: Young, A. R.; Gardner, L. D.; Kohl, J. L.; Raymond, J. C.;
   Savin, D. W.; Reisenfeld, D. B.
Bibcode: 1990BAAS...22..799Y
Altcode:
  No abstract at ADS

Title: The Ultraviolet Coronagraph Spectrometer for SOHO
Authors: Kohl, J. L.; Noci, G.
Bibcode: 1989BAAS...21..831K
Altcode:
  No abstract at ADS

Title: Doppler Dimming Measurement of Solar Wind Outflow
Authors: Strachan, L.; Kohl, J. L.; Munro, R. H.; Withbroe, G. L.
Bibcode: 1989BAAS...21..840S
Altcode:
  No abstract at ADS

Title: Observations of the Extended Solar Corona from a Spartan
    Carrier
Authors: Gardner, L. D.; Kohl, J. L.; Weiser, H.; Fisher, R.; Sime, D.
Bibcode: 1989BAAS...21..840G
Altcode:
  No abstract at ADS

Title: Coronagraph observations and analyses of the ultraviolet
    solar corona
Authors: Kohl, John L.
Bibcode: 1989sao..rept.....K
Altcode:
  The major activities on the Spartan Ultraviolet Coronal Spectrometer
  project include both scientific and experimental/technical efforts. In
  the scientific area, a detailed analysis of the previously reported
  Doppler dimming of HI Ly-alpha from the July 1982 rocket flight has
  determined an outflow velocity at 2 solar radii from sun center to
  be between 153 and 251 km/s at 67 percent confidence. The technical
  activities include, several improvements made to the instrument that
  will result in enhanced scientific performance or in regaining a
  capability that had deteriorated during the delay time in the launch
  date. These include testing and characterizing the detector for
  OVI radiation, characterizing a serrated occulter at UV and visible
  wavelengths, fabricating and testing telescope mirrors with improved
  edges, testing and evaluating a new array detector system, modifying the
  slit mask mechanism and installing a mask in the instrument to block
  the Ly-alpha resonance line when the electron scattered component is
  being observed.

Title: Spectroscopic measurements of solar wind parameters near
    the sun.
Authors: Kohl, J. L.; Weizer, H.; Livi, S.
Bibcode: 1989GMS....54...81K
Altcode: 1989sspp.conf...81K
  Instrumentation and plasma diagnostic techniques are being developed
  to obtain a detailed empirical description of solar wind acceleration
  regions at heights between the coronal base and about 10 solar radii
  from sun center. The instruments which are being developed for remote
  sensing of the extended corona consist of an occulted telescope system
  and a high resolution spectrometer. The basic design was proven on
  three sounding rocket flights. Initial data on proton temperatures
  and solar wind outflow velocities for heliospheric heights between
  1.5 and 3.5 solar radii from sun center have been obtained.

Title: UVCS: An Ultraviolet Coronagraph Spectrometer for SOHO
Authors: Kohl, J. L.; Hartmann, L. W.; van Ballegooijen, A. A.;
   Withbroe, G. L.; Rayomnd, J. C.; Weiser, H.; Noci, G.; Antonucci,
   E.; Geiss, J.; Gloeckler, G.
Bibcode: 1989ESASP1104...49K
Altcode:
  The UltraViolet Coronagraph Spectrometer (UVCS) of SOHO (solar
  and heliospheric observatory) provides ultraviolet spectroscopic
  observations of the solar corona out to ten solar radii from
  suncenter. This capability is expected to greatly expand the
  number of plasma parameters that can be specified by remote sensing
  techniques. Plasma diagnostic techniques are expected to provide a
  sufficient number of empirically derived parameters to significantly
  constrain theories of solar wind acceleration, coronal heating, and
  solar wind composition. The spectral line profiles and intensities
  are sensitive to random velocity distributions and to the effective
  temperatures of protons, minor ions, and electrons. Ion densities,
  chemical abundances, and outflow velocities of coronal protons and
  ions into the solar wind are also taken into consideration.

Title: UVCS: an Ultraviolet Coronagraph Spectrometer for SOHO
Authors: Kohl, J. L.; Hartmann, L. W.; van Ballegooijen, A. A.;
   Withbroe, G. L.; Raymond, J. C.; Weiser, H.; Noci, G.; Antonucci,
   E.; Geiss, J.; Gloeckler, G.
Bibcode: 1988sohi.rept...49K
Altcode:
  The UltraViolet Coronagraph Spectrometer (UVCS) of SOHO (solar
  and heliospheric observatory) provides ultraviolet spectroscopic
  observations of the solar corona out to ten solar radii from
  sun-center. This capability is expected to greatly expand the
  number of plasma parameters that can be specified by remote sensing
  techniques. Plasma diagnostic techniques are expected to provide a
  sufficient number of empirically derived parameters to significantly
  constrain theories of solar wind acceleration, coronal heating, and
  solar wind composition. The spectral line profiles and intensities
  are sensitive to random velocity distributions and to the effective
  temperatures of protons, minor ions, and electrons. Ion densities,
  chemical abundances, and outflow velocities of coronal protons and
  ions into the solar wind are also taken into consideration.

Title: Instrument for Ultraviolet Spectroscopy of the Extended
    Solar Corona
Authors: Kohl, John L.
Bibcode: 1988soae.conf...30K
Altcode:
  No abstract at ADS

Title: Measurement of electron-impact excitation in boronlike carbon
Authors: Lafyatis, G. P.; Kohl, J. L.
Bibcode: 1987PhRvA..36...59L
Altcode:
  The cross section for the electron-impact excitation of C(+) (2s2
  2p 2P0)-(2s2p2 2D) is measured in a colliding-beams apparatus for
  several collision energies near the threshold for the process. A cross
  section of (1.1 + or - 0.3) x 10 to the -16th sq cm at threshold is
  found. Reasonable agreement is found with close-coupling calculations.

Title: Solar Wind Diagnostics from Doppler-enhanced Scattering
Authors: Noci, Giancarlo; Kohl, John L.; Withbroe, George L.
Bibcode: 1987ApJ...315..706N
Altcode:
  Solar wind ions can attain sufficient outflow speed, w, to cause line
  excitation by chromospheric or transition region radiation in a nearby
  line. It is shown that this extends the diagnostic possibilities of a
  coronal EUV line to much larger values of w than would be possible if
  pumping were limited to radiation from the same spectral line. For the
  1037.6 A coronal line of O VI, the pumping effect of the chromospheric
  C II 1037.0 A line is efficient for w between 100 and 250 km/s. An
  approximate expression for the line ratio for a doublet of the Li or
  Na isoelectronic sequences is derived, and the diagnostic capabilities
  of doublet line ratios, either by themselves or combined with the
  observation of other quantities, are discussed. In particular, that
  the determination of doublet line ratios at several heights can be
  sufficient to yield the solar wind velocity at those heights together
  with a constraint on other coronal parameters.

Title: Photometry and activity of the nucleus of P/Halley at
    heliocentric distances larger than 4.6 AU, pre-perihelion
Authors: Festou, M. C.; Lecacheux, J.; Kohl, J. L.; Encrenaz, T.;
   Baudrand, J.
Bibcode: 1986A&A...169..336F
Altcode:
  Photometric data collected during the preperihelion phase of the passage
  of Comet Halley are discussed in terms of the observed brightness
  variations and the rotation period of the comet. The primary data were
  collected at four different terrestrial observatories. Reflected light
  from the nucleus within 8 AU distance is determined to be only partially
  responsible for the photometric variations, leading to the conclusion
  that it is at the present time not possible to quantify the rotational
  period of a comet by its photometric variations. The behavior of the
  brightness variations at various distances from the sun indicated that
  outbursts are not temperature dependent and that the energy released
  is proportional to the energy stored at a given distance from the sun.

Title: Analysis of Coronal H i Lyman-Alpha Measurements in a Polar
    Region of the Sun Observed in 1979
Authors: Withbroe, G. L.; Kohl, J. L.; Weiser, H.
Bibcode: 1986ApJ...307..381W
Altcode:
  Measurements of the intensities and spectral line profiles of resonantly
  scattered hydrogen Ly-alpha radiation have been used to determine
  hydrogen kinetic temperatures and electron densities between r = 1.5
  and 2.2 solar radii in a polar region of the corona observed in 1979
  near solar maximum. The mean temperature, 1.8 x 10 to the 6th K, in
  this region is significantly higher, by about 60 percent, than that
  obtained in a similar region observed in a 1980 rocket flight. The
  densities in these two polar regions are similar and are a factor
  of about 4 larger than in polar coronal holes observed at solar
  minimum. The flow velocities in both regions are most likely subsonic
  for r less than about 4 solar radii. The results reported here support
  the hypothesis that polar coronal holes observed at different times
  during the solar cycle can have different temperatures, densities,
  and possibly flow velocities.

Title: Concept study of a UV coronagraph spectrometer for the
    pinhole-occulter facility
Authors: Kohl, J. L.
Bibcode: 1986sao..reptQ....K
Altcode:
  The results of a very short study to define an Ultraviolet
  Coronagraph-Spectrometer (UVCS) for the Pinhole/Occulter Facility (P/OF)
  are summarized. The P/OF instrument was based on docummentation from
  the Definition Phase of the Spacelab Coronographs Program which was
  effectively completed in August 1980. The primary differences between
  the P/OF instrument and the Spacelab experiment are the remote occulter
  mask, the telescope size , and the deployable structure to accommodate
  P/OF's length restrictions. Requirement for P/OF that are associated
  with these features are briefly considered, but further study is need
  to more fully consider the unusual implications, particularly in the
  interplay between the instrument pointing and the P/OF boom control.

Title: Spacelab Lyman Alpha-White Light Coronagraph Program
Authors: Kohl, J. L.
Bibcode: 1986sao..reptR....K
Altcode:
  The Spacelab Lyman Alpha Coronagraph (SLAC) of the Smithsonian
  Astrophysical Observatory (SAO) and the White Light Coronagraph (WLC)
  to be provided by the High Altitude Observatory (HAO) are two separate
  coronagraphs which would be operated in a joint fashion during Spacelab
  missions to be flown by the Space Shuttle. The two instruments would be
  used to perform joint observations of solar coronal structures from 1.2
  to 8.0 solar radii from sun-center in vacuum ultraviolet and visible
  radiations. Temperatures, densities, and flow velocities throughout
  the solar wing acceleration region of the inner solar corona were
  measured. The Phase I Definition activity resulted in the successful
  definition and preliminary design of the experiment/instrumentation
  subsystem and associated software, ground support equipment and
  interfaces to the extended required to accurately estimate the scope
  of the investigation and prepare an Investigational Development Plan;
  the performance of the necessary functional, operations, and safety
  analyses necessary to complete the Experiment Requirements document.

Title: Bi-dimensional Observations of Several Molecules in Comet
    Halley's Coma
Authors: Kohl, J. L.; Lecacheux, J.; Festou, M. C.; Picat, J. P.;
   Vapillon, L.
Bibcode: 1986BAAS...18..826K
Altcode:
  No abstract at ADS

Title: The Spectrophotometer of the National Observatory
Authors: Codina Landaberry, S. J.; Freitas Pacheco, J. A.; Kohl,
   J. L.; Bazzanella, B.; Ribeiro, R. T.
Bibcode: 1986RMxAA..12..405C
Altcode:
  No abstract at ADS

Title: The spectrophotometer of the National Observatory.
Authors: Landaberry, S. J. C.; de Freitas Pacheco, J. A.; Kohl, J. L.;
   Bazzanella, B.; Ribeiro, R. T.
Bibcode: 1986RMxAA..12..405L
Altcode:
  No abstract at ADS

Title: OVI Diagnostics of Solar Wind Generation
Authors: Noci, G.; Kohl, J. L.; Withbroe, G. L.
Bibcode: 1986ASSL..123...53N
Altcode: 1986shtd.symp...53N
  The O VI resonance doublet is partly collisionally and partly
  radiatively excited in the solar corona. In the solar wind the O VI
  ions can attain sufficient outflow speed to cause excitation of the
  2P<SUB>1/2</SUB> level by the chromospheric C II λ1037.0 line. The
  authors show that this extends the diagnostic possibilities of the O VI
  resonance doublet. In particular, the determination of the intensity
  ratio of the doublet lines at several heights can be sufficient to
  yield the solar wind velocity at those heights and hence information
  on the mechanisms of solar wind acceleration.

Title: Coronal Spectroscopy and Imaging from Spartan during the
    Polar Passage of Ulysses
Authors: Kohl, J. L.; Weiser, H.; Withbroe, G. L.; Noci, G.; Munro,
   R. H.
Bibcode: 1986ASSL..123...39K
Altcode: 1986shtd.symp...39K
  A joint payload consisting of a UV Coronal Spectrometer and a White
  Light Coronagraph is being developed for a series of flights on NASA's
  Spartan carrier. Spartan, which is deployed and retrieved by Shuttle,
  is intended to provide at least 27 orbits of solar observations per
  mission. The first flight of this payload is planned for October 1986,
  and it is anticipated that a subsequent flight will occur at each polar
  passage of Ulysses. Coordinated measurements of solar wind acceleration
  parameters in polar regions of the solar corona with Spartan and
  'in situ' measurements of the polar wind from Ulysses will provide a
  unique opportunity to establish empirical constraints on polar wind
  models. Spectroscopic diagnostics to be provided by Spartan include
  determinations of the electron and neutral hydrogen random velocities,
  outflow velocities in the 30 to 300 km/s range and electron densities.

Title: Coronal temperatures, heating, and energy flow in a polar
    region of the sun at solar maximum
Authors: Withbroe, G. L.; Kohl, J. L.; Weiser, H.; Munro, R. H.
Bibcode: 1985ApJ...297..324W
Altcode:
  The profiles of resonantly scattered Lyman-alpha coronal radiation have
  been used to determine the hydrogen kinetic temperature from 1.5 to 4
  solar radius from the center of the polar region of the corona observed
  in 1980 at solar maximum. Hydrogen temperatures derived from the line
  profiles were found to decrease with height from 1.2 million K at r =
  1.5 solar radii to 600,000 K at r = 4 solar radius. Comparison of the
  measured kinetic temperatures with predictions from a semiempirical
  two-fluid model showed evidence of a small amount of heating or a
  nonthermal contribution to the motions of coronal protons between
  1.5 and 4 solar radius. The widths of the profiles confirmed an upper
  limit of 110 + or - 15 km/s on the rms magnitude of the line-of-sight
  component of velocities between 1.5 and 4 solar radius. Density
  measurements obtained in situ in the solar wind in the ecliptic were
  used to locate the sources of low speed and high-speed winds in the
  polar region. An eclipse photograph of the corona at solar maximum
  is provided.

Title: Evidence for Supersonic Solar Wind Velocities at 2.1
    R<SUB>⊙</SUB>
Authors: Kohl, J. L.; Weiser, H.; Withbroe, G. L.; Zapata, C. A.;
   Munro, R. H.
Bibcode: 1984BAAS...16..531K
Altcode:
  No abstract at ADS

Title: Cross Section Measurement for Electron Impact Excitation of
    C II
Authors: Lafyatis, G. P.; Deutsch, L. K.; Kohl, J. L.
Bibcode: 1984BAAS...16..529L
Altcode:
  No abstract at ADS

Title: Measurements of Absolute Collisional Cross Sections at
    Harvard-Smithsonian CFA
Authors: Kohl, J. L.; Deutsch, L. K.; Gardner, L. D.; Lafyatis, G. P.;
   Young, A. R.
Bibcode: 1984uxsa.coll..179K
Altcode: 1984uxsa.conf..179K; 1984IAUCo..86..179K
  No abstract at ADS

Title: Photodissociation of Neutral Free Radicals of Astrophysical
    Interest
Authors: Gardner, L. D.; Graff, M. M.; Kohl, J. L.
Bibcode: 1984uxsa.coll..167G
Altcode: 1984IAUCo..86..167G; 1984uxsa.conf..167G
  No abstract at ADS

Title: The Solar Wind Generation Experiment for SPARTAN Mission 201
Authors: Kohl, J. L.; Weiser, H.; Withbroe, G. L.; Munro, R. H.
Bibcode: 1984uxsa.coll...29K
Altcode: 1984uxsa.conf...29K; 1984IAUCo..86...29K
  No abstract at ADS

Title: Spectroscopic measurements of solar wind generation.
Authors: Kohl, J. L.; Withbroe, G. L.; Zapata, C. A.; Noci, G.
Bibcode: 1983NASCP.2280..47K
Altcode: 1983sowi.conf...47K
  Spectroscopically observable quantities are described which are
  sensitive to the primary plasma parameters of the solar wind's source
  region. The method is discussed in which those observable quantities are
  used as constraints in the construction of empirical models of various
  coronal structures. Simulated observations are used to examine the
  fractional contributions to observed spectral intensities from coronal
  structures of interest which co-exist with other coronal structures
  along simulated lines-of-sight. The sensitivity of spectroscopic
  observables to the physical parameters within each of those structures
  is discussed.

Title: New Observations of the Extended Ultraviolet Corona
Authors: Kohl, J. L.; Weiser, H.; Withbroe, G. L.; Munro, R. H.;
   Noci, G.
Bibcode: 1982BAAS...14..976K
Altcode:
  No abstract at ADS

Title: Measurements of Electron Impact Excitation of C II and Si IV
Authors: Lafyatis, G. P.; Kohl, J. L.
Bibcode: 1982BAAS...14..923L
Altcode:
  No abstract at ADS

Title: EUV spectroscopic plasma diagnostics for the solar wind
    acceleration region
Authors: Kohl, J. L.; Withbroe, G. L.
Bibcode: 1982ApJ...256..263K
Altcode:
  Possibilities are considered for probing physical conditions in the
  solar corona with strong EUV resonance lines from ions such as N V, O
  VI, Ne VIII, Mg X, and Si XII. Through measurements of the intensities
  and profiles of EUV spectral lines with coronagraphic instrumentation
  employing normal incidence reflecting optics, it is possible to
  acquire information on electron, proton, and ion temperatures and
  velocity distributions; electron, H I, and ion densities; mass flow
  and nonthermal velocities; and chemical abundances. This information
  will provide critical empirical constraints on physical processes
  responsible for plasma heating, solar wind acceleration, and transport
  of mass, momentum, and energy in the solar corona, as well as providing
  constraints on theoretical models for solar and stellar coronae and
  mass loss.

Title: Analysis of coronal H I Lyman alpha measurements from a rocket
    flight on 1979 April 13
Authors: Withbroe, G. L.; Kohl, J. L.; Weiser, H.; Noci, G.; Munro,
   R. H.
Bibcode: 1982ApJ...254..361W
Altcode:
  It is noted that measurements of the profiles of resonantly scattered
  hydrogen Lyman-alpha coronal radiation have been used in determining
  hydrogen kinetic temperatures from 1.5 to 4 solar radii from sun
  center in a quiet region of the corona. Proton temperatures derived
  using the line widths decrease with height from 2.6 x 10 to the 6th
  K at 1.5 solar radii to 1.2 x 10 to the 6th K at 4 solar radii. These
  measurements, together with temperatures for lower heights determined
  from earlier Skylab and eclipse data, suggest that there is a
  maximum in the quiet coronal proton temperature at about 1.5 solar
  radii. Comparison of measured Lyman-alpha intensities with those
  calculated using a representative model for the radial variation of
  the coronal electron density yields information on the magnitude of
  the electron temperature gradient and suggests that the solar wind
  flow was subsonic for distances less than 4 solar radii.

Title: Probing the solar wind acceleration region using spectroscopic
    techniques.
Authors: Withbroe, G. L.; Kohl, J. L.; Weiser, H.; Munro, R. H.
Bibcode: 1982SSRv...33...17W
Altcode:
  Measurements of the intensities and profiles of UV and EUV spectral
  lines can provide a powerful tool for probing the physical
  conditions in the solar corona out to 8 R <SUB>⊙</SUB> and
  beyond. We discuss here how measurements of spectral line radiation
  in conjunction with measurements of the white light K-corona can
  provide information on electron, proton and ion temperatures and
  velocity distribution functions; densities; chemical abundances and
  mass flow velocities. Because of the fundamental importance of such
  information, we provide a comprehensive review of the formation of
  coronal resonance line radiation, with particular emphasis on the H i
  Lα line, and discuss observational considerations such as requirements
  for rejection of stray light and effects of emission from the geocorona
  and interplanetary dust. Finally, we summarize some results of coronal H
  i Lα and white light observations acquired on sounding rocket flights.

Title: 1980 rocket coronagraph measurements of the solar wind
    acceleration region.
Authors: Withbroe, G. L.; Kohl, J. L.; Munro, R. H.; Weiser, H.
Bibcode: 1982SAOSR.392A..99W
Altcode: 1982csss....2...99W
  Spectroscopic measurements of temperatures, densities and flow
  velocities in the solar wind acceleration region provide critical
  empirical constraints on solar stellar wind theory. Preliminary results
  of an analysis of H I Lyman-alpha and white light measurements made on
  16 February 1980 in a polar coronal region are reported. The hydrogen
  kinetic temperatures in the observed region were found to be nearly
  constant with T<SUB>HI</SUB> approximately equals 10 degrees K at
  heliocentric distances between 1.5 and 4 solar radii. The outflow
  velocities were found to be subsonic indicating that the critical
  point in the observed region was located at r approximately greater
  than 4 solar radii.

Title: Shuttle contamination effects on ultraviolet coronagraphic
    observations
Authors: Kohl, J. L.; Weiser, H.
Bibcode: 1982SPIE..287...35K
Altcode:
  The ultraviolet light coronagraph being developed for Shuttle by the
  Harvard-Smithsonian Center for Astrophysics is described. Effects of
  Shuttle contaminants on ultraviolet coronagraphic observations are
  discussed and column densities for acceptable attenuation are provided
  which are generally applicable to high spectral resolution measurements
  in the 600 A - 1700 A spectral range.

Title: The Spacelab Lyman-Alpha and White Light Coronagraphs Program
Authors: Kohl, J. L.; Withbroe, G. L.; Weiser, H.; MacQueen, R. M.;
   Munro, R. H.
Bibcode: 1981SSRv...29..419K
Altcode:
  The Harvard-Smithsonian Center for Astrophysics and the High Altitude
  Observatory have defined a joint coronagraphs experiment for a
  future Spacelab mission. The instrumentation package would include an
  ultraviolet light coronagraph to measure the intensity and profiles of
  spectral lines formed between 1.2 and 8 solar radii from Sun center and
  a white light coronagraph to measure the intensity and polarization
  of visible light. The overall goals of the joint program are to use
  new coronal plasma diagnostic techniques to understand the physical
  processes and mechanisms operating in the solar corona, to understand
  the acceleration of high-speed and low-speed solar wind streams and to
  extrapolate this knowledge to other stars in order to help understand
  the physics of stellar coronae and stellar mass loss.

Title: Ion Beam Measurements of Electron Excitation Coefficients
Authors: Kohl, J. L.; Lafyatis, G. P.; Parkinson, W. H.
Bibcode: 1981BAAS...13Q.911K
Altcode:
  No abstract at ADS

Title: The Pinhole/Occulter Facility
Authors: Hudson, H. S.; Kohl, J. L.; Lin, R. P.; MacQueen, R. M.;
   Tandberg-Hanssen, E.; Pabbs, J. R.
Bibcode: 1981pof..rept.....H
Altcode:
  A large occulting system in space can be used for high resolution
  X-ray observations and for large aperture coronagraphic observations in
  visible and UV light. The X-ray observations can combine high angular
  resolution in hand (10 keV) X-radiation with the high sensitivity
  of a multiple pinhole camera, and can permit sensitive observations
  of bremsstrahlung from nonthermal particles in the corona. The
  large aperture coronagraphs have two major advantages: high angular
  resolution and good photon collection. This will permit observations
  of small scale structures in the corona for the first time and will
  give sufficient counting rates above the coronal background rates
  for sensitive diagnostic analysis of intensities and line profiles
  for coronal structures in the solar wind acceleration region. The
  technical basis for performing observations with a large occulting
  system in these three wavelength ranges is described as well as a
  pinhole/occulter facility presently being considered for Spacelab. Some
  indications about future developments are included.

Title: Results of Ly-α Coronagraphic Observations Following the
    1980 Eclipse
Authors: Weiser, H.; Kohl, J. L.; Munro, R. H.; Withbroe, G. L.
Bibcode: 1981BAAS...13R.913W
Altcode:
  No abstract at ADS

Title: Coronal Outflow Velocities: 1980 Rocket Measurements
Authors: Munro, R. H.; Kohl, J. L.; Weiser, H.; Withbroe, G. L.
Bibcode: 1981BAAS...13..912M
Altcode:
  No abstract at ADS

Title: Shuttle contamination effects on ultraviolet coronographic
    observations.
Authors: Kohl, J. L.; Weiser, H.
Bibcode: 1981SPIE..287...35K
Altcode:
  No abstract at ADS

Title: Solar spectral radiance and irradiance at 225.2-319.6
    nanometers
Authors: Kohl, J. L.; Parkinson, W. H.; Zapata, C. A.
Bibcode: 1980ApJS...44..295K
Altcode:
  Mean absolute intensities (spectral radiance) over 0.1 nm intervals
  between 225.2 nm and 319.6 nm at disk center and near the limb of
  the sun (mu = 0.23 + or - 0.04) are derived from the high spectral
  resolution measurements published by Kohl, Parkinson, and Kurucz. The
  corresponding limb-to-center ratios and spectral irradiance values are
  provided. A comparison with existing measurements of solar spectral
  radiance and spectral irradiance for the most part shows agreement
  within the estimated error limits, although some narrow band variations
  may be outside experimental errors. The contribution to the solar
  constant of the 230-305 nm band is derived to be 19.7 W/square m +
  or - 12%.

Title: Measurements of coronal kinetic temperatures from 1.5 to 3
    solar radii
Authors: Kohl, J. L.; Weiser, H.; Withbroe, G. L.; Noyes, R. W.;
   Parkinson, W. H.; Reeves, E. M.; Munro, R. H.; MacQueen, R. M.
Bibcode: 1980ApJ...241L.117K
Altcode:
  A rocket-borne Lyman-alpha coronagraph has been used to make the first
  measurements of the spectral line profile of resonantly scattered
  hydrogen Lyman-alpha coronal radiation between 1.5 and 3 solar
  radii. These data provide, for the first time, direct measurements of
  coronal temperatures above 1.5 solar radii. Data were obtained in a
  coronal hole, quiet region, and streamer. The widths of the profiles
  from the quiet region decrease with height and correspond to a steady
  decrease in hydrogen kinetic temperature, with increasing radius, from
  about 2.5 million K at r = 2 solar radii to about 1 million K at r =
  9 solar radii. In the coronal hole the measured line widths indicate
  a kinetic temperature of 1.8 million K at r = 2.5 solar radii.

Title: Coronagraphic H I Lyman-Alpha Observations following the 1980
    Solar Eclipse
Authors: Weiser, H.; Kohl, J. L.; Parkinson, W. H.; Withbroe, G. L.
Bibcode: 1980BAAS...12R.917W
Altcode:
  No abstract at ADS

Title: The Spacelab Lyman-Alpha and White-Light Coronagraphs Program
Authors: Kohl, J. L.; MacQueen, R. W.; Withbroe, G. L.; Munro, R.;
   Weiser, H.
Bibcode: 1980BAAS...12..793K
Altcode:
  No abstract at ADS

Title: Implications of Lyman α Measurements on Coronal Electron
    and Proton Temperatures between 2.0 and 4.0 R<SUB>⊙</SUB>
Authors: Withbroe, G. L.; Kohl, J. L.; Weiser, H.
Bibcode: 1980BAAS...12Q.917W
Altcode:
  No abstract at ADS

Title: (Invited Paper) Spectroscopy of the Corona between 1 and 8
    Solar Radii
Authors: Withbroe, G.; Kohl, J.
Bibcode: 1980BAAS...12..544W
Altcode:
  No abstract at ADS

Title: Computer assisted performance tests of the Lyman Alpha
    Coronagraph
Authors: Parkinson, W. H.; Kohl, J. L.
Bibcode: 1979hco..rept.....P
Altcode:
  Preflight calibration and performance tests of the Lyman Alpha
  Coronagraph rocket instrument in the laboratory, with the experiment
  in its flight configuration and illumination levels near those
  expected during flight were successfully carried out using a pulse
  code modulation telemetry system simulator interfaced in real time to
  a PDP 11/10 computer system. Post acquisition data reduction programs
  developed and implemented on the same computer system aided in the
  interpretation of test and calibration data.

Title: High resolution atmospheric transmission calculations down
    to 28.7 km in the 200-243-nm spectral range (TE)
Authors: Cann, M. W. P.; Evans, W. F. J.; Kohl, J. L.; Kurucz, R.;
   Parkinson, W. H.; Reeves, E. M.; Nicholls, Ralph W.
Bibcode: 1979ApOpt..18..964C
Altcode:
  Decrease in stratospheric ozone absorption and increase in oxygen
  absorption with decreasing wavelength combine to produce a window
  of maximum atmospheric transmission near 210 nm. Since solar
  radiation in this spectral region dissociates molecular oxygen,
  the deep atmospheric penetration at this wavelength is of particular
  aeronomical interest. High resolution calculations of the transmittance
  down to 28.65 km were made for the 200-243-nm spectral range in this
  window region, in support of a stratospheric balloon flight from Fort
  Churchill in July 1974. The calculations were made by dividing the
  atmosphere into layers which were chosen so that each could be assumed
  homogeneous; optical depths were calculated separately for each of
  these layers and then summed to obtain the over-all transmittance of the
  atmosphere. Absorption by molecular oxygen (line and continuum) and by
  ozone was included, as well as extinction through Rayleigh scattering
  by air molecules. The calculated transmittances were combined with high
  altitude (above 100-km) rocket measurements of the sun-center spectrum
  and center-to-limb variations to give residual high resolution solar
  spectral flux for several altitudes and solar zenith angles.

Title: Lyman Alpha Line Profiles from 1.5 to 3.0 Solar Radii.
Authors: Kohl, J. L.; Weiser, H.; Withbroe, G. L.; Munro, R. H.;
   Parkinson, W. H.; Reeves, E. M.
Bibcode: 1979BAAS...11..398K
Altcode:
  No abstract at ADS

Title: Comparison of Satellite and Rocket Coronal Observations around
    April 13, 1979
Authors: Howard, R. A.; Michels, D. J.; Koomen, M. J.; Sheeley, N. R.,
   Jr.; Kohl, J. L.; Munro, R. H.; Weiser, H.
Bibcode: 1979BAAS...11..408H
Altcode:
  No abstract at ADS

Title: Lyman-α and White Light Observations of the Outer Solar
    Corona.
Authors: Munro, R. H.; Kohl, J. L.; MacQueen, R. M.; Noyes, R. W.;
   Parkinson, W. H.; Weiser, H.; Withbroe, G. L.
Bibcode: 1979BAAS...11..398M
Altcode:
  No abstract at ADS

Title: The Rocket Lyman Alpha Coronagraph
Authors: Weiser, H.; Kohl, J. L.; Kirkham, B.
Bibcode: 1979BAAS...11..397W
Altcode:
  No abstract at ADS

Title: Spectroscopic mapping of solar wind velocities
Authors: Kohl, J. L.
Bibcode: 1978clus.nasa..354K
Altcode:
  During the total solar eclipse of 1970, measurements of resonantly
  scattered Lyman-alpha radiation from the solar corona revealed a means
  to determine temperatures and densities in the solar corona beyond 1.5
  R solar radii. A natural extension of this work is to use the Solar
  Probe to measure the spectral line profile of Lyman-alpha radiation
  backscattered toward the Sun from coronal regions between 4 R solar
  radii and 10 R solar radii. The backscattered profile would provide
  unique and quantitative determinations of the outlaw velocities of
  coronal material into the solar wind. Such information is of critical
  importance for understanding solar-wind formation and solar-terrestrial
  effects on the earth's climate. There is no known way to obtain this
  information without a Solar Probe-type mission.

Title: Absolute cross section for photoionization of atomic oxygen
Authors: Kohl, J. L.; Lafyatis, G. P.; Palenius, H. P.; Parkinson,
   W. H.
Bibcode: 1978PhRvA..18..571K
Altcode:
  The absolute cross section for photoionization of atomic oxygen from
  the 2p4 3P ground state of O(0) to the 2p3 4S ground state of O(+)
  has been measured at five narrow wavelength intervals between 89.8 and
  76.2 nm. The cross section near the 2p3 4S threshold is 4.5 Mb + or -
  7%. Recent calculations by Taylor and Burke (1976) and by Pradhan
  and Saraph (1977) are in reasonable agreement with this work. The
  dipole-length results of Taylor and Burke (4.1 Mb) are in better
  agreement with the experiment than their dipole-velocity results
  (3.2 Mb).

Title: The Lyman alpha coronagraph.
Authors: Kohl, J. L.; Reeves, E. M.; Kirkham, B.
Bibcode: 1978nisa.symp...91K
Altcode: 1978nisa.conf...91K
  No abstract at ADS

Title: Center and limb solar spectrum in high spectral resolution
    225.2 NM to 319.6 NM
Authors: Kohl, John L.; Parkinson, William H.; Kurucz, Robert L.
Bibcode: 1978clss.book.....K
Altcode: 1978QB551.K63......
  The atlas has been designed to fulfill the need in solar and stellar
  astronomy, in aeronomy, and in space science for a convenient reference
  source that provides a detailed and accurate record of the measured
  solar ultraviolet spectrum in high spectral resolution for the
  wavelength range from 225.2 nm to 319.6 nm. The atlas also contains
  a preliminary synthetic solar spectrum with a legend for identifying
  and describing the features of the synthetic spectrum. Attention is
  given to aspects of instrumentation, the radiometric calibration,
  the wavelength scale, background noise random fluctuations and
  data filtering, intermittent noise, the observational conditions,
  the experimental uncertainty, the atlas format, references, tables,
  and plots.

Title: The Lyman alpha coronagraph
Authors: Kohl, J. L.; Reeves, E. M.; Kirkham, B.
Bibcode: 1977cosp.meetU....K
Altcode:
  The rocket-borne Lyman alpha coronagraph (RLAC) is to be used in the
  absence of a natural solar eclipse to determine coronal temperatures
  from measurements of the line width of Lyman-alpha and to determine
  neutral hydrogen densities of coronal material from the absolute
  intensity. The coronagraph consists of a 75-cm Fastie-Ebert scanning
  spectrometer with an AMR 641 photoelectric detection system, an off-axis
  parabolic primary mirror, and an occulting system. A special optical
  arrangement achieves rejection of radiation from the solar disk.

Title: The solar boron abundance.
Authors: Kohl, J. L.; Parkinson, W. H.; Withbroe, G. L.
Bibcode: 1977ApJ...212L.101K
Altcode:
  Positive evidence for the presence of boron in the sun is reported,
  and the chemical abundance of boron in the photosphere is derived from
  photoelectric measurements of the solar spectrum near 2500 A obtained
  with a rocketborne high-resolution spectrometer. Short sections
  of the spectrum in the vicinities of the B I lines at 2496.772
  and 2497.723 A are plotted. The photospheric boron abundance is
  determined primarily by analyzing the solar-center spectrum near the
  first of the two lines in the framework of several single-component
  photospheric models. The logarithmic boron abundance obtained is 2.6,
  with an estimated uncertainty of plus or minus 0.3 dex, on the scale
  where that of hydrogen is 12.0. This value is shown to be in excellent
  agreement with that predicted for a nucleosynthesis model in which Li,
  Be, and B are produced by cosmic-ray spallation.

Title: The components of the Balmer-alpha line of He II in the Sun.
Authors: Kohl, J. L.
Bibcode: 1977ApJ...211..958K
Altcode:
  New photoelectric measurements of the absolute intensities of the
  components of the Balmera line of He ii in the Sun with a spectral
  resolution of 0.029 A are reported. Highly constrained curve fits are
  used to test the consistency of the measurements with the line widths
  that are predicted by a recombination model, a collisional excitation
  model, and a combination of the two. Neither model alone is fully
  consistent with the measurements. For the "quiet Sun," about 287o of
  the total intensity of the Balmer-a line of He ii is attributed to the
  recombination mechanism. Collisional excitation appears to dominate
  for the n = 3 level. The recombination mechanism is apparently more
  important in the active Sun because measurements of a very quiet Sun do
  not show the narrow He ii peaks that were observed in measurements of
  a more active Sun. Subject headings: Sun: chromosphere - Sun: corona -
  Sun: spectra

Title: Absolute Photoionization Cross-Section for 0 I 3p --&gt;
    0 II <SUP>4</SUP>S<SUP>0</SUP>.
Authors: Kohl, J. L.; Lafayetis, G.; Polenius, H. P.; Parkinson, W. H.
Bibcode: 1977uxsa.coll....5K
Altcode: 1977IAUCo..43....5K
  No abstract at ADS

Title: Absolute measurement of the photoionization cross section of
    atomic hydrogen with a shock tube for the extreme ultraviolet
Authors: Palenius, H. P.; Kohl, J. L.; Parkinson, W. H.
Bibcode: 1976PhRvA..13.1805P
Altcode:
  The paper reports an experiment which is part of a program to measure
  the absolute values of the atomic photoionization cross sections of
  astrophysically abundant elements, particularly in stars and planetary
  atmospheres. An aerodynamic pressure-driven shock tube constructed from
  stainless steel with a quadratic cross section was used to measure the
  photoionization cross section of H I at 19 wavelength points from 910
  to 609 A with experimental uncertainties between 7 and 20%. The shock
  tube was used to produce fully dissociated hydrogen and neon mixtures
  for the photoabsorption measurements.

Title: The Mg II h and k lines. I. Absolute center and limb
    measurements of the solar profiles.
Authors: Kohl, J. L.; Parkinson, W. H.
Bibcode: 1976ApJ...205..599K
Altcode:
  We report new measurements of the solar Mg II h and k lines with
  uncertainties in the absolute intensities at k1 and h1 of - 20 to +
  12 percent with smaller uncertainties for higher intensities. The
  spectral resolution, defined by the full width at half-maximum of the
  instrumental profile, was 0.028 A, and the angular resolution element
  was 184" by 1,5. Measurements were made for a quiet region near the disk
  center and for a quiet region at cos 0 = 0.23. The measured profiles
  are suitable for detailed comparisons with theoretical solar and stellar
  profiles, as will be discussed in the paper by Ayres and Linsky (Paper
  II) that will follow in a later issue. Our measured minimum intensities
  (k1 and h1) relative to the core intensities (k3 and h3) and to the
  average peak intensities (k2 and h2) are fainter than the corresponding
  intensities that were reported by Lemaire and Skumanich. Subject
  headings: line profiles - Sun: spectra - ultraviolet: spectra

Title: The Solar Profiles of the Hyperfine Components of HeII 1640
    A From Rocket Observations.
Authors: Kohl, J. L.; Parkinson, W. H.
Bibcode: 1975BAAS....7..450K
Altcode:
  No abstract at ADS

Title: Measurements of Solar Line Profiles between 1175 and 3200 Å
Authors: Kohl, J. L.; Parkinson, W. H.; Reeves, E. M.
Bibcode: 1975BAAS....7R.360K
Altcode:
  No abstract at ADS

Title: Rocket spectrometer for investigation of the far ultraviolet
    solar spectrum
Authors: Parkinson, W. H.; Reeves, E. M.; Kohl, J. L.
Bibcode: 1974hco..rept.....P
Altcode:
  A rocket-borne Ebert spectrometer and telescope were used for
  analysis of the solar spectrum. The instrument was arranged in the high
  resolution line scanning mode. Selected emission lines between 1170 and
  1640 A were scanned, and a complete wavelength scan was made from 1170
  A to 1850 A. Accurate measurements were made of the line profiles of
  the He II lines at 1640 A, C IV lines at 1550 A, Si IV lines at 1400
  A, C II lines at 1335 A, the N V lines at 1240 A, and the C III lines
  at 1175 A. Accurate intensity measurements of the quiet sun spectrum
  for wavelengths between 1174 A and 3220 A were obtained. Spectral
  resolution was better than 0.03 A over most of the range and spatial
  resolution was relatively low so that the observations are averaged
  over the chromospheric network. Plots of absolute intensity versus wave
  length were prepared for the full wavelength range of the observations.

Title: Absolute Intensity Calibration of a High-Resolution Rocket
    Spectrometer
Authors: Kohl, J. L.; Parkinson, W. H.
Bibcode: 1974spop.conf..511K
Altcode:
  No abstract at ADS

Title: Measurement of the Neutral-Aluminum Photoionization
    Cross-Section and Parameters of the 3p 2PO-3s3p2 2S112 Autoionization
    Doublet
Authors: Kohl, J. L.; Parkinson, W. H.
Bibcode: 1973ApJ...184..641K
Altcode:
  The photoionization cross-section of neutral aluminum for absorption
  from the 3p 2P0 ground state was measured between 207.0 and 173
  nanometers (hm) by use of the aerodynamic shock tube. The population
  number density of the ground state was determined directly and precisely
  by using hook-method measurements of the 3p 2P'112,312-4s 2S112
  transitions. Our measured value at the first ionization limit of 65 i 7
  Mbarns is considerably greater than earlier theoretical and experimental
  values. This cross-section, when used in the solar model of Vernazza,
  Avrett, and Loeser, improves the agreement between the predicted solar
  intensity below the aluminum limit and the observations. The absolute
  values of the Shore autoionization parameters for the aluminum doublet
  at 193.20 and 193.64 nm were found to be equal within the experimental
  accuracy and are b = 133Mb + l2percent,F = 6.84 x 10-15ergs j 3percent,a
  = -55Mb + 32percentforthemoreaccurately determined line at 193.64
  nm. Subject headings:autoionization - opacities - spectra, solar -
  spectra, ultraviolet - transition probabilities

Title: High Resolution Rocket Observations of Solar Line Profiles
    between 166.0 and 154.7 nm
Authors: Kohl, J. L.; Parkinson, W. H.; Reeves, E. M.
Bibcode: 1973BAAS....5R.274K
Altcode:
  No abstract at ADS

