Author name code: domingo
ADS astronomy entries on 2022-09-14
author:"Domingo, Vicente" 
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Title: The Polarimetric and Helioseismic Imager on Solar Orbiter
Authors: Solanki, S. K.; del Toro Iniesta, J. C.; Woch, J.; Gandorfer,
   A.; Hirzberger, J.; Alvarez-Herrero, A.; Appourchaux, T.; Martínez
   Pillet, V.; Pérez-Grande, I.; Sanchis Kilders, E.; Schmidt, W.;
   Gómez Cama, J. M.; Michalik, H.; Deutsch, W.; Fernandez-Rico, G.;
   Grauf, B.; Gizon, L.; Heerlein, K.; Kolleck, M.; Lagg, A.; Meller, R.;
   Müller, R.; Schühle, U.; Staub, J.; Albert, K.; Alvarez Copano, M.;
   Beckmann, U.; Bischoff, J.; Busse, D.; Enge, R.; Frahm, S.; Germerott,
   D.; Guerrero, L.; Löptien, B.; Meierdierks, T.; Oberdorfer, D.;
   Papagiannaki, I.; Ramanath, S.; Schou, J.; Werner, S.; Yang, D.;
   Zerr, A.; Bergmann, M.; Bochmann, J.; Heinrichs, J.; Meyer, S.;
   Monecke, M.; Müller, M. -F.; Sperling, M.; Álvarez García, D.;
   Aparicio, B.; Balaguer Jiménez, M.; Bellot Rubio, L. R.; Cobos
   Carracosa, J. P.; Girela, F.; Hernández Expósito, D.; Herranz, M.;
   Labrousse, P.; López Jiménez, A.; Orozco Suárez, D.; Ramos, J. L.;
   Barandiarán, J.; Bastide, L.; Campuzano, C.; Cebollero, M.; Dávila,
   B.; Fernández-Medina, A.; García Parejo, P.; Garranzo-García, D.;
   Laguna, H.; Martín, J. A.; Navarro, R.; Núñez Peral, A.; Royo, M.;
   Sánchez, A.; Silva-López, M.; Vera, I.; Villanueva, J.; Fourmond,
   J. -J.; de Galarreta, C. Ruiz; Bouzit, M.; Hervier, V.; Le Clec'h,
   J. C.; Szwec, N.; Chaigneau, M.; Buttice, V.; Dominguez-Tagle, C.;
   Philippon, A.; Boumier, P.; Le Cocguen, R.; Baranjuk, G.; Bell,
   A.; Berkefeld, Th.; Baumgartner, J.; Heidecke, F.; Maue, T.; Nakai,
   E.; Scheiffelen, T.; Sigwarth, M.; Soltau, D.; Volkmer, R.; Blanco
   Rodríguez, J.; Domingo, V.; Ferreres Sabater, A.; Gasent Blesa,
   J. L.; Rodríguez Martínez, P.; Osorno Caudel, D.; Bosch, J.; Casas,
   A.; Carmona, M.; Herms, A.; Roma, D.; Alonso, G.; Gómez-Sanjuan, A.;
   Piqueras, J.; Torralbo, I.; Fiethe, B.; Guan, Y.; Lange, T.; Michel,
   H.; Bonet, J. A.; Fahmy, S.; Müller, D.; Zouganelis, I.
Bibcode: 2020A&A...642A..11S
Altcode: 2019arXiv190311061S
  <BR /> Aims: This paper describes the Polarimetric and Helioseismic
  Imager on the Solar Orbiter mission (SO/PHI), the first magnetograph and
  helioseismology instrument to observe the Sun from outside the Sun-Earth
  line. It is the key instrument meant to address the top-level science
  question: How does the solar dynamo work and drive connections between
  the Sun and the heliosphere? SO/PHI will also play an important role
  in answering the other top-level science questions of Solar Orbiter,
  while hosting the potential of a rich return in further science. <BR
  /> Methods: SO/PHI measures the Zeeman effect and the Doppler shift
  in the Fe I 617.3 nm spectral line. To this end, the instrument
  carries out narrow-band imaging spectro-polarimetry using a tunable
  LiNbO<SUB>3</SUB> Fabry-Perot etalon, while the polarisation modulation
  is done with liquid crystal variable retarders. The line and the nearby
  continuum are sampled at six wavelength points and the data are recorded
  by a 2k × 2k CMOS detector. To save valuable telemetry, the raw data
  are reduced on board, including being inverted under the assumption of
  a Milne-Eddington atmosphere, although simpler reduction methods are
  also available on board. SO/PHI is composed of two telescopes; one,
  the Full Disc Telescope, covers the full solar disc at all phases of
  the orbit, while the other, the High Resolution Telescope, can resolve
  structures as small as 200 km on the Sun at closest perihelion. The high
  heat load generated through proximity to the Sun is greatly reduced by
  the multilayer-coated entrance windows to the two telescopes that allow
  less than 4% of the total sunlight to enter the instrument, most of
  it in a narrow wavelength band around the chosen spectral line. <BR />
  Results: SO/PHI was designed and built by a consortium having partners
  in Germany, Spain, and France. The flight model was delivered to
  Airbus Defence and Space, Stevenage, and successfully integrated into
  the Solar Orbiter spacecraft. A number of innovations were introduced
  compared with earlier space-based spectropolarimeters, thus allowing
  SO/PHI to fit into the tight mass, volume, power and telemetry budgets
  provided by the Solar Orbiter spacecraft and to meet the (e.g. thermal)
  challenges posed by the mission's highly elliptical orbit.

Title: Small magnetic structures near the polar regions of the Sun
Authors: Cabello, I.; Blanco Rodríguez, J.; Balmaceda, L.; Domingo, V.
Bibcode: 2017IAUS..327...40C
Altcode:
  The study of the small magnetic structures of the solar photosphere
  is of great relevance because of their association with concentrations
  of magnetic field and their possible contribution to the variations of
  the Total Solar Irradiance. These structures are known to appear close
  to active regions and ubiquitously in the quiet Sun areas. Numerous
  studies about their distribution across all over the solar surface
  have been done with high-resolution instrumentation. However, since the
  observations have always been carried out from the ecliptic plane, their
  distribution near the polar regions is not well known. Future missions,
  like Solar Orbiter, will certainly provide valuable information on
  these yet unexplored regions. In this work, and in preparation for
  that moment, we select favorable periods for the observation of the
  polar regions of the Sun, and study the fraction of covered surface
  by small magnetic structures and its variation with the solar activity.

Title: Detección y análisis de pequeñas estructuras magnéticas
    en las regiones próximas a los polos solares
Authors: Cabello, I.; Blanco Rodríguez, J.; Balmaceda, L.; Domingo, V.
Bibcode: 2017BAAA...59..154C
Altcode:
  The solar magnetic field plays a fundamental role in the overall
  behaviour of the Sun. In the solar photosphere, the magnetic field
  is evidenced with a wide range of structures with different sizes,
  shapes and intensities. Bright Points (BPs) are the smallest of these
  manifestations discernible with the current instruments, and their
  presence is observable all over the solar disk, on both active and
  quiet regions. However, due to difficulties in observing polar areas,
  the presence of BPs in these regions is poorly known so far. The Solar
  Orbiter mission will be launched in 2018 and will observe the Sun up
  to 30º outside the ecliptic, allowing the analysis of BPs appearance
  in areas close to the solar poles. A preliminar study can be done
  considering the inclination of the ecliptic plane relative to the
  solar axis, so that these regions can be observed at certain times
  in the year. In this work, G-band images have been used to detect and
  analyse BPs located in areas close to the solar poles.

Title: Multi-wavelength observations of vortex-like flows in the
    photosphere using ground-based and space-borne telescopes
Authors: Palacios, J.; Vargas Domínguez, S.; Balmaceda, L. A.;
   Cabello, I.; Domingo, V.
Bibcode: 2017arXiv170400660P
Altcode:
  In this work we follow a series of papers on high-resolution
  observations of small-scale structures in the solar atmosphere
  \citep[][Cabello et al., in prep]{Balmaceda2009, Balmaceda2010,
  Vargas2011, Palacios2012, Domingo2012, Vargas2015}, combining several
  multi-wavelength data series. These were acquired by both ground-based
  (SST) and space-borne (Hinode) instruments during the joint campaign of
  the Hinode Operation Program 14, in September 2007. Diffraction-limited
  SST data were taken in the G-band and G-cont, and were restored by
  the MFBD technique. Hinode instruments, on the other hand, provided
  multispectral data from SOT-FG in the CN band, and Mg~{\sc I} and
  Ca {\sc II}~lines, as well as from SOT-SP in the Fe~{\sc I} line. In
  this series of works we have thoroughly studied vortex flows and their
  statistical occurrences, horizontal velocity fields by means of Local
  Correlation Tracking (LCT), divergence and vorticity. Taking advantage
  of the high-cadence and high spatial resolution data, we have also
  studied bright point statistics and magnetic field intensification,
  highlighting the importance of the smallest-scale magnetic element
  observations.

Title: Multi-wavelength Observations of Photospheric Vortex Flows
    in the Photosphere Using Ground-based and Space-borne Telescopes
Authors: Palacios, J.; Vargas Domínguez, S.; Balmaceda, L. A.;
   Cabello, I.; Domingo, V.
Bibcode: 2016ASPC..504..139P
Altcode:
  In this work we follow a series of papers on high-resolution
  observations of small-scale structures in the solar atmosphere
  (Balmaceda et al. 2009, 2010; Vargas Domínguez et al. 2011; Palacios et
  al. 2012; Domingo et al. 2012; Vargas Domínguez et al. 2015, Cabello et
  al., in prep), combining several multi-wavelength data series. These
  were acquired by both ground-based (SST) and space-borne (Hinode)
  instruments during the joint campaign of the Hinode Operation Program
  14, in September 2007. Diffraction-limited SST data were taken in the
  G-band and G-cont, and were restored by the MFBD technique. Hinode
  instruments, on the other hand, provided multispectral data from SOT-FG
  in the CN band, and Mg I and Ca II lines, as well as from SOT-SP in
  the Fe I line. In this series of works we have thoroughly studied
  vortex flows and their statistical occurrences, horizontal velocity
  fields by means of Local Correlation Tracking (LCT), divergence and
  vorticity. Taking advantage of the high-cadence and high spatial
  resolution data, we have also studied bright point statistics and
  magnetic field intensification, highlighting the importance of the
  smallest-scale magnetic element observations.

Title: Influence of a plasma swirl motion on fine magnetic
    concentrations in the solar photosphere
Authors: Palacios, Judith; Balmaceda, Laura; Cabello, Iballa; Domingo,
   Vicente
Bibcode: 2016Tecci..11....1P
Altcode:
  High-resolution observations from ground-based (Solar Swedish Telescope)
  and space-borne (Hinode) solar telescopes acquired data with various
  filters, obtaining images of a quiet Sun region populated with
  small-scale magnetic elements. The region is also characterized by the
  presence of photospheric swirl convective plasma structures. This work
  abridges the results of different analyses applied over time series of
  images to follow the evolution of magnetic features aiming to establish
  the influence of the plasma vortices on their motions.

Title: Evolution of Small-Scale Magnetic Elements in the Vicinity
    of Granular-Sized Swirl Convective Motions
Authors: Vargas Domínguez, S.; Palacios, J.; Balmaceda, L.; Cabello,
   I.; Domingo, V.
Bibcode: 2015SoPh..290..301V
Altcode: 2014SoPh..tmp..187V; 2014arXiv1405.2380V
  Advances in solar instrumentation have led to widespread use of time
  series to study the dynamics of solar features, especially at small
  spatial scales and at very fast cadences. Physical processes at such
  scales are important as building blocks for many other processes
  occurring from the lower to the upper layers of the solar atmosphere
  and beyond, ultimately for understanding the larger picture of solar
  activity. Ground-based (Swedish Solar Telescope) and space-borne
  (Hinode) high-resolution solar data are analyzed in a quiet-Sun region
  that displays negative-polarity small-scale magnetic concentrations
  and a cluster of bright points observed in G-band. The region is
  characterized by two granular-sized convective vortex-type plasma
  motions, one of which appears to be affecting the dynamics of magnetic
  features and bright points in its vicinity and is therefore the main
  target of our investigations. We followed the evolution of the bright
  points, intensity variations at different atmospheric height, and
  the magnetic evolution for a set of interesting selected regions. We
  describe the evolution of the photospheric plasma motions in the region
  near the convective vortex and some plausible cases for convective
  collapse detected in Stokes profiles.

Title: Magnetic evolution of faculae observed with IMaX
Authors: Blanco, J.; Palacios, J.; Cabello, I.; Domingo, V.;
   Sunrise Team
Bibcode: 2013hsa7.conf..803B
Altcode:
  The SUNRISE mission, consisting of a one metre diameter telescope on
  board a stratospheric balloon, was launched on June 2009 on route over
  the artic circle. At approximately 36 km height, the balloon flight
  allowed to observe with almost no atmospheric influence yielding
  very good quality data as well as observations in ultraviolet
  spectral lines (by means of the SUFI instrument). The mission's
  artic summer-circumpolar flight path provided continuous solar
  observations, without day-night cycles, during the almost 5 days of
  the mission. IMaX/SUNRISE instrument --developed by a consortium of
  Spanish institutions-- is a spectropolarimeter based in the use of a
  Fabry-Pérot etalon and liquid crystals for spectral and polarimetric
  analysis, respectively. It obtained full-Stokes vector maps at the
  selected wavelength of Fe I 5250.2 Å with a temporal cadence of
  around 30 seconds and a spatial resolution of approximately 0.15--0.18
  arcsec. In this poster, we present a temporal series of a group of limb
  faculae comprising approximately 21 minutes. Thanks to the data quality,
  as well as the full-Stokes maps and fast temporal cadence, small-scale
  magnetic cancellations and emergences can be observed around and at
  the faculae positions. We focused on a small area of the instrument
  field of view where the cancellation magnetogram shows high magnetic
  polarity changes. What we observe are confronted patches of opposite
  polarities from the longitudinal magnetic field, being cancelled
  and reappearing, while the transversal field signal present changes
  also accordingly. This reflects as well in the continuum intensity
  images where facular brightenings are seen enhancing and decreasing
  in consonance with the transversal field evolution. Studies of this
  cancellation phenomena and evolution of the facular structures as
  magnetic tubes are being performed for more thorough analyses.

Title: Study of small magnetic structures in the solar photosphere
Authors: Cabello, I.; Domingo, V.; Bonet, J. A.; Blanco Rodríguez,
   J.; Balmaceda, L. A.
Bibcode: 2013hsa7.conf..805C
Altcode:
  The study of small scale magnetic structures in the solar photosphere
  is of great relevance for the understanding of the global behaviour of
  the Sun. Because of the small spatial and temporal scales involved, the
  use of high resolution images and fast cadence is fundamental for their
  study. In order to obtain such images, sophisticated computational
  techniques that compensate for the atmospheric degradation and
  telescope aberration have been developed, improving in this way the
  spatial resolution. In this work, we use G-band images obtained with
  the 1 m-Swedish Solar Telescope located at La Palma (Canary Islands,
  Spain). The images have been restored with MOMFBD (Multi-Object
  Multi-Frame Blind Deconvolution), a technique that combines multiple
  images acquired in a short time interval. The resulting images have
  a resolution close to the diffraction limit of the telescope (0.1
  arcsec) allowing the study of very small bright structures present
  in the inter-granular lanes in the solar photosphere, known as Bright
  Points. It is highlighted the great presence of magnetic structures in
  quiet Sun regions analyzed from different observational campaigns. The
  density of BPs in the quiet Sun shows a decrease as we approach the
  limb, with values of ≃q 1% at the centre (μ ≈ 1), and ≃q 0.2%
  at μ ≈ 0.3. We also present the discovery of small vortexes detected
  in the solar surface through the movement of BPs, with radii around 241
  km and lifetimes longer than 5 minutes. Further analyses, comprising
  longer time series and information from different solar layers, are
  being performed aiming at a more in-depth knowledge of these phenomena.

Title: Small magnetic bright structures in the quiet Sun
Authors: Domingo, V.; Cabello, I.; Blanco Rodríguez, J.
Bibcode: 2013hsa7.conf..782D
Altcode:
  This work aims at further developing our knowledge of the ubiquitous
  small scale magnetic structures of the solar surface, focusing on
  the poles of the Sun. To get a clearer view of the situation at the
  very high latitudes, we make use of the inclination of the solar axis
  with respect to the ecliptic. We find the known continuous decrease of
  the area covered by bright points from centre to limb. However, when
  the solar rotation axis is inclined toward us there is an increase in
  bright points areas coverage near the limb, i.e. near the poles.

Title: Structure of Small Magnetic Elements in the Solar Atmosphere
Authors: Domingo, V.; Palacios, J.; Balmaceda, L. A.; Domínguez,
   S. V.; Cabello, I.
Bibcode: 2012ASPC..454...69D
Altcode: 2012arXiv1209.0978D
  High resolution images at different wavelengths, spectrograms and
  magnetograms, representing different levels of the solar atmosphere
  obtained with Hinode have been combined to study the 3-dimensional
  structure of the small magnetic elements in relation to their
  radiance. A small magnetic element is described as example of the study.

Title: Observations of Vortex Motion in the Solar Photosphere Using
    Hinode-SP Data
Authors: Palacios, J.; Balmaceda, L. A.; Domínguez, S. V.; Cabello,
   I.; Domingo, V.
Bibcode: 2012ASPC..454...51P
Altcode: 2012arXiv1209.0190P
  In this work, we focus in the magnetic evolution of a small
  region as seen by Hinode-SP during the time interval of about one
  hour. High-cadence LOS magnetograms and velocity maps were derived,
  allowing the study of different small-scale processes such as the
  formation/dissappearance of bright points accompanying the evolution
  of an observed convective vortical motion.

Title: First Results from the SUNRISE Mission
Authors: Solanki, S. K.; Barthol, P.; Danilovic, S.; Feller, A.;
   Gandorfer, A.; Hirzberger, J.; Jafarzadeh, S.; Lagg, A.; Riethmüller,
   T. L.; Schüssler, M.; Wiegelmann, T.; Bonet, J. A.; González,
   M. J. M.; Pillet, V. M.; Khomenko, E.; Yelles Chaouche, L.; Iniesta,
   J. C. d. T.; Domingo, V.; Palacios, J.; Knölker, M.; González,
   N. B.; Borrero, J. M.; Berkefeld, T.; Franz, M.; Roth, M.; Schmidt,
   W.; Steiner, O.; Title, A. M.
Bibcode: 2012ASPC..455..143S
Altcode:
  The SUNRISE balloon-borne solar observatory consists of a 1m aperture
  Gregory telescope, a UV filter imager, an imaging vector polarimeter,
  an image stabilization system, and further infrastructure. The first
  science flight of SUNRISE yielded high-quality data that reveal the
  structure, dynamics, and evolution of solar convection, oscillations,
  and magnetic fields at a resolution of around 100 km in the quiet
  Sun. Here we describe very briefly the mission and the first results
  obtained from the SUNRISE data, which include a number of discoveries.

Title: Detection of Vortex Tubes in Solar Granulation from
    Observations SUNRISE
Authors: Steiner, O.; Franz, M.; González, N. B.; Nutto, C.; Rezaei,
   R.; Pillet, V. M.; Bonet, J. A.; Iniesta, J. C. d. T.; Domingo, V.;
   Solanki, S. K.; Knölker, M.; Schmidt, W.; Barthol, P.; Gandorfer, A.
Bibcode: 2012ASPC..455...35S
Altcode:
  We investigated a time series of continuum intensity maps and
  Dopplergrams of granulation in a very quiet solar region at the disk
  center, recorded with the Imaging Magnetograph eXperiment (IMaX)
  on board the balloon-borne solar observatory SUNRISE. We find that
  granules frequently show substructure in the form of lanes composed of
  a leading bright rim and a trailing dark edge, which move together
  from the boundary of a granule into the granule itself. We find
  strikingly similar events in synthesized intensity maps from an ab
  initio numerical simulation of solar surface convection. We conclude
  that these granular lanes are the visible signature of (horizontally
  oriented) vortex tubes. The characteristic optical appearance of vortex
  tubes at the solar surface is explained. This paper is a summary and
  update of the results previously presented in Steiner et al. (2010).

Title: Supersonic Magnetic Flows in the Quiet Sun Observed with
    SUNRISE/IMaX
Authors: Borrero, J. M.; Pillet, V. M.; Schlichenmaier, R.; Schmidt,
   W.; Berkefeld, T.; Solanki, S. K.; Bonet, J. A.; Iniesta, J. C. d. T.;
   Domingo, V.; Barthol, P.; Gandorfer, A.
Bibcode: 2012ASPC..455..155B
Altcode: 2012arXiv1202.4354B
  In this contribution we describe some recent observations of high-speed
  magnetized flows in the quiet Sun granulation. These observations
  were carried out with the Imaging Magnetograph eXperiment (IMaX)
  onboard the stratospheric balloon SUNRISE, and possess an unprecedented
  spatial resolution and temporal cadence. These flows were identified as
  highly shifted circular polarization (Stokes V) signals. We estimate
  the LOS velocity responsible for these shifts to be larger than 6 km
  s<SUP>-1</SUP>, and therefore we refer to them as supersonic magnetic
  flows. The average lifetime of the detected events is 81.3 s and
  they occupy an average area of about 23 000 km<SUP>2</SUP>. Most of
  the events occur within granular cells and correspond therefore to
  upflows. However some others occur in intergranular lanes or bear no
  clear relation to the convective velocity pattern. We analyze a number
  of representative examples and discuss them in terms of magnetic loops,
  reconnection events, and convective collapse.

Title: Actinide and Ultra-Heavy Abundances in the Local Galactic
Cosmic Rays: An Analysis of the Results from the LDEF Ultra-Heavy
    Cosmic-Ray Experiment
Authors: Donnelly, J.; Thompson, A.; O'Sullivan, D.; Daly, J.; Drury,
   L.; Domingo, V.; Wenzel, K. -P.
Bibcode: 2012ApJ...747...40D
Altcode:
  The LDEF Ultra-Heavy Cosmic-Ray Experiment (UHCRE) detected
  Galactic cosmic rays (GCRs) of charge Z &gt;= 70 in Earth orbit
  with an exposure factor of 170 m<SUP>2</SUP> sr yr, much larger
  than any other experiment. The major results include the first
  statistically significant uniform sample of GCR actinides with
  35 events passing quality cuts, evidence for the existence of
  transuranic nuclei in the GCR with one <SUB>96</SUB>Cm candidate
  event, and a low <SUB>82</SUB>Pb/<SUB>78</SUB>Pt ratio consistent
  with other experiments. The probability of the existence of a
  transuranic component is estimated as 96%, while the most likely
  <SUB>92</SUB>U/<SUB>90</SUB>Th ratio is found to be 0.4 within a wide
  70% confidence interval ranging from 0 to 0.96. Overall, the results are
  consistent with a volatility-based acceleration bias and source material
  which is mainly ordinary interstellar medium material with some recent
  contamination by freshly synthesized material. Uncertainty in the key
  <SUB>92</SUB>U/<SUB>90</SUB>Th ratio is dominated by statistical errors
  resulting from the small sample size and any improved determination
  will thus require an experiment with a substantially larger exposure
  factor than the UHCRE.

Title: Magnetic field emergence in mesogranular-sized exploding
    granules observed with sunrise/IMaX data
Authors: Palacios, J.; Blanco Rodríguez, J.; Vargas Domínguez, S.;
   Domingo, V.; Martínez Pillet, V.; Bonet, J. A.; Bellot Rubio, L. R.;
   Del Toro Iniesta, J. C.; Solanki, S. K.; Barthol, P.; Gandorfer, A.;
   Berkefeld, T.; Schmidt, W.; Knölker, M.
Bibcode: 2012A&A...537A..21P
Altcode: 2011arXiv1110.4555P
  We report on magnetic field emergences covering significant
  areas of exploding granules. The balloon-borne mission Sunrise
  provided high spatial and temporal resolution images of the solar
  photosphere. Continuum images, longitudinal and transverse magnetic
  field maps and Dopplergrams obtained by IMaX onboard Sunrise are
  analyzed by local correlation traking (LCT), divergence calculation
  and time slices, Stokes inversions and numerical simulations are also
  employed. We characterize two mesogranular-scale exploding granules
  where ~10<SUP>18</SUP> Mx of magnetic flux emerges. The emergence
  of weak unipolar longitudinal fields (~100 G) start with a single
  visible magnetic polarity, occupying their respective granules' top
  and following the granular splitting. After a while, mixed polarities
  start appearing, concentrated in downflow lanes. The events last around
  20 min. LCT analyses confirm mesogranular scale expansion, displaying
  a similar pattern for all the physical properties, and divergence
  centers match between all of them. We found a similar behaviour
  with the emergence events in a numerical MHD simulation. Granule
  expansion velocities are around 1 kms<SUP>-1</SUP> while magnetic
  patches expand at 0.65 kms<SUP>-1</SUP>. One of the analyzed events
  evidences the emergence of a loop-like structure. Advection of
  the emerging magnetic flux features is dominated by convective
  motion resulting from the exploding granule due to the magnetic
  field frozen in the granular plasma. Intensification of the
  magnetic field occurs in the intergranular lanes, probably
  because of being directed by the downflowing plasma. <P />Movies
  associated to Figs. 2-4 are available in electronic form at <A
  href="http://www.aanda.org">http://www.aanda.org</A>

Title: Spatial distribution and statistical properties of small-scale
    convective vortex-like motions in a quiet-Sun region
Authors: Vargas Domínguez, S.; Palacios, J.; Balmaceda, L.; Cabello,
   I.; Domingo, V.
Bibcode: 2011MNRAS.416..148V
Altcode: 2011MNRAS.tmp.1046V; 2011arXiv1105.3092V
  High-resolution observations of a quiet-Sun internetwork region taken
  with the Solar 1-m Swedish Telescope in La Palma are analysed. We
  determine the location of small-scale vortex motions in the solar
  photospheric region by computing the horizontal proper motions
  of small-scale structures on time-series of images. These plasma
  convectively driven swirl motions are associated to (1) downdrafts
  (that have been commonly explained as corresponding to sites where
  the plasma is cooled down and hence returned to the interior below
  the visible photospheric level) and (2) horizontal velocity vectors
  converging on a central point. The sink cores are proved to be the final
  destination of passive floats tracing plasma flows towards the centre
  of each vortex. We establish the occurrence of these events to be 1.4
  × 10<SUP>-3</SUP> and 1.6 × 10<SUP>-3</SUP> vortices Mm<SUP>-2</SUP>
  min<SUP>-1</SUP>, respectively, for the two time-series analysed here.

Title: The Sun at high resolution: first results from the Sunrise
    mission
Authors: Solanki, S. K.; Barthol, P.; Danilovic, S.; Feller,
   A.; Gandorfer, A.; Hirzberger, J.; Lagg, A.; Riethmüller, T. L.;
   Schüssler, M.; Wiegelmann, T.; Bonet, J. A.; Pillet, V. Martínez;
   Khomenko, E.; del Toro Iniesta, J. C.; Domingo, V.; Palacios, J.;
   Knölker, M.; González, N. Bello; Borrero, J. M.; Berkefeld, T.;
   Franz, M.; Roth, M.; Schmidt, W.; Steiner, O.; Title, A. M.
Bibcode: 2011IAUS..273..226S
Altcode:
  The Sunrise balloon-borne solar observatory consists of a 1m aperture
  Gregory telescope, a UV filter imager, an imaging vector polarimeter,
  an image stabilization system and further infrastructure. The first
  science flight of Sunrise yielded high-quality data that reveal the
  structure, dynamics and evolution of solar convection, oscillations
  and magnetic fields at a resolution of around 100 km in the quiet
  Sun. Here we describe very briefly the mission and the first results
  obtained from the Sunrise data, which include a number of discoveries.

Title: The Imaging Magnetograph eXperiment (IMaX) for the Sunrise
    Balloon-Borne Solar Observatory
Authors: Martínez Pillet, V.; del Toro Iniesta, J. C.;
   Álvarez-Herrero, A.; Domingo, V.; Bonet, J. A.; González Fernández,
   L.; López Jiménez, A.; Pastor, C.; Gasent Blesa, J. L.; Mellado, P.;
   Piqueras, J.; Aparicio, B.; Balaguer, M.; Ballesteros, E.; Belenguer,
   T.; Bellot Rubio, L. R.; Berkefeld, T.; Collados, M.; Deutsch, W.;
   Feller, A.; Girela, F.; Grauf, B.; Heredero, R. L.; Herranz, M.;
   Jerónimo, J. M.; Laguna, H.; Meller, R.; Menéndez, M.; Morales, R.;
   Orozco Suárez, D.; Ramos, G.; Reina, M.; Ramos, J. L.; Rodríguez,
   P.; Sánchez, A.; Uribe-Patarroyo, N.; Barthol, P.; Gandorfer, A.;
   Knoelker, M.; Schmidt, W.; Solanki, S. K.; Vargas Domínguez, S.
Bibcode: 2011SoPh..268...57M
Altcode: 2010SoPh..tmp..181M; 2010arXiv1009.1095M
  The Imaging Magnetograph eXperiment (IMaX) is a spectropolarimeter
  built by four institutions in Spain that flew on board the Sunrise
  balloon-borne solar observatory in June 2009 for almost six days over
  the Arctic Circle. As a polarimeter, IMaX uses fast polarization
  modulation (based on the use of two liquid crystal retarders),
  real-time image accumulation, and dual-beam polarimetry to reach
  polarization sensitivities of 0.1%. As a spectrograph, the instrument
  uses a LiNbO<SUB>3</SUB> etalon in double pass and a narrow band
  pre-filter to achieve a spectral resolution of 85 mÅ. IMaX uses the
  high-Zeeman-sensitive line of Fe I at 5250.2 Å and observes all four
  Stokes parameters at various points inside the spectral line. This
  allows vector magnetograms, Dopplergrams, and intensity frames to be
  produced that, after reconstruction, reach spatial resolutions in the
  0.15 - 0.18 arcsec range over a 50×50 arcsec field of view. Time
  cadences vary between 10 and 33 s, although the shortest one only
  includes longitudinal polarimetry. The spectral line is sampled in
  various ways depending on the applied observing mode, from just two
  points inside the line to 11 of them. All observing modes include
  one extra wavelength point in the nearby continuum. Gauss equivalent
  sensitivities are 4 G for longitudinal fields and 80 G for transverse
  fields per wavelength sample. The line-of-sight velocities are estimated
  with statistical errors of the order of 5 - 40 m s<SUP>−1</SUP>. The
  design, calibration, and integration phases of the instrument,
  together with the implemented data reduction scheme, are described in
  some detail.

Title: The Sunrise Mission
Authors: Barthol, P.; Gandorfer, A.; Solanki, S. K.; Schüssler,
   M.; Chares, B.; Curdt, W.; Deutsch, W.; Feller, A.; Germerott, D.;
   Grauf, B.; Heerlein, K.; Hirzberger, J.; Kolleck, M.; Meller, R.;
   Müller, R.; Riethmüller, T. L.; Tomasch, G.; Knölker, M.; Lites,
   B. W.; Card, G.; Elmore, D.; Fox, J.; Lecinski, A.; Nelson, P.;
   Summers, R.; Watt, A.; Martínez Pillet, V.; Bonet, J. A.; Schmidt,
   W.; Berkefeld, T.; Title, A. M.; Domingo, V.; Gasent Blesa, J. L.;
   del Toro Iniesta, J. C.; López Jiménez, A.; Álvarez-Herrero, A.;
   Sabau-Graziati, L.; Widani, C.; Haberler, P.; Härtel, K.; Kampf,
   D.; Levin, T.; Pérez Grande, I.; Sanz-Andrés, A.; Schmidt, E.
Bibcode: 2011SoPh..268....1B
Altcode: 2010arXiv1009.2689B; 2010SoPh..tmp..224B
  The first science flight of the balloon-borne Sunrise telescope took
  place in June 2009 from ESRANGE (near Kiruna/Sweden) to Somerset
  Island in northern Canada. We describe the scientific aims and
  mission concept of the project and give an overview and a description
  of the various hardware components: the 1-m main telescope with its
  postfocus science instruments (the UV filter imager SuFI and the imaging
  vector magnetograph IMaX) and support instruments (image stabilizing
  and light distribution system ISLiD and correlating wavefront sensor
  CWS), the optomechanical support structure and the instrument mounting
  concept, the gondola structure and the power, pointing, and telemetry
  systems, and the general electronics architecture. We also explain
  the optimization of the structural and thermal design of the complete
  payload. The preparations for the science flight are described,
  including AIV and ground calibration of the instruments. The course
  of events during the science flight is outlined, up to the recovery
  activities. Finally, the in-flight performance of the instrumentation
  is discussed.

Title: SUNRISE: Instrument, Mission, Data, and First Results
Authors: Solanki, S. K.; Barthol, P.; Danilovic, S.; Feller, A.;
   Gandorfer, A.; Hirzberger, J.; Riethmüller, T. L.; Schüssler, M.;
   Bonet, J. A.; Martínez Pillet, V.; del Toro Iniesta, J. C.; Domingo,
   V.; Palacios, J.; Knölker, M.; Bello González, N.; Berkefeld, T.;
   Franz, M.; Schmidt, W.; Title, A. M.
Bibcode: 2010ApJ...723L.127S
Altcode: 2010arXiv1008.3460S
  The SUNRISE balloon-borne solar observatory consists of a 1 m aperture
  Gregory telescope, a UV filter imager, an imaging vector polarimeter,
  an image stabilization system, and further infrastructure. The first
  science flight of SUNRISE yielded high-quality data that revealed the
  structure, dynamics, and evolution of solar convection, oscillations,
  and magnetic fields at a resolution of around 100 km in the quiet
  Sun. After a brief description of instruments and data, the first
  qualitative results are presented. In contrast to earlier observations,
  we clearly see granulation at 214 nm. Images in Ca II H display narrow,
  short-lived dark intergranular lanes between the bright edges of
  granules. The very small-scale, mixed-polarity internetwork fields
  are found to be highly dynamic. A significant increase in detectable
  magnetic flux is found after phase-diversity-related reconstruction
  of polarization maps, indicating that the polarities are mixed right
  down to the spatial resolution limit and probably beyond.

Title: Supersonic Magnetic Upflows in Granular Cells Observed with
    SUNRISE/IMAX
Authors: Borrero, J. M.; Martínez-Pillet, V.; Schlichenmaier, R.;
   Solanki, S. K.; Bonet, J. A.; del Toro Iniesta, J. C.; Schmidt, W.;
   Barthol, P.; Gandorfer, A.; Domingo, V.; Knölker, M.
Bibcode: 2010ApJ...723L.144B
Altcode: 2010arXiv1009.1227B
  Using the IMaX instrument on board the SUNRISE stratospheric balloon
  telescope, we have detected extremely shifted polarization signals
  around the Fe I 5250.217 Å spectral line within granules in the solar
  photosphere. We interpret the velocities associated with these events
  as corresponding to supersonic and magnetic upflows. In addition, they
  are also related to the appearance of opposite polarities and highly
  inclined magnetic fields. This suggests that they are produced by the
  reconnection of emerging magnetic loops through granular upflows. The
  events occupy an average area of 0.046 arcsec<SUP>2</SUP> and last for
  about 80 s, with larger events having longer lifetimes. These supersonic
  events occur at a rate of 1.3 × 10<SUP>-5</SUP> occurrences per second
  per arcsec<SUP>2</SUP>.

Title: Detection of Vortex Tubes in Solar Granulation from
    Observations with SUNRISE
Authors: Steiner, O.; Franz, M.; Bello González, N.; Nutto, Ch.;
   Rezaei, R.; Martínez Pillet, V.; Bonet Navarro, J. A.; del Toro
   Iniesta, J. C.; Domingo, V.; Solanki, S. K.; Knölker, M.; Schmidt,
   W.; Barthol, P.; Gandorfer, A.
Bibcode: 2010ApJ...723L.180S
Altcode: 2010arXiv1009.4723S
  We have investigated a time series of continuum intensity maps and
  corresponding Dopplergrams of granulation in a very quiet solar region
  at the disk center, recorded with the Imaging Magnetograph eXperiment
  (IMaX) on board the balloon-borne solar observatory SUNRISE. We
  find that granules frequently show substructure in the form of lanes
  composed of a leading bright rim and a trailing dark edge, which move
  together from the boundary of a granule into the granule itself. We
  find strikingly similar events in synthesized intensity maps from an
  ab initio numerical simulation of solar surface convection. From cross
  sections through the computational domain of the simulation, we conclude
  that these granular lanes are the visible signature of (horizontally
  oriented) vortex tubes. The characteristic optical appearance of vortex
  tubes at the solar surface is explained. We propose that the observed
  vortex tubes may represent only the large-scale end of a hierarchy of
  vortex tubes existing near the solar surface.

Title: Where the Granular Flows Bend
Authors: Khomenko, E.; Martínez Pillet, V.; Solanki, S. K.; del Toro
   Iniesta, J. C.; Gandorfer, A.; Bonet, J. A.; Domingo, V.; Schmidt,
   W.; Barthol, P.; Knölker, M.
Bibcode: 2010ApJ...723L.159K
Altcode: 2010arXiv1008.0517K
  Based on IMaX/SUNRISE data, we report on a previously undetected
  phenomenon in solar granulation. We show that in a very narrow region
  separating granules and intergranular lanes, the spectral line width
  of the Fe I 5250.2 Å line becomes extremely small. We offer an
  explanation of this observation with the help of magneto-convection
  simulations. These regions with extremely small line widths correspond
  to the places where the granular flows bend from upflow in granules
  to downflow in intergranular lanes. We show that the resolution and
  image stability achieved by IMaX/SUNRISE are important requisites to
  detect this interesting phenomenon.

Title: Bright Points in the Quiet Sun as Observed in the Visible
    and Near-UV by the Balloon-borne Observatory SUNRISE
Authors: Riethmüller, T. L.; Solanki, S. K.; Martínez Pillet, V.;
   Hirzberger, J.; Feller, A.; Bonet, J. A.; Bello González, N.; Franz,
   M.; Schüssler, M.; Barthol, P.; Berkefeld, T.; del Toro Iniesta,
   J. C.; Domingo, V.; Gandorfer, A.; Knölker, M.; Schmidt, W.
Bibcode: 2010ApJ...723L.169R
Altcode: 2010arXiv1009.1693R
  Bright points (BPs) are manifestations of small magnetic elements
  in the solar photosphere. Their brightness contrast not only gives
  insight into the thermal state of the photosphere (and chromosphere) in
  magnetic elements, but also plays an important role in modulating the
  solar total and spectral irradiance. Here, we report on simultaneous
  high-resolution imaging and spectropolarimetric observations of
  BPs using SUNRISE balloon-borne observatory data of the quiet Sun
  at the disk center. BP contrasts have been measured between 214 nm
  and 525 nm, including the first measurements at wavelengths below
  388 nm. The histograms of the BP peak brightness show a clear trend
  toward broader contrast distributions and higher mean contrasts at
  shorter wavelengths. At 214 nm, we observe a peak brightness of up to
  five times the mean quiet-Sun value, the highest BP contrast so far
  observed. All BPs are associated with a magnetic signal, although in
  a number of cases it is surprisingly weak. Most of the BPs show only
  weak downflows, the mean value being 240 m s<SUP>-1</SUP>, but some
  display strong down- or upflows reaching a few km s<SUP>-1</SUP>.

Title: Transverse Component of the Magnetic Field in the Solar
    Photosphere Observed by SUNRISE
Authors: Danilovic, S.; Beeck, B.; Pietarila, A.; Schüssler, M.;
   Solanki, S. K.; Martínez Pillet, V.; Bonet, J. A.; del Toro Iniesta,
   J. C.; Domingo, V.; Barthol, P.; Berkefeld, T.; Gandorfer, A.;
   Knölker, M.; Schmidt, W.; Title, A. M.
Bibcode: 2010ApJ...723L.149D
Altcode: 2010arXiv1008.1535D
  We present the first observations of the transverse component of
  a photospheric magnetic field acquired by the imaging magnetograph
  SUNRISE/IMaX. Using an automated detection method, we obtain statistical
  properties of 4536 features with significant linear polarization
  signal. We obtain a rate of occurrence of 7 × 10<SUP>-4</SUP>
  s<SUP>-1</SUP> arcsec<SUP>-2</SUP>, which is 1-2 orders of magnitude
  larger than the values reported by previous studies. We show that
  these features have no characteristic size or lifetime. They appear
  preferentially at granule boundaries with most of them being caught
  in downflow lanes at some point. Only a small percentage are entirely
  and constantly embedded in upflows (16%) or downflows (8%).

Title: Detection of Large Acoustic Energy Flux in the Solar Atmosphere
Authors: Bello González, N.; Franz, M.; Martínez Pillet, V.; Bonet,
   J. A.; Solanki, S. K.; del Toro Iniesta, J. C.; Schmidt, W.; Gandorfer,
   A.; Domingo, V.; Barthol, P.; Berkefeld, T.; Knölker, M.
Bibcode: 2010ApJ...723L.134B
Altcode: 2010arXiv1009.4795B
  We study the energy flux carried by acoustic waves excited by convective
  motions at sub-photospheric levels. The analysis of high-resolution
  spectropolarimetric data taken with IMaX/SUNRISE provides a total
  energy flux of ~6400-7700 W m<SUP>-2</SUP> at a height of ~250 km
  in the 5.2-10 mHz range, i.e., at least twice the largest energy
  flux found in previous works. Our estimate lies within a factor of
  two of the energy flux needed to balance radiative losses from the
  chromosphere according to the estimates of Anderson &amp; Athay and
  revives interest in acoustic waves for transporting energy to the
  chromosphere. The acoustic flux is mainly found in the intergranular
  lanes but also in small rapidly evolving granules and at the bright
  borders, forming dark dots and lanes of splitting granules.

Title: Magnetic Loops in the Quiet Sun
Authors: Wiegelmann, T.; Solanki, S. K.; Borrero, J. M.; Martínez
   Pillet, V.; del Toro Iniesta, J. C.; Domingo, V.; Bonet, J. A.;
   Barthol, P.; Gandorfer, A.; Knölker, M.; Schmidt, W.; Title, A. M.
Bibcode: 2010ApJ...723L.185W
Altcode: 2010arXiv1009.4715W
  We investigate the fine structure of magnetic fields in the atmosphere
  of the quiet Sun. We use photospheric magnetic field measurements from
  SUNRISE/IMaX with unprecedented spatial resolution to extrapolate
  the photospheric magnetic field into higher layers of the solar
  atmosphere with the help of potential and force-free extrapolation
  techniques. We find that most magnetic loops that reach into the
  chromosphere or higher have one footpoint in relatively strong magnetic
  field regions in the photosphere. Ninety-one percent of the magnetic
  energy in the mid-chromosphere (at a height of 1 Mm) is in field
  lines, whose stronger footpoint has a strength of more than 300 G,
  i.e., above the equipartition field strength with convection. The
  loops reaching into the chromosphere and corona are also found to be
  asymmetric in the sense that the weaker footpoint has a strength B &lt;
  300 G and is located in the internetwork (IN). Such loops are expected
  to be strongly dynamic and have short lifetimes, as dictated by the
  properties of the IN fields.

Title: SUNRISE/IMaX Observations of Convectively Driven Vortex Flows
    in the Sun
Authors: Bonet, J. A.; Márquez, I.; Sánchez Almeida, J.; Palacios,
   J.; Martínez Pillet, V.; Solanki, S. K.; del Toro Iniesta, J. C.;
   Domingo, V.; Berkefeld, T.; Schmidt, W.; Gandorfer, A.; Barthol, P.;
   Knölker, M.
Bibcode: 2010ApJ...723L.139B
Altcode: 2010arXiv1009.1992B
  We characterize the observational properties of the convectively driven
  vortex flows recently discovered on the quiet Sun, using magnetograms,
  Dopplergrams, and images obtained with the 1 m balloon-borne SUNRISE
  telescope. By visual inspection of time series, we find some 3.1
  × 10<SUP>-3</SUP> vortices Mm<SUP>-2</SUP> minute<SUP>-1</SUP>,
  which is a factor of ~1.7 larger than previous estimates. The mean
  duration of the individual events turns out to be 7.9 minutes, with
  a standard deviation of 3.2 minutes. In addition, we find several
  events appearing at the same locations along the duration of the time
  series (31.6 minutes). Such recurrent vortices show up in the proper
  motion flow field map averaged over the time series. The typical
  vertical vorticities are lsim6 × 10<SUP>-3</SUP> s<SUP>-1</SUP>,
  which corresponds to a period of rotation of some 35 minutes. The
  vortices show a preferred counterclockwise sense of rotation, which
  we conjecture may have to do with the preferred vorticity impinged by
  the solar differential rotation.

Title: Surface Waves in Solar Granulation Observed with SUNRISE
Authors: Roth, M.; Franz, M.; Bello González, N.; Martínez Pillet,
   V.; Bonet, J. A.; Gandorfer, A.; Barthol, P.; Solanki, S. K.;
   Berkefeld, T.; Schmidt, W.; del Toro Iniesta, J. C.; Domingo, V.;
   Knölker, M.
Bibcode: 2010ApJ...723L.175R
Altcode: 2010arXiv1009.4790R
  Solar oscillations are expected to be excited by turbulent flows in
  the intergranular lanes near the solar surface. Time series recorded
  by the IMaX instrument on board the SUNRISE observatory reveal solar
  oscillations at high spatial resolution, which allow the study of
  the properties of oscillations with short wavelengths. We analyze
  two time series with synchronous recordings of Doppler velocity and
  continuum intensity images with durations of 32 minutes and 23 minutes,
  respectively, recorded close to the disk center of the Sun to study
  the propagation and excitation of solar acoustic oscillations. In
  the Doppler velocity data, both the standing acoustic waves and the
  short-lived, high-degree running waves are visible. The standing
  waves are visible as temporary enhancements of the amplitudes of the
  large-scale velocity field due to the stochastic superposition of
  the acoustic waves. We focus on the high-degree small-scale waves by
  suitable filtering in the Fourier domain. Investigating the propagation
  and excitation of f- and p <SUB>1</SUB>-modes with wavenumbers k&gt;1.4
  Mm<SUP>-1</SUP>, we also find that exploding granules contribute to
  the excitation of solar p-modes in addition to the contribution of
  intergranular lanes.

Title: Fully Resolved Quiet-Sun Magnetic flux Tube Observed with
    the SUNRISE/IMAX Instrument
Authors: Lagg, A.; Solanki, S. K.; Riethmüller, T. L.; Martínez
   Pillet, V.; Schüssler, M.; Hirzberger, J.; Feller, A.; Borrero,
   J. M.; Schmidt, W.; del Toro Iniesta, J. C.; Bonet, J. A.; Barthol, P.;
   Berkefeld, T.; Domingo, V.; Gandorfer, A.; Knölker, M.; Title, A. M.
Bibcode: 2010ApJ...723L.164L
Altcode: 2010arXiv1009.0996L
  Until today, the small size of magnetic elements in quiet-Sun areas has
  required the application of indirect methods, such as the line-ratio
  technique or multi-component inversions, to infer their physical
  properties. A consistent match to the observed Stokes profiles could
  only be obtained by introducing a magnetic filling factor that specifies
  the fraction of the observed pixel filled with magnetic field. Here,
  we investigate the properties of a small magnetic patch in the quiet
  Sun observed with the IMaX magnetograph on board the balloon-borne
  telescope SUNRISE with unprecedented spatial resolution and low
  instrumental stray light. We apply an inversion technique based on
  the numerical solution of the radiative transfer equation to retrieve
  the temperature stratification and the field strength in the magnetic
  patch. The observations can be well reproduced with a one-component,
  fully magnetized atmosphere with a field strength exceeding 1 kG and
  a significantly enhanced temperature in the mid to upper photosphere
  with respect to its surroundings, consistent with semi-empirical flux
  tube models for plage regions. We therefore conclude that, within the
  framework of a simple atmospheric model, the IMaX measurements resolve
  the observed quiet-Sun flux tube.

Title: The IMaX polarimeter for the solar telescope SUNRISE of the
    NASA long duration balloon program
Authors: Alvarez-Herrero, A.; Martínez-Pillet, V.; Del Toro Iniesta,
   J. C.; Domingo, V.
Bibcode: 2010EPJWC...505002A
Altcode:
  On June 8th 2009 the SUNRISE mission was successfully launched. This
  mission consisted of a 1m aperture solar telescope on board of a
  stratospheric balloon within the Long Duration Balloon NASA program. The
  flight followed the foreseen circumpolar trajectory over the Artic
  and the duration was 5 days and 17 hours. One of the two postfocal
  instruments onboard was IMaX, the Imaging Magnetograph eXperiment. This
  instrument is a solar magnetograph which is a diffraction limited imager
  capable to resolve 100 km on the solar surface, and simultaneously
  a high sensitivity polarimeter (&lt;10<SUP>-3</SUP>) and a high
  resolution spectrograph (bandwidth &lt;70mÅ). The magnetic vectorial
  map can be extracted thanks to the well-know Zeeman effect, which takes
  place in the solar atoms, allowing to relate polarization and spectral
  measurements to magnetic fields. The technological challenge of the IMaX
  development has a special relevance due to the utilization of innovative
  technologies in the Aeroespacial field and it is an important precedent
  for future space missions such as Solar Orbiter from ESA. Among these
  novel technologies the utilization of Liquid Crystal Variable Retarders
  (LCVRs) as polarization modulators and a LiNbO<SUB>3</SUB> etalon as
  tunable spectral filter are remarkable. Currently the data obtained
  is being analyzed and the preliminary results show unprecedented
  information about the solar dynamics.

Title: Evidence of small-scale magnetic concentrations dragged by
    vortex motion of solar photospheric plasma
Authors: Balmaceda, L.; Vargas Domínguez, S.; Palacios, J.; Cabello,
   I.; Domingo, V.
Bibcode: 2010A&A...513L...6B
Altcode: 2010arXiv1004.1185B
  Vortex-type motions have been measured by tracking bright points in
  high-resolution observations of the solar photosphere. These small-scale
  motions are thought to be determinant in the evolution of magnetic
  footpoints and their interaction with plasma and therefore likely to
  play a role in heating the upper solar atmosphere by twisting magnetic
  flux tubes. We report the observation of magnetic concentrations being
  dragged towards the center of a convective vortex motion in the solar
  photosphere from high-resolution ground-based and space-borne data. We
  describe this event by analyzing a series of images at different solar
  atmospheric layers. By computing horizontal proper motions, we detect a
  vortex whose center appears to be the draining point for the magnetic
  concentrations detected in magnetograms and well-correlated with the
  locations of bright points seen in G-band and CN images.

Title: Observations of Magnetic Elements in the Quiet Sun Internetwork
Authors: Balmaceda, L. A.; Palacios, J.; Cabello, I.; Domingo, V.
Bibcode: 2009ASPC..415..156B
Altcode:
  We present here the analysis of high-resolution images of the quiet Sun
  at disk center taken with the Solar Optical Telescope (SOT) on board
  Hinode in the CN bandhead (388.35 nm) and magnetograms in the Mg I line
  (517.27 nm). These observations are complemented with data from the
  Swedish 1m Solar Telescope (SST). All data sets were obtained during
  the Hinode/Canary Islands joint campaign (HOP 0014) in September,
  2007. In particular, we investigate the morphology, radiative and
  magnetic properties of small-scale elements in the solar atmosphere.

Title: Solar Surface Magnetism and Irradiance on Time Scales from
    Days to the 11-Year Cycle
Authors: Domingo, V.; Ermolli, I.; Fox, P.; Fröhlich, C.; Haberreiter,
   M.; Krivova, N.; Kopp, G.; Schmutz, W.; Solanki, S. K.; Spruit, H. C.;
   Unruh, Y.; Vögler, A.
Bibcode: 2009SSRv..145..337D
Altcode:
  The uninterrupted measurement of the total solar irradiance during the
  last three solar cycles and an increasing amount of solar spectral
  irradiance measurements as well as solar imaging observations
  (magnetograms and photometric data) have stimulated the development
  of models attributing irradiance variations to solar surface
  magnetism. Here we review the current status of solar irradiance
  measurements and modelling efforts based on solar photospheric
  magnetic fields. Thereby we restrict ourselves to the study of solar
  variations from days to the solar cycle. Phenomenological models
  of the solar atmosphere in combination with imaging observations of
  solar electromagnetic radiation and measurements of the photospheric
  magnetic field have reached high enough quality to show that a large
  fraction (at least, about 80%) of the solar irradiance variability
  can be explained by the radiative effects of the magnetic activity
  present in the photosphere. Also, significant progress has been made
  with magnetohydrodynamic simulations of convection that allow us to
  relate the radiance of the photospheric magnetic structures to the
  observations.

Title: Convectively Driven Vortex Flows in the Sun
Authors: Bonet, J. A.; Márquez, I.; Sánchez Almeida, J.; Cabello,
   I.; Domingo, V.
Bibcode: 2008ApJ...687L.131B
Altcode: 2008arXiv0809.3885B
  We have discovered small whirlpools in the Sun, with a size similar to
  terrestrial hurricanes (lesssim0.5 Mm). The theory of solar convection
  predicts them, but they had remained elusive so far. The vortex flows
  are created at the downdrafts where the plasma returns to the solar
  interior after cooling down, and we detect them because some magnetic
  bright points (BPs) follow a logarithmic spiral on their way to being
  engulfed by a downdraft. Our disk-center observations show 0.9 ×
  10<SUP>-2</SUP> vortexes per Mm<SUP>2</SUP>, with a lifetime of the
  order of 5 minutes, and with no preferred sense of rotation. They are
  not evenly spread out over the surface, but they seem to trace the
  supergranulation and the mesogranulation. These observed properties are
  strongly biased by our type of measurement, unable to detect vortexes
  except when they are engulfing magnetic BPs.

Title: Convectively driven vortex flows in the Sun
Authors: Bonet, J. A.; Márquez, I.; Sánchez Almeida, J.; Cabello,
   I.; Domingo, V.
Bibcode: 2008iac..talk..143B
Altcode: 2008iac..talk...26B
  No abstract at ADS

Title: Small magnetic structures in the photosphere, radiative
    properties
Authors: Palacios, Judith; Domingo, Vicente; Cabello, Iballa; Bonet,
   José Antonio; Sánchez Almeida, Jorge
Bibcode: 2008cosp...37.2331P
Altcode: 2008cosp.meet.2331P
  The three dimensional structure of small magnetic field features in the
  photosphere, their dynamic behavior and their radiative properties are
  studied. We analyze data obtained in simultaneous observations made on
  Sept 29 and 30, 2007 with the HINODE spacecraft and the Swedish Solar
  Telescope (SST) in La Palma in different wavelengths, such as CaII
  (396.85 nm) and CN (388.35 nm) and other with Hinode data; and Gband
  (430.56 nm) with SST. Tha analysis is completed with high resolution
  Gband and Gcontinuum (436.39 nm) images from SST obtained on 2005 and
  2006. Magnetograms have been obtained from both observatories. SST
  images have been processed with MOMFB code. Ribbon-like structures and
  "flowers" are studied in detail. Comparisons with solar atmospheric
  models are presented.

Title: The DynaMICS perspective
Authors: Turck-Chièze, S.; Schmutz, W.; Thuillier, G.; Jefferies,
   S.; Pallé; Dewitt, S.; Ballot, J.; Berthomieu, G.; Bonanno, A.;
   Brun, A. S.; Christensen-Dalsgaard, J.; Corbard, T.; Couvidat, S.;
   Darwich, A. M.; Dintrans, B.; Domingo, V.; Finsterle, W.; Fossat,
   E.; Garcia, R. A.; Gelly, B.; Gough, D.; Guzik, J.; Jiménez, A. J.;
   Jiménez-Reyes, S.; Kosovichev, A.; Lambert, P.; Lefebvre, S.; Lopes,
   I.; Martic, M.; Mathis, S.; Mathur, S.; Nghiem, P. A. P.; Piau, L.;
   Provost, J.; Rieutord, M.; Robillot, J. M.; Rogers, T.; Roudier, T.;
   Roxburgh, I.; Rozelot, J. P.; Straka, C.; Talon, S.; Théado, S.;
   Thompson, M.; Vauclair, S.; Zahn, J. P.
Bibcode: 2006ESASP.624E..24T
Altcode: 2006soho...18E..24T
  No abstract at ADS

Title: Scientific Objectives of the Novel Formation Flying Mission
    Aspiics
Authors: Turck-Chièze, S.; Schmutz, W.; Thuillier, G.; Jefferies,
   S.; Pallé; Dewitt, S.; Ballot, J.; Berthomieu, G.; Bonanno, A.;
   Brun, A. S.; Christensen-Dalsgaard, J.; Corbard, T.; Couvidat, S.;
   Darwich, A. M.; Dintrans, B.; Domingo, V.; Finsterle, W.; Fossat,
   E.; Garcia, R. A.; Gelly, B.; Gough, D.; Guzik, J.; Jiménez, A. J.;
   Jiménez-Reyes, S.; Kosovichev, A.; Lambert, P.; Lefebvre, S.; Lopes,
   I.; Martic, M.; Mathis, S.; Mathur, S.; Nghiem, P. A. P.; Piau, L.;
   Provost, J.; Rieutord, M.; Robillot, J. M.; Rogers, T.; Roudier, T.;
   Roxburgh, I.; Rozelot, J. P.; Straka, C.; Talon, S.; Théado, S.;
   Thompson, M.; Vauclair, S.; Zahn, J. P.
Bibcode: 2006ESASP.617E.164L
Altcode: 2006soho...17E.164L
  No abstract at ADS

Title: The EUV Variability Experiment (EVE) on the Solar Dynamics
Observatory (SDO): Science Plan and Instrument Overview
Authors: Turck-Chièze, S.; Schmutz, W.; Thuillier, G.; Jefferies,
   S.; Pallé; Dewitt, S.; Ballot, J.; Berthomieu, G.; Bonanno, A.;
   Brun, A. S.; Christensen-Dalsgaard, J.; Corbard, T.; Couvidat, S.;
   Darwich, A. M.; Dintrans, B.; Domingo, V.; Finsterle, W.; Fossat,
   E.; Garcia, R. A.; Gelly, B.; Gough, D.; Guzik, J.; Jiménez, A. J.;
   Jiménez-Reyes, S.; Kosovichev, A.; Lambert, P.; Lefebvre, S.; Lopes,
   I.; Martic, M.; Mathis, S.; Mathur, S.; Nghiem, P. A. P.; Piau, L.;
   Provost, J.; Rieutord, M.; Robillot, J. M.; Rogers, T.; Roudier, T.;
   Roxburgh, I.; Rozelot, J. P.; Straka, C.; Talon, S.; Théado, S.;
   Thompson, M.; Vauclair, S.; Zahn, J. P.
Bibcode: 2006ESASP.617E.165W
Altcode: 2006soho...17E.165W
  No abstract at ADS

Title: The Dynamics Project
Authors: Turck-Chièze, S.; Schmutz, W.; Thuillier, G.; Jefferies,
   S.; Pallé; Dewitt, S.; Ballot, J.; Berthomieu, G.; Bonanno, A.;
   Brun, A. S.; Christensen-Dalsgaard, J.; Corbard, T.; Couvidat, S.;
   Darwich, A. M.; Dintrans, B.; Domingo, V.; Finsterle, W.; Fossat,
   E.; Garcia, R. A.; Gelly, B.; Gough, D.; Guzik, J.; Jiménez, A. J.;
   Jiménez-Reyes, S.; Kosovichev, A.; Lambert, P.; Lefebvre, S.; Lopes,
   I.; Martic, M.; Mathis, S.; Mathur, S.; Nghiem, P. A. P.; Piau, L.;
   Provost, J.; Rieutord, M.; Robillot, J. M.; Rogers, T.; Roudier, T.;
   Roxburgh, I.; Rozelot, J. P.; Straka, C.; Talon, S.; Théado, S.;
   Thompson, M.; Vauclair, S.; Zahn, J. P.
Bibcode: 2006ESASP.617E.162T
Altcode: 2006soho...17E.162T
  No abstract at ADS

Title: Solar Photospheric Magnetic Elements Dimension and Radiance
Authors: Cabello, I.; Domingo, V.
Bibcode: 2006ESASP.617E..55C
Altcode: 2006soho...17E..55C
  No abstract at ADS

Title: Detailed design of the imaging magnetograph experiment (IMaX):
    a visible imager magnetograph for the Sunrise mission
Authors: Álvarez-Herrero, A.; Belenguer, T.; Pastor, C.; González,
   L.; Heredero, R. L.; Ramos, G.; Reina, M.; Sánchez, A.; Villanueva,
   J.; Sabau, L.; Martínez Pillet, V.; Bonet, J. A.; Collados, M.;
   Jochum, L.; Ballesteros, E.; Medina Trujillo, J. L.; Ruiz, Cobo B.;
   González, J. C.; del Toro Iniesta, J. C.; López Jiménez, A. C.;
   Castillo Lorenzo, J.; Herranz, M.; Jerónimo, J. M.; Mellado, P.;
   Morales, R.; Rodríguez, J.; Domingo, V.; Gasent, J. L.; Rodríquez, P.
Bibcode: 2006SPIE.6265E..4CA
Altcode: 2006SPIE.6265E.132A
  In this work, it is described the Imaging Magnetograph eXperiment,
  IMaX, one of the three postfocal instruments of the Sunrise mission. The
  Sunrise project consists on a stratospheric balloon with a 1 m aperture
  telescope, which will fly from the Antarctica within the NASA Long
  Duration Balloon Program. IMaX will provide vector magnetograms
  of the solar surface with a spatial resolution of 70 m. This data
  is relevant for understanding how the magnetic fields emerge in
  the solar surface, how they couple the photospheric base with the
  million degrees of temperature of the solar corona and which are the
  processes that are responsible of the generation of such an immense
  temperatures. To meet this goal IMaX should work as a high sensitivity
  polarimeter, high resolution spectrometer and a near diffraction
  limited imager. Liquid Crystal Variable Retarders will be used as
  polarization modulators taking advantage of the optical retardation
  induced by application of low electric fields and avoiding mechanical
  mechanisms. Therefore, the interest of these devices for aerospace
  applications is envisaged. The spectral resolution required will be
  achieved by using a LiNbO <SUB>3</SUB> Fabry-Perot etalon in double
  pass configuration as spectral filter before the two CCDs detectors. As
  well phase-diversity techniques will be implemented in order to improve
  the image quality. Nowadays, IMaX project is in the detailed design
  phase before fabrication, integration, assembly and verification. This
  paper briefly describes the current status of the instrument and the
  technical solutions developed to fulfil the scientific requirements.

Title: The intensity contrast of solar photospheric faculae and
    network elements. II. Evolution over the rising phase of solar
    cycle 23
Authors: Ortiz, A.; Domingo, V.; Sanahuja, B.
Bibcode: 2006A&A...452..311O
Altcode: 2006astro.ph..2556O
  We studied the radiative properties of small magnetic elements (active
  region faculae and the network) during the rising phase of solar cycle
  23 from 1996 to 2001, determining their contrasts as a function of
  heliocentric angle, magnetogram signal, and the solar cycle phase. We
  combined near-simultaneous full disk images of the line-of-sight
  magnetic field and photospheric continuum intensity provided by the
  MDI instrument on board the SOHO spacecraft. Sorting the magnetogram
  signal into different ranges allowed us to distinguish between the
  contrast of different magnetic structures. We find that the contrast
  center-to-limb variation (CLV) of these small magnetic elements is
  independent of time with a 10% precision, when measured during the
  rising phase of solar cycle 23. A 2-dimensional empirical expression
  for the contrast of photospheric features as a function of both the
  position on the disk and the averaged magnetic field strength was
  determined, showing its validity through the studied time period. A
  study of the relationship between magnetogram signal and the peak
  contrasts shows that the intrinsic contrast (maximum contrast per unit
  of magnetic flux) of network flux tubes is higher than that of active
  region faculae during the solar cycle.

Title: Centre-to-limb variation of photospheric facular radiance
    and image resolution
Authors: Domingo, Vicente; Ortiz, Ada; Sanahuja, Blai; Cabello, Iballa
Bibcode: 2005AdSpR..35..345D
Altcode:
  We study the effect of the angular resolution on the determination
  of the angular properties of the facular radiance. We analyze
  photospheric intensity in the continuum, around the Ni 676.8 nm line,
  and longitudinal magnetic field along the line of sight, measured by
  the MDI instrument aboard SOHO with two spatial resolutions, 4″ and
  1.2″ (2″ and 0.6″ pixels, respectively). The effect of the limited
  photometric sensitivity of the instrument and the limited information on
  the angular structure of the magnetic field tubes are considered. Our
  study of the high-resolution data shows that intensity contrast of
  magnetic features between 80 and 600 Gauss increases from centre to
  limb up to a maximum that occurs at higher heliocentric angles ( θ)
  when obtained with higher resolution data than for lower resolution
  data. There is a suggestion that at heliocentric angles below about
  75° there is only a monotonic increase in the contrast as one goes
  from cos ( θ) = 1 to cos ( θ) = 0.2.

Title: The imaging magnetograph eXperiment for the SUNRISE balloon
    Antarctica project
Authors: Martinez Pillet, Valentin; Bonet, Jose A.; Collados, Manuel
   V.; Jochum, Lieselotte; Mathew, S.; Medina Trujillo, J. L.; Ruiz Cobo,
   B.; del Toro Iniesta, Jose Carlos; Lopez Jimenez, A. C.; Castillo
   Lorenzo, J.; Herranz, M.; Jeronimo, J. M.; Mellado, P.; Morales, R.;
   Rodriguez, J.; Alvarez-Herrero, Alberto; Belenguer, Tomas; Heredero,
   R. L.; Menendez, M.; Ramos, G.; Reina, Manuel; Pastor, C.; Sanchez,
   A.; Villanueva, J.; Domingo, Vicente; Gasent, J. L.; Rodriguez, P.
Bibcode: 2004SPIE.5487.1152M
Altcode:
  The SUNRISE balloon project is a high-resolution mission to study solar
  magnetic fields able to resolve the critical scale of 100 km in the
  solar photosphere, or about one photon mean free path. The Imaging
  Magnetograph eXperiment (IMaX) is one of the three instruments that
  will fly in the balloon and will receive light from the 1m aperture
  telescope of the mission. IMaX should take advantage of the 15 days
  of uninterrupted solar observations and the exceptional resolution
  to help clarifying our understanding of the small-scale magnetic
  concentrations that pervade the solar surface. For this, IMaX should
  act as a diffraction limited imager able to carry out spectroscopic
  analysis with resolutions in the 50.000-100.000 range and capable
  to perform polarization measurements. The solutions adopted by the
  project to achieve all these three demanding goals are explained in this
  article. They include the use of Liquid Crystal Variable Retarders for
  the polarization modulation, one LiNbO<SUB>3</SUB> etalon in double pass
  and two modern CCD detectors that allow for the application of phase
  diversity techniques by slightly changing the focus of one of the CCDs.

Title: Excess facular emission from an isolated active region during
solar minimum: the example of NOAA AR 7978
Authors: Ortiz, A.; Domingo, V.; Sanahuja, B.; Fröhlich, C.
Bibcode: 2004JASTP..66...67O
Altcode: 2004JATP...66...67O
  The facular contribution to solar irradiance variations on the short
  time scale is studied by analyzing a simple case of an isolated active
  region that crossed the solar disk during the 1996 minimum of activity,
  NOAA AR 7978. Its passage during several Carrington rotations,
  specifically from rotation 1911 to 1916, allows us to analyze the
  evolution of the angular distribution of the excess radiance of
  the facular region using SOHO/VIRGO and MDI data. We associate this
  evolution with the evolution of the extent corresponding to the isolated
  active region as well as with the aging of the region itself. Finally,
  we evaluate the total (i.e. in all directions) emission of this facular
  region and its spectral and temporal evolution.

Title: Magnetic field tubes emerging in the photosphere
Authors: Domingo, V.; Marco, E.; Ortiz, A.; Sanahuja, B.
Bibcode: 2004cosp...35.4732D
Altcode: 2004cosp.meet.4732D
  Magnetic field tubes emerging in the photosphere are the dominant
  contributors to the solar irradiance variations with time. The knowledge
  of the radiative properties of the photospheric magnetic field elements
  is, therefore, of high interest to understand the solar irradiance. A
  classical way to quantify the angular distribution of their radiative
  properties is the measurement of the contrast between their radiance
  and the one from the surrounding photosphere as a function of
  their heliocentric angle location, known as centre-to-limb-variation
  (CLV). There are many published measurements of the CLV of photospheric
  small magnetic elements, mostly faculae, made in different conditions
  and giving different results. One of the parameters that may be
  different from one observation to another is the angular resolution. We
  study the effect of the angular resolution on the determination of
  the angular properties of the facular radiance, with measurements
  of photospheric intensity in the continuum, around the Fe 676.8 nm,
  and of the longitudinal magnetic field, along the line of sight,
  made with the MDI instrument aboard SOHO with two resolutions, 4 arc
  seconds and 1.2 arc seconds (2 and 0.6 arc second pixels, respectively)
  . The effect of the limited photometric sensitivity of the instrument
  and the limited information on the angular structure of the magnetic
  field tubes are considered.

Title: Contribution of the small photospheric magnetic elements to
    the long-term solar irradiance
Authors: Ortiz, Ada; Domingo, Vicente; Sanahuja, Blai
Bibcode: 2003ESASP.535...43O
Altcode: 2003iscs.symp...43O
  We used near-simultaneous full disk magnetograms and images of the
  photospheric continuum intensity provided by MDI/SOHO to analyze
  the long-term evolution of the intensity contrast of small magnetic
  features - faculae and magnetic network - as a function of position,
  magnetic signal and time, from minimum to maximum of cycle 23. We
  find that the spectral irradiance characteristics, at 676.8 nm, of
  the small photospheric magnetic elements are practically invariable
  throughout the rising phase of solar cycle 23. A preliminary statistical
  analysis of the magnetic field suggests that the small magnetic elements
  are likely to provide a significant contribution to the solar cycle
  irradiance change.

Title: IMax: a visible magnetograph for SUNRISE
Authors: Jochum, Lieselotte; Collados, Manuel; Martínez Pillet,
   Valentin; Bonet, Jose A.; del Toro Iniesta, Jose Carlos; Lopez,
   Antonio; Alvarez-Herrero, Alberto; Reina, Manuel; Fabregat, Juan;
   Domingo, Vicente
Bibcode: 2003SPIE.4843...20J
Altcode:
  The description of the Imaging Magnetograph eXperiment (IMaX) is
  presented in this contribution. This is a magnetograph which will
  fly by the end of 2006 on a stratospheric balloon, together with
  other instruments (to be described elsewhere). Especial emphasis
  is put on the scientific requirements to obtain diffraction-limited
  visible magnetograms, on the optical design and several constraining
  characteristics, such as the wavelength tuning or the crosstalk between
  the Stokes parameters.

Title: SOHO, Yohkoh, Ulysses and Trace: The four solar missions in
    perspective, and available resources
Authors: Domingo, V.
Bibcode: 2002Ap&SS.282..171D
Altcode:
  Four solar observing spacecraft, now in operation, have obtained and
  continue to obtain data during the late phase of solar cycle 22 and
  hopefully most of cycle 23. The data are available for scientific
  analysis, practically in an unrestricted manner. A large pool of
  software suited for the processing and to help programming any data
  analysis is freely available. An almost random list of results that
  are being obtained with this data is presented as an example of what
  can be done by analysing the data from these spacecraft, either alone
  or combining results among them, with ground observatories, or with
  other spacecraft, such as those that measure particles and fields
  in interplanetary space or in geospace, to study solar physics or
  solar-terrestrial relations.

Title: On the intensity contrast of solar photospheric faculae and
    network elements
Authors: Ortiz, A.; Solanki, S. K.; Domingo, V.; Fligge, M.;
   Sanahuja, B.
Bibcode: 2002A&A...388.1036O
Altcode: 2002astro.ph..7008O
  Sunspots, faculae and the magnetic network contribute to solar
  irradiance variations. The contribution due to faculae and the network
  is of basic importance, but suffers from considerable uncertainty. We
  determine the contrasts of active region faculae and the network,
  both as a function of heliocentric angle and magnetogram signal. To
  achieve this, we analyze near-simultaneous full disk images of
  photospheric continuum intensity and line-of-sight magnetic field
  provided by the Michelson Doppler Interferometer (MDI) on board
  the SOHO spacecraft. Starting from the surface distribution of
  the solar magnetic field we first construct a mask, which is then
  used to determine the brightness of magnetic features, and the
  relatively field-free part of the photosphere separately. By sorting
  the magnetogram signal into different bins we are able to distinguish
  between the contrasts of different concentrations of magnetic field. We
  find that the center-to-limb variation (CLV) of the contrast changes
  strongly with magnetogram signal. Thus, the contrasts of active region
  faculae (large magnetogram signal) and the network (small signal)
  exhibit a very different CLV, showing that the populations of magnetic
  flux tubes that underly the two kinds of features are different. The
  results are compatible with, on average, larger flux tubes in faculae
  than in the network. This implies that these elements need to be treated
  separately when reconstructing variations of the total solar irradiance
  with high precision. We have obtained an analytical expression for
  the contrast of photospheric magnetic features as a function of both
  position on the disk and spatially averaged magnetic field strength,
  by performing a 2-dimensional fit to the observations. We also provide
  a linear relationship between magnetogram signal and the mu =cos (theta
  ), where theta is the heliocentric angle, at which the contrast is
  maximal. Finally, we show that the maximum contrast per unit magnetic
  flux decreases rapidly with increasing magnetogram signal, supporting
  earlier evidence that the intrinsic contrast of magnetic flux tubes
  in the network is higher.

Title: Variation of the facular and network contrast during the
    rising phase of cycle 23
Authors: Ortiz, A.; Domingo, V.; Sanahuja, B.; Solanki, S. K.
Bibcode: 2002ESASP.508..185O
Altcode: 2002soho...11..185O
  Magnetic activity contributes to solar irradiance variations, both on
  short and long time-scales. While sunspots and active region faculae
  are the dominant contributors to irradiance changes on time-scales of
  days to weeks, the origin of the long-term increase of the irradiance
  between activity minimum and maximum (~0.1%) is still debated. It
  has been proposed that the small-scale magnetic elements composing the
  enhanced and quiet network contribute substantially to this increase. To
  contribute to this debate, we attempt to see if there is a change in
  the radiative properties of these elements along the solar cycle,
  and to evaluate such a change. We use near-simultaneous full disk
  magnetograms and images of the photospheric continuum intensity provided
  by MDI/SOHO. We have studied the center-to-limb variations (CLV) of the
  contrast as a function of magnetic strength and we are now analyzing how
  the noise level of the images changes throughout time, as a preliminary
  step towards an analysis of the temporal irradiance variations.

Title: A first step towards proton flux forecasting
Authors: Aran, A.; Sanahuja, B.; Lario, D.; Domingo, V.
Bibcode: 2002cosp...34E1078A
Altcode: 2002cosp.meetE1078A
  We present a preliminary version of a potential tool for real time
  proton flux prediction which provides proton flux profiles and
  cumulative fluence profiles at 0.5 MeV and 2 MeV of Solar Energetic
  Particle (SEP) events, from their onset up to the arrival of the
  interplanetary shock at the spacecraft position (located at 1 AU or
  0.4 AU). Based on the proton transport model by Lario et al. (1998) and
  the MHD shock propagation model of Wu et al. (1983), we have generated
  a database containing "synthetic" profiles of the proton fluxes and
  cumulative fluences of 384 SEP events. These events describe different
  interplanetary scenarios which comprise a set of various MHD-shocks
  and several heliolongitude locations of the solar activity sites, as
  well as different conditions for particle transport. We are currently
  validating the applicability of this code for space weather forecasting
  by comparing the resulting "synthetic" flux profiles with those of
  several real SEP events. References: Lario D., Sanahuja B. and Heras
  A.M., 1998, Astrophys. J., 509, 415 Wu S.T., Dryer M., Han S.M., 1983,
  Solar Physics, 84, 395

Title: Four years of SOHO discoveries - some highlights.
Authors: Fleck, B.; Brekke, P.; Haugan, S.; Duarte, L. S.; Domingo,
   V.; Gurman, J. B.; Poland, A. I.
Bibcode: 2000ESABu.102...68F
Altcode:
  Analysis of the helioseismic data from SOHO has shed new light on
  solar and heliosheric physics: the structure and dynamics of the
  solar interior, the heating and dynamics of the solar corona, and the
  acceleration and composition of the solar wind.

Title: An Example of Isolated Active Region Energy Evolution: NOAA
    AR 7978
Authors: Ortiz, A.; Domingo, V.; Sanahuja, B.; Sánchez, L.
Bibcode: 2000ESASP.463..395O
Altcode: 2000sctc.proc..395O
  The facular contribution to solar irradiance variations on the short
  time scale is studied by analysing a simple case of an isolated
  active region, NOAA AR7978, during the minimum of 1996. We focus on
  the relationship between the temporal evolution of the active region
  surface magnetic field, its physical characteristics and the total
  facular energy emission, using VIRGO/SOHO and MDI/SOHO data sets.

Title: On the Contrast of Faculae and Small Magnetic Features
Authors: Ortiz, A.; Solanki, S. K.; Fligge, M.; Domingo, V.;
   Sanahuja, B.
Bibcode: 2000ESASP.463..399O
Altcode: 2000sctc.proc..399O
  Sunspots, faculae and the magnetic network contribute to solar
  irradiance variations. The contribution due to faculae and the network
  is important for understanding solar irradiance variations, but suffers
  from considerable uncertainty. We focus our study on the faculae and
  the network which produce an increase in the irradiance. Data from
  the Michelson Doppler Interferometer (MDI) are employed. Starting from
  the surface distribution of the solar magnetic field we build a mask
  to detect bright features and study their contrast dependence on limb
  angle and magnetic field. By sorting the magnetic field strength into
  different bins we can distinguish between different associated bright
  features. We find that the contrast of active region faculae and the
  network exhibits different centre to limb variations, implying that
  they need to be treated separately when reconstructing variations of
  the total solar irradiance.

Title: Division XI: Space and High Energy Astrophysics(Astrophysique
    Spatiale et Des Hautes Energies)
Authors: Wamsteker, Willem; Baliunas, S.; Brosch, N.; Cesarsky, C.;
   Courvoisier, Th. -J. L.; da Costa, J. M.; Domingo, V.; Fransson,
   C.; Fabian, A.; Fazio, G.; Hasinger, G.; Inoe, H.; Li, Zhongyuan;
   O'Brien, P.; Oertel, G.; Okuda, H.; Quintana, H.; Rangarajan, T. N.;
   Schilizzi, R.; Shustov, B.; Thronson, H.; Vilhu, O.; Wang, Zhenru
Bibcode: 2000IAUTA..24..357W
Altcode:
  No abstract at ADS

Title: Observations of the latitudinal variation of the solar radiance
    of non-active regions of the sun.
Authors: Domingo, V.; Sanchez, L.; Appourchaux, T.; Andersen, B.
Bibcode: 1998IAUS..185..111D
Altcode:
  The Luminosity Oscillations Imager (LOI) of the VIRGO experiment
  aboard SOHO provides continuous measurement of the solar irradiance
  in a 5 nm band around 500 nm. The solar image is broken down in 12
  pixels distributed in 4 latitudinal bands. The first year of operation
  of the instrument has taken place during a period of solar minimum
  activity. The measurements provide an indication of the distribution
  of the solar irradiance variations versus latitude. Contributions to
  the observed variations due to the presence of active regions are
  discussed in relation to the possible effect of the evolving solar
  cycle (structure of the convection zone): short term variations versus
  long term variations. The problem of the photometric stability of
  the measurements needed for the investigation is thoroughly treated
  by self consistency and by comparison with other instruments on SOHO
  (VIRGO sun- photometers and MDI intensity measurements).

Title: Overview of the SOHO Mission
Authors: Domingo, Vicente
Bibcode: 1998sers.conf..375D
Altcode:
  No abstract at ADS

Title: On the Effect of Active Regions on the Solar Irradiance
Authors: Domingo, V.; Sanchez, L.; Appourchaux, T.; Fröhlich, C.;
   Wehrli, C.; Crommelynck, D.; Pap, J.
Bibcode: 1997ESASP.415..469D
Altcode: 1997cpsh.conf..469D
  No abstract at ADS

Title: SOHO, its day in the Sun
Authors: Domingo, V.
Bibcode: 1997AdSpR..20..581D
Altcode:
  SOHO, the Solar and Heliospheric Observatory, is a project of
  international cooperation between ESA and NASA to study the Sun,
  from its deep core to the outer corona, and the solar wind. Three
  helioseismology instruments are providing unique data for the study
  of the structure and dynamics of the solar interior, from the very
  deep core to the outermost layers of the convection zone. A set of
  five complementary remote sensing instruments, consisting of EUV,
  UV and visible light imagers, spectrographs and coronagraphs, give us
  our first comprehensive view of the outer solar atmosphere and corona,
  leading to a better understanding of the enigmatic coronal heating and
  solar wind acceleration processes. Finally, three experiments complement
  the remote sensing observations by making in-situ measurements of
  the composition and energy of the solar wind and charged energetic
  particles, and another instrument maps the neutral hydrogen in the
  heliosphere, and its dynamic change of the Solar Wind. This paper
  highlights some of the first results from SOHO.

Title: Study of the Effect of Active Regions on the Solar Irradiance
    During Solar Minimum
Authors: Domingo, V.; Sanchez, L.; Appourchaux, T.; Froehlich, C.;
   Wehrli, C.; Hoeksema, T.; Pap, J.
Bibcode: 1997SPD....28.0206D
Altcode: 1997BAAS...29..893D
  We have determined both the size of the area that contributes to the
  solar irradiance increase around an active region and the angular
  distribution of the radiance excess in it, using data obtained during
  about one year around solar minimum (April 1996 - April 1997). During
  the solar minimum and the early raising phase of the new maximum it
  is possible to study the effect of isolated active regions while there
  are few of them. The result of this study will be important to separate
  the contribution of the active regions to the solar irradiance change
  during the solar cycle from any underlying long term effect, if there
  is one. The solar radiance measured by the Low-resolution Oscillations
  Imager (LOI) of the VIRGO instrument and by the MDI instrument aboard
  SOHO is used to determine the dimension of the radiating area. The
  increase in irradance is determined by the Sun Photometers (SPM)
  and Radiometers on the VIRGO instrument.

Title: First results from VIRGO on SoHO
Authors: Frohlich, C.; Andersen, B. N.; Appourchaux, T.; Berthomieu,
   G.; Crommelynck, D. A.; Domingo, V.; Fichot, A.; Finsterle, W.;
   Gómez, M. F.; Gough, D.; Jiménez, A.; Leifsen, T.; Lombaerts, M.;
   Pap, J. M.; Provost, J.; Roca Cortés, T.; Romero, J.; Roth, H. -J.;
   Sekii, T.; Telljohann, U.; Toutain, T.; Wehrli, C.
Bibcode: 1997IAUS..181...67F
Altcode:
  No abstract at ADS

Title: The Solar and Heliospheric Observatory (SOHO) in 1996.
Authors: Domingo, V.; Fleck, B.; Martens, P.; Sanchez, L.
Bibcode: 1997joso.proc....4D
Altcode:
  This report gives a brief overview of SOHO's scientific production in
  its first year of operation.

Title: First Results from VIRGO, the Experiment for Helioseismology
    and Solar Irradiance Monitoring on SOHO
Authors: Fröhlich, Claus; Andersen, Bo N.; Appourchaux, Thierry;
   Berthomieu, Gabrielle; Crommelynck, Dominique A.; Domingo, Vicente;
   Fichot, Alain; Finsterle, Wolfgang; Gómez, Maria F.; Gough, Douglas;
   Jiménez, Antonio; Leifsen, Torben; Lombaerts, Marc; Pap, Judit M.;
   Provost, Janine; Roca Cortés, Teodoro; Romero, José; Roth, Hansjörg;
   Sekii, Takashi; Telljohann, Udo; Toutain, Thierry; Wehrli, Christoph
Bibcode: 1997SoPh..170....1F
Altcode:
  First results from the VIRGO experiment (Variability of solar IRradiance
  and Gravity Oscillations) on the ESA/NASA Mission SOHO (Solar and
  Heliospheric Observatory) are reported. The observations started
  mid-January 1996 for the radiometers and sunphotometers and near the
  end of March for the luminosity oscillation imager. The performance of
  all the instruments is very good, and the time series of the first 4-6
  months are evaluated in terms of solar irradiance variability, solar
  background noise characteristics and p-mode oscillations. The solar
  irradiance is modulated by the passage of active regions across the
  disk, but not all of the modulation is straightforwardly explained in
  terms of sunspot flux blocking and facular enhancement. Helioseismic
  inversions of the observed p-mode frequencies are more-or-less in
  agreement with the latest standard solar models. The comparison of
  VIRGO results with earlier ones shows evidence that magnetic activity
  plays a significant role in the dynamics of the oscillations beyond
  its modulation of the resonant frequencies. Moreover, by comparing
  the amplitudes of different components ofp -mode multiplets, each of
  which are influenced differently by spatial inhomogeneity, we have
  found that activity enhances excitation.

Title: The first results from SOHO.
Authors: Domingo, V.; Fleck, B.; Poland, A.
Bibcode: 1996ESABu..87....7D
Altcode:
  SOHO, launched by an Atlas II-AS from Cape Canaveral on 2 December 1995,
  was inserted into its halo orbit around the L1 Lagrangian point. Typical
  examples of the unique results being obtained with SOHO's instruments
  are presented.

Title: SOLCON Solar Constant Observations from the ATLAS Missions
Authors: Crommelynck, Dominique; Fichot, Alain; Domingo, Vicente;
   Lee, Robert, III
Bibcode: 1996GeoRL..23.2293C
Altcode:
  The solar constant observations obtained by the SOLCON/ATLAS
  experiment during the three successive missions are presented
  based on the Space Absolute Radiometric Reference (SARR) defined
  during the ATLAS-2 mission. The objectives of SOLCON, namely to
  obtain accurate measurements of the solar constant and to compare
  them with the observations obtained from free flyers in the hope of
  establishing a baseline and strategy for monitoring the solar constant
  at climate scale, have been achieved successfully with the three ATLAS
  missions. The long range objective of insuring the solar constant data
  continuity will, however, require that an alternative approach than
  that of the ATLAS program be found to fly and retrieve SOLCON.

Title: The history of thge SOHO mission.
Authors: Huber, M. C. E.; Bonnet, R. M.; Dale, D. C.; Arduini, M.;
   Fröhlich, C.; Domingo, V.; Whitcomb, G.
Bibcode: 1996ESABu..86...25H
Altcode:
  No abstract at ADS

Title: ESA Report to the : 31 : COSPAR meeting held in Birmingham,
    UK July 1996
Authors: Benvenuti, P.; Chicarro, A.; Domingo, V.
Bibcode: 1996ertc.book.....B
Altcode:
  No abstract at ADS

Title: VIRGO: Experiment for Helioseismology and Solar Irradiance
    Monitoring
Authors: Fröhlich, Claus; Romero, José; Roth, Hansjörg; Wehrli,
   Christoph; Andersen, Bo N.; Appourchaux, Thierry; Domingo, Vicente;
   Telljohann, Udo; Berthomieu, Gabrielle; Delache, Philippe; Provost,
   Janine; Toutain, Thierry; Crommelynck, Dominique A.; Chevalier,
   André; Fichot, Alain; Däppen, Werner; Gough, Douglas; Hoeksema,
   Todd; Jiménez, Antonio; Gómez, Maria F.; Herreros, José M.; Cortés,
   Teodoro Roca; Jones, Andrew R.; Pap, Judit M.; Willson, Richard C.
Bibcode: 1995SoPh..162..101F
Altcode:
  The scientific objective of the VIRGO experiment (Variability of solar
  IRradiance and Gravity Oscillations) is to determine the characteristics
  of pressure and internal gravity oscillations by observing irradiance
  and radiance variations, to measure the solar total and spectral
  irradiance and to quantify their variability over periods of days to
  the duration of the mission. With these data helioseismological methods
  can be used to probe the solar interior. Certain characteristics of
  convection and its interaction with magnetic fields, related to, for
  example, activity, will be studied from the results of the irradiance
  monitoring and from the comparison of amplitudes and phases of the
  oscillations as manifest in brightness from VIRGO, in velocity from
  GOLF, and in both velocity and continuum intensity from SOI/MDI. The
  VIRGO experiment contains two different active-cavity radiometers for
  monitoring the solar `constant', two three-channel sunphotometers (SPM)
  for the measurement of the spectral irradiance at 402, 500 and 862 nm,
  and a low-resolution imager (LOI) with 12 pixels, for the measurement
  of the radiance distribution over the solar disk at 500 um. In this
  paper the scientific objectives of VIRGO are presented, the instruments
  and the data acquisition and control system are described in detail,
  and their measured performance is given.

Title: Preface
Authors: Fleck, B.; Domingo, V.; Poland, A.
Bibcode: 1995SoPh..162D...9F
Altcode:
  No abstract at ADS

Title: The SOHO mission.
Authors: Fleck, B.; Domingo, V.; Poland, A. I.
Bibcode: 1995SoPh..162.....F
Altcode:
  SOHO, the Solar and Heliospheric Observatory, is a project of
  international cooperation between ESA and NASA to study the Sun, from
  its deep core to the outer corona. This special issue is dedicated to
  the SOHO payload and to its operation.

Title: The SOHO Mission: an Overview
Authors: Domingo, V.; Fleck, B.; Poland, A. I.
Bibcode: 1995SoPh..162....1D
Altcode:
  The Solar and Heliospheric Observatory (SOHO) is a space mission
  that forms part of the Solar-Terrestrial Science Program (STSP),
  developed in a collaborative effort by the European Space Agency (ESA)
  and the National Aeronautics and Space Administration (NASA). The
  STSP constitutes the first "cornerstone" of ESA's long-term
  programme known as "Space Science — Horizon 2000". The principal
  scientific objectives of the SOHO mission are a) to reach a better
  understanding of the structure and dynamics of the solar interior
  using techniques of helioseismology, and b) to gain better insight
  into the physical processes that form and heat the Sun's corona,
  maintain it and give rise to its acceleration into the solar wind. To
  achieve these goals, SOHO carries a payload consisting of 12 sets of
  complementary instruments. SOHO is a three-axis stabilized spacecraft
  with a total mass of 1850 kg; 1150 W of power will be provided by
  the solar panels. The payload weighs about 640 kg and will consume
  450 W in orbit. SOHO will be launched by an ATLAS II-AS and will
  be placed in a halo orbit around the Sun-Earth L1 Lagrangian point
  where it will be continuously pointing to Sun centre with an accuracy
  of 10 arcsec. Pointing stability will be better than 1 arcsec over
  15 min intervals. The SOHO payload produces a continuous science
  data stream of 40 kbits/s which will be increased by 160 kbits/s
  whenever the solar oscillations imaging instrument is operated in its
  highrate mode. Telemetry will be received by NASA's Deep Space Network
  (DSN). Planning, coordination and operation of the spacecraft and the
  scientific payload will be conducted from the Experiment Operations
  Facility (EOF) at NASA's Goddard Space Flight Center (GSFC).

Title: The SOHO payload and its testing.
Authors: Berner, C.; Domingo, V.
Bibcode: 1995ESABu..84...92B
Altcode:
  The following topics are dealt with: history, science objectives and
  payload, the AIV programme.

Title: Helioseismology
Authors: Hoeksema, J. T.; Domingo, V.; Fleck, B.; Battrick, Bruce
Bibcode: 1995ESASP.376b....H
Altcode: 1995help.confP....H
  No abstract at ADS

Title: SOHO: The Solar and Heliospheric Observatory
Authors: Domingo, V.; Fleck, B.; Poland, A. I.
Bibcode: 1995SSRv...72...81D
Altcode:
  The Solar and Heliospheric Observatory (SOHO), together with the Cluster
  mission, constitutes ESA's Solar Terrestrial Science Programme (STSP),
  the first “Cornerstone” of the Agency's long-term programme “Space
  Science — Horizon 2000”. STSP, which is being developed in a strong
  collaborative effort with NASA, will allow comprehensive studies
  to be made of the both the Sun's interior and its outer atmosphere,
  the acceleration and propagation of the solar wind and its interaction
  with the Earth. This paper gives a brief overview of one part of STSP,
  the SOHO mission.

Title: The SOHO Mission and Helioseismology
Authors: Domingo, V.
Bibcode: 1995ESASP.376a...3D
Altcode: 1995soho....1....3D; 1995heli.conf....3D
  Three of the SOHO scientific instruments are devoted to helioseismology,
  and the mission has been designed with specifications that are required
  to obtain good oscillations measurements. The three instruments were
  selected to complement each other to achieve a comprehensive set of data
  to tackle the pending helioseismologic problems that were considered
  difficult to solve with ground-based instruments. GOLF (l = 0-3) and
  VIRGO (l = 0-7) in the low degree modes area and MDI in the complete
  range up to l = 4000 modes. In addition, several instruments of SOHO
  investigate, by imaging and spectroscopy, the transition region and
  the corona. Three other investigations aboard SOHO study "in situ"
  the resulting solar wind and energetic particles.

Title: VIRGO - the Solar Monitor Experiment on SOHO
Authors: Appourchaux, T.; Domingo, V.; Frohlich, C.; Romero, J.;
   Wehrli, C.; Andersen, B. N.; Berthomieu, G.; Delache, P.; Crommelynck,
   D.; Jimenez, A.; Roca Cortes, T.; Jones, A. R.
Bibcode: 1995ASPC...76..408A
Altcode: 1995gong.conf..408A
  No abstract at ADS

Title: The SOHO mission
Authors: Fleck, B.; Domingo, V.; Poland, A.
Bibcode: 1995somi.book.....F
Altcode:
  No abstract at ADS

Title: SOHO: The Solar and Heliospheric Observatory
Authors: Domingo, V.; Fleck, B.; Poland, A. I.
Bibcode: 1995hlh..conf...81D
Altcode:
  No abstract at ADS

Title: Helioseismology
Authors: Hoeksema, J. T.; Domingo, V.; Fleck, B.; Battrick, Bruce
Bibcode: 1995ESASP.376a....H
Altcode: 1995heli.conf.....H
  No abstract at ADS

Title: The SOHO mission Poland.
Authors: Fleck, B.; Domingo, V.; Poland, Arthur I.
Bibcode: 1995sohp.book.....F
Altcode: 1995QB521.S5828....
  No abstract at ADS

Title: Book Review: Solar photo rates for planetary atmospheres and
    atmospheric pollutants / Kluwer, 1992
Authors: Domingo, V.; Domingo, V.
Bibcode: 1994SoPh..154..401D
Altcode: 1994SoPh..154..401H
  No abstract at ADS

Title: The scientific payload of the space-based Solar and
    Heliospheric Observatory (SOHO)
Authors: Domingo, V.; Fleck, B.; Poland, A. I.
Bibcode: 1994SSRv...70....7D
Altcode:
  The space-based Solar and Heliospheric Observatory (SOHO) is a joint
  venture of ESA and NASA within the frame of the Solar Terrestrial
  Science Programme (STSP), the first “Cornerstone” of ESA's long-term
  programme “Space Science — Horizon 2000”. The principal scientific
  objectives of the SOHO mission are: a) a better understanding of
  the structure and dynamics of the solar interior using techniques of
  helioseismology, and b) a better insight into the physical processes
  that form and heat the Sun's corona, maintain it and give rise to
  its acceleration into the solar wind. To achieve these goals, SOHO
  carries a payload consisting of 12 sets of complementary instruments
  which are briefly described here.

Title: SOHO operations and ground system
Authors: Poland, A. I.; Domingo, V.; Fleck, B.
Bibcode: 1994SSRv...70...13P
Altcode:
  SOHO is a joint ESA/NASA mission to study the sun from its interior to,
  and including, the solar wind in interplanetary space. It is currently
  scheduled for launch in 1995. After launch SOHO with be operated from
  the Experiment Operations Facility (EOF) at Goddard Space Flight Center
  (GSFC). The EOF will consist of facilities for instrument commanding,
  data reception, data reduction and data analysis. In this paper the
  operations concepts including instrument ground commanding from the EOF
  and communications capabilities between the EOF and ground observatories
  and the public networks in general will be described.

Title: Preliminary results of solar constant observations with the
    SOLCON experiment on ATLAS-1
Authors: Crommelynck, D.; Domingo, V.; Barkstrom, B.; Lee, R. B.;
   Donaldson, J.; Telljohann, U.; Warren, L.; Fichot, A.
Bibcode: 1994AdSpR..14i.253C
Altcode: 1994AdSpR..14..253C
  A brief description is given of the SOLCON experiment on ATLAS 1,
  its scientific and technical objectives, as well as its measurement
  principle and its on board chronology of operations. A preliminary
  value of the solar constant during the third solar operation of the
  mission is also provided.

Title: Summary of Future Space Observations at Different Wavelengths
Authors: Domingo, V.
Bibcode: 1994svsp.coll..101D
Altcode: 1994IAUCo.143P.101D
  No abstract at ADS

Title: Total Solar Irradiance Observations from the EURECA and
    ATLAS Experiments
Authors: Crommelynck, D.; Domingo, V.; Fichot, A.; Lee, B.
Bibcode: 1994svsp.coll...63C
Altcode: 1994IAUCo.143P..63C
  No abstract at ADS

Title: SOHO Science Opportunities
Authors: Fleck, B.; Domingo, V.; Poland, A. I.
Bibcode: 1994scs..conf..609F
Altcode: 1994IAUCo.144..609F
  The principal scientific objectives of the SOHO mission are: a)
  a better understanding of the structure and dynamics of the solar
  interior using techniques of helioseismology, and b) a better insight
  into the physical processes that form and heat the Sun's corona,
  maintain it and give rise to its acceleration into the solar wind. To
  achieve these goals, SOHO carries a payload consisting of 12 sets of
  complementary instruments which are briefly described here.

Title: SOHO Operations
Authors: Fleck, B.; Domingo, V.; Poland, A. I.
Bibcode: 1994scs..conf..614F
Altcode: 1994IAUCo.144..614F
  SOHO, the Solar and Heliospheric Observatory, is currently scheduled
  for launch in 1995. After launch SOHO will be operated from the
  Experiment Operations Faciliy (EOF) at Goddard Space Flight Center
  (GSFC). The EOF will consist of facilities for instrument commanding,
  data reception, data reduction and data analysis. This paper briefly
  describes the operations concepts.

Title: SOHO - The Solar and Heliospheric Observatory
Authors: Fleck, B.; Domingo, V.
Bibcode: 1994smf..conf..408F
Altcode:
  No abstract at ADS

Title: SOHO: science objectives and capabilities
Authors: Fleck, B.; Domingo, V.; Poland, A. I.
Bibcode: 1994ASIC..433..517F
Altcode:
  No abstract at ADS

Title: Invited Talk: (SOHO Operations and Coordination with
    Ground-based Observatories)
Authors: Domingo, V.; Fleck, B.
Bibcode: 1993BAAS...25.1195D
Altcode:
  No abstract at ADS

Title: Some European activities in support of the SOHO mission.
Authors: Huber, Martin C. E.; Domingo, Vicente
Bibcode: 1992ESASP.348..393H
Altcode: 1992cscl.work..393H
  The rationale and potential functions of the European Science Data
  and Operations Centre (ESDOC) are outlined. Other efforts, namely
  the gathering of support - through the Joint Organisation for Solar
  Observations (JOSO) - for ground-based observations in the context of
  the SOHO mission, as well as the development of a vacuum-ultraviolet
  (VUV) transfer source standard - to be used for radiometrically
  intercomparing spectrometric SOHO instruments - are also described.

Title: ESA's report to the 29th COSPAR Meeting
Authors: Appourchaux, T.; Chicarro, A.; Domingo, V.; Fridlund, M.;
   Huber, M.; Innocenti, L.; Jakobsen, P.; Kessler, M.; Lebreton, J. P.;
   Parmar, A.
Bibcode: 1992wadc.meet.....A
Altcode:
  All ESA missions in operation, under development, or in planning are
  described. Missions beyond the operational phase are also presented
  if considerable effort is still being expended in supporting the data
  analysis through an archive. The aging and completed missions are:
  IUE, Exosat, Hipparcos, Giotto extended mission, Ulysses, and Hubble
  Space Telescope. The projects under development are: Infrared Space
  Observatory (ISO), the Solar Terrestrial Science Program (STSP) (which
  comprises the four Cluster spacecraft and the Solar and Heliospheric
  Observatory (SOHO)), the X-ray Multimirror Mission (XMM) and the
  Cassini/Huygens mission. Missions under study are: the Far Infrared
  Space Telescope (FIRST), the comet nucleus sample return (Rosetta),
  the International Gamma Ray Laboratory (INTEGRAL), a network of three
  semi hard landers to be placed on the Martian surface (MARSNET), a
  mission for probing the interior and rotation of stars (PRISMA), and
  a Satellite Test of the Equivalence Principle (STEP). Missions beyond
  Horizon 2000 are: Return to the Moon, interferometry from space, and
  Vulcan. ESA platforms described are Eureca (the European retrieval
  carrier) and Simuris (a solar system and stellar interferometric
  mission for ultrahigh resolution imaging and spectroscopy).

Title: SOHO and Cluster. Solar and geospheric plasmas and solar
    structure.
Authors: Domingo, V.; Schmidt, R.
Bibcode: 1991EN.....22..213D
Altcode:
  The SOHO/Cluster satellite missions will provide an unique opportunity
  to advance our understanding of the physics of the solar-terrestrial
  system.

Title: Three Solar Filament Disappearances Associated with
    Interplanetary Low Energy Particle Events
Authors: Sanahuja, B.; Heras, A. M.; Domingo, V.; Joselyn, J. A.
Bibcode: 1991SoPh..134..379S
Altcode:
  Three low-energy particle events (35-1600 keV) associated with
  interplanetary shocks, detected at 1 AU by ISEE-3, have been
  identified as originating in solar disappearing filaments instead
  of large flares. This increases to fourteen the number of events
  of this kind presently known. The observational characteristics of
  these non-flare generated events are similar to the ones of the other
  eleven events already known (i.e., absence of type II or IV bursts,
  weak X-ray emission, Hα brightening in the surroundings of the
  filament disappearance, frequent presence of a double-ribbon event,
  slow propagation of the generated interplanetary shock, lack of shock
  deceleration).

Title: The SOHO Space Satellite: UV instrumentation.
Authors: Poland, Arthur I.; Domingo, Vicente
Bibcode: 1991SPIE.1343..310P
Altcode:
  The solar and heliospheric observatory, SOHO will be placed into a halo
  orbit around the L1 sun-earth Lagrangian point in 1995. The authors
  describe the ultra-violet and EUV instruments designed to study
  the solar atmosphere from the chromosphere through the corona. The
  instruments and their basic characteristics are: 1) SUMER - a normal
  incidence telescope with a normal incidence spherical concave grating
  for stigmatic imaging to measure line profiles and images in the
  wavelength range from 500 Å to 1600 Å with a 1.5″resolution; 2) CDS
  - a grazing incidence telescope with one grazing incidence astigmatic
  spectrograph and one normal incidence toroidal grating spectrograph
  to measure line ratios and images in the range from 170 Å to 800
  Å with a 2″resolution; 3) EIT - a normal incidence multilayered
  telescope to produce narrow band pass images in the spectral lines at
  171 Å, 195 Å, 284 Å, and 304 Å with a 3″resolution; 4) UVCS - a
  normal incidence coronagraph with a normal incidence toroidal grating
  spectrograph to measure line profiles and images of several EUV lines
  from ≡500 Å to ≡1200 Å with a several arcsecond resolution;
  and 5) SWAN - a lens with hydrogen absorption cell and interference
  filter to measure Ly-α profiles in the far corona and heliosphere.

Title: The helioseismology experiment on the Phobos planetary
    mission. Preliminary results
Authors: Frohlich, C.; Bonnet, R. M.; Bruns, A. V.; Vial, J. C.;
   Delaboudiniere, J. P.; Domingo, V.; Kollath, Z.; Kotov, V. A.;
   Rachkovskii, D. N.; Wehrli, Ch.; Toulain, T.; Shumko, S. M.
Bibcode: 1991BCrAO..83...18F
Altcode:
  No abstract at ADS

Title: The Solar Variations (SOVA) experiment in the EURECA space
    platform
Authors: Crommelynck, D.; Domingo, V.; Fröhlich, C.
Bibcode: 1991AdSpR..11d..83C
Altcode: 1991AdSpR..11Q..83C
  The Solar Variations (SOVA) experiment aboard EURECA will measure the
  total and spectral irradiance of the Sun, and their variations. Aims
  of the experiment are: - to study the short term (hours to months)
  variations of the solar irradiance for the investigation of the
  mechanisms of energy redistribution in the convection zone, - to study
  periodic fluctuations, with periods between a few minutes and several
  hours, for helioseismology and, - to measure the absolute value of the
  solar constant to determine its long term variations when compared
  with previous and future measurements. Two absolute active cavity
  radiometers of different design will measure independently the value
  of the total solar irradiance, one relative radiometer will measure
  the variations of the total solar irradiance and five photometers
  will measure the variations of the spectral irradiance in 5-nm wide
  wavelength bands centred at 335, 480, 500, 546 and 865 nm. The European
  Retrievable Carrier (Eureca), is an ESA space platform that will be
  placed in orbit around the Earth by the NASA Shuttle in October 1991,
  and will be recovered after 6 months of operation.

Title: Phase difference between irradiance and velocity in low degree
    solar p-modes
Authors: Schrijver, C. J.; Jiménez, A.; Domingo, V.; Fröhlich, C.
Bibcode: 1991AdSpR..11d..77S
Altcode: 1991AdSpR..11Q..77S
  We derive phase differences between irradiance and full-disk velocity
  variations for l=0, 1, and 2 modes with order ranging from 11 up to 30
  (1.8-4.3mHz). We use irradiance measurements from the IPHIR instrument
  flown on the PHOBOS mission to Mars during the second half of 1988,
  and simultaneous velocity measurements obtained at Tenerife. The
  IPHIR instrument measures broad-band irradiance fluctuations and the
  derived phase differences are therefore typical of the deep layers of
  the photosphere. We select three one week intervals from the 155 day
  observing interval of PHOBOS 2 for which simultaneous good quality
  velocity data are available. We find a smooth variation of the phase
  difference between irradiance at 500nm (5nm FWHM) and velocity from
  about 70° at 1.8mHz to 145° at 2.5mHz, while it remains roughly
  constant at 145° degrees up to at least 3.5mHz, and possibly up to
  4.3mHz. We also show that the phase differences between the green
  (500nm) and red (865nm) channels does not differ significantly from
  zero below 3mHz, while a small difference of about 10° may exist at
  higher frequencies.

Title: The helioseismological experiment at the Phobos interplanetary
    station - Preliminary results
Authors: Froehlich, C.; Bonnet, R. M.; Bruns, A. V.; Vial, J. C.;
   Delaboudiniere, J. P.; Domingo, V.; Kollath, Z.; Kotov, V. A.;
   Rachkovskii, D. N.; Wehrli, Ch.
Bibcode: 1991IzKry..83...22F
Altcode:
  Preliminary results obtained from IPHIR (Interplanetary Helioseismology
  by Irradiance Measurements), a solar irradiance experiment on board
  the Soviet planetary mission Phobos-2, are presented. During the
  spacecraft's flight to Mars, the instrument gathered valuable data on
  tiny variations of solar irradiance over the course of six months. The
  data clearly show 5-min oscillations with relative amplitudes of about
  10 exp -5 and with a well-defined pattern of discrete peaks in the
  power spectrum. The data of the red channel (it exhibited the lowest
  degradation of sensitivity over time) reveal remarkable temporal changes
  of amplitudes of discrete peaks within a period range of about 5 min,
  but with excellent frequency stability.

Title: Desapariciones de filamentos solares como origen de sucesos
    de particulas y de los choques interplanetarios asociados.
Authors: Heras, A. M.; Sanahuja, B.; Domingo, V.
Bibcode: 1991BAOM...12...12H
Altcode:
  No abstract at ADS

Title: ESA's report to the 28th COSPAR meeting
Authors: Chicarro, A.; Domingo, V.; Frisk, U. O.; Jakobsen, P.;
   Knott, K.; Kessler, M. F.; Lebreton, J. P.; Marsden, R.; Peacock,
   A.; Perryman, M. A. C.
Bibcode: 1990STIN...9030141C
Altcode:
  Ongoing and complete missions, including IUE, EXOSAT, Hipparcos and
  Giotto, are discussed. Projects under development, including Ulysses,
  Hubble Space Telescope, ISO (Infrared Space Observatory), the Solar
  Terrestrial Science Programme (STSP), Cassini/Huygens and the high
  throughput X ray spectroscopy mission (XMM), are reported. Missions
  under study are reviewed; the submillimeter spectroscopy mission
  (FIRST); Rosetta CNSR (Comet Nucleus Sample Return); third millenium
  Mars exploration, interferometry from space and Vulcan missions. The
  Eureca A and Columbus Polar Platforms are included.

Title: Phase Differences Between Luminosity and Velocity Measurements
    of the Acoustic Modes
Authors: Jiménez, A.; Álvarez, M.; Andersen, N. B.; Domingo, V.;
   Jones, A.; Pallé, P. L.; Roca Cortés, T.
Bibcode: 1990SoPh..126....1J
Altcode:
  With two photometric stations (Tenerife and Baja California)
  the luminosity p-mode spectrum at different wavelengths has been
  identified. After a coherence analysis between data from both stations
  to verify the solar origin of the peaks identified in luminosity, a
  comparative study with simultaneous velocity measurements (obtained at
  Tenerife only) has also been made. As a result the frequency dependence
  of the phase difference between luminosity and velocity p-modes has been
  obtained that is interpreted in terms of a nonadiabatic behaviour of the
  solar atmosphere. The amplitude ratios between luminosity and velocity
  p-modes have also been obtained. All these results are compared with
  theoretical expectations.

Title: SOHO - an Observatory to Study the Solar Interior and the
    Solar Atmosphere
Authors: Poland, A. I.; Domingo, V.
Bibcode: 1990ASSL..166..277P
Altcode: 1990oeob.coll..277P; 1990IAUCo.123..277P
  The Solar and Heliospheric Observatory (SOHO) is described. The two
  main objectives of SOHO are to improve understanding of solar coronal
  phenomena and to study solar structure and interior dynamics from
  its core to the photosphere. The primary goals of the coronal and
  solar wind studies are to understand the coronal heating mechanism
  and its expansion into the solar wind. These goals will be achieved
  both by remote sensing of the solar atmosphere with high resolution
  spectrometers and telescopes and by in situ measurement of the
  composition and energy of the resulting solar wind and the energetic
  particles that propagate through it. The structure and interior dynamics
  are to be studied by helioseismological methods and the measurement
  of solar irradiance variations. The SOHO spacecraft will be three-axis
  stabilized and located in a halo orbit around the L1 Lagrangian point
  (approximately 1 percent of the distance from the Earth to the Sun). It
  is currently scheduled for launch in July 1995.

Title: The Soho Project and Helioseismology
Authors: Domingo, Vicente
Bibcode: 1990LNP...367..257D
Altcode: 1990psss.conf..257D
  The Solar and heliospheric observatory (Soho) space mission being
  developed by ESA and NASA will carry together with other instruments
  devoted to the study of the solar atmosphere and solar wind, a set
  of instruments that will provide a comprehensive set of measurements
  of solar oscillations. Two investigations in Soho aim primarily at the
  study of g-modes and low l p-modes and a third one will have the central
  interest in high degree oscillations while aiming to extend the validity
  of its measurements to low 1 modes overlapping with the other two
  investigations. The Soho mission is being designed having into account
  the needs of the helioseismology experiments and therefore should be
  able to provide the best possible infrastructure for the production
  of good quality data. For the data analysis the three experiments
  will coordinate their operation and the data handling. It is expected
  that Soho will greatly profit of the experience gained with GONG, as
  a large fraction of the co-investigators in the Soho helioseismology
  investigations form part of the GONG project. The investigations in
  Soho have finished the definition phase of their instruments and
  the contractor selected by ESA has started on 1 December 1989 the
  industrial Phase B, or design phase, of the spacecraft and mission
  for a launch in March 1995.

Title: Retrieval from Earth Orbit of the Ultra Heavy Cosmic Ray
    Experiment on the LDEF Spacecraft
Authors: Thompson, A.; O'Sullivan, D.; Wenzel, K. -P.; Domingo, V.;
   Domingo, C.; Daly, J.; Smit, A.
Bibcode: 1990ICRC....4..441T
Altcode: 1990ICRC...21d.441T; 1989ICRC....4..441T
  No abstract at ADS

Title: Energetic particles, interplanetary shocks and solar activity
Authors: Domingo, V.; Sanahuja, B.; Heras, A. M.
Bibcode: 1989AdSpR...9d.191D
Altcode: 1989AdSpR...9..191D
  The study of the flow-pattern of energetic protons (35-1600 keV)
  associated with interplanetary shocks observed by ISEE-3, is analyzed
  as a function of the relative position of the spacecraft with respect
  to the shock and to the solar activity that has triggered the events,
  and is complemented with a statistical study on the thickness
  of bidirectional particle regimes associated with interplanetary
  shocks. The result indicates that the region behind the shock where the
  driver would be located extends over a wide angle around the longitude
  of the triggering event, with little asymmetry with respect to the
  propagation direction.

Title: Solar Luminosity Oscillation Telescope (SLOT).
Authors: Andersen, Bo Nyborg; Domingo, V.; Jones, A. R.; Korzennik,
   Sylvain G.; Jimenez, A.; Palle, Pere L.; Regulo, C.; Roca Cortés,
   Teodoro
Bibcode: 1988ESASP.286..175A
Altcode: 1988ssls.rept..175A
  Low degree l = 0-2 solar p-modes have been detected with the
  SLOT instruments at Izaña and Baja California. The main source
  of noise for these ground based observations is in the terrestrial
  atmosphere. However, the data acquisition system still has to have very
  slow intrinsic noise. The authors describe how this is achieved in the
  SLOT instruments. They also give a general description of the design
  and operating principles of the photometers and data acquisition system.

Title: VIRGO: The solar monitor experiment on SOHO.
Authors: Froehlich, C.; Andersen, Bo Nyborg; Berthomieu, G.;
   Crommelynck, D.; Delache, Philippe; Domingo, V.; Jimenez, A.; Jones,
   A. R.; Roca Cortés, Teodoro; Wehrli, Ch.
Bibcode: 1988ESASP.286..371F
Altcode: 1988ssls.rept..371F
  The VIRGO Experiment (Variability of solar Irradiance and Gravity
  Oscillations) contains two types of active cavity radiometers for
  monitoring of the solar "constant", two three channel sunphotometers
  (SPM) for the measurement of spectral irradiance at 335, 500 and 865 nm
  and a low resolution imager (LOI) with 12 pixels. The main scientific
  objective is probing the solar interior by helioseismology with p-
  and g-mode solar oscillations determined from spectral irradiance
  (SPM) and radiance (LOI) variations on time scales of minutes to
  the mission time. Moreover, the measurements of the variability of
  the solar "constant" and spectral irradiance over periods of days to
  the mission time will yield information about the convection zone, as
  will the comparison of the amplitudes and phases of the oscillations
  as manifested in irradiance and radiance (from VIRGO) and velocity
  (from GOLF and SOI).

Title: Soho status.
Authors: Domingo, V.
Bibcode: 1988ESASP.286..363D
Altcode: 1988ssls.rept..363D
  The scientific payload for Solar and Heliospheric Observatory (Soho)
  space mission has been selected. Soho will study the structure of
  the solar interior, the physics of the solar corona and the origin of
  the solar wind. The spacecraft definition phase will start in October
  1989. The launch is expected for March 1995.

Title: Solar luminosity oscillations from two stations and correlation
    with velocity measurements.
Authors: Jimenez, A.; Palle, Pere L.; Roca Cortés, Teodoro; Andersen,
   N. B.; Domingo, V.; Jones, A. R.; Alvarez, M.; Ledezma, E.
Bibcode: 1988ESASP.286..163J
Altcode: 1988ssls.rept..163J
  Since 1984 the measurements of a quadrupole photometer sites at the
  Observatorio del Teide (Izaña, Tenerife) have made it possible to
  identify the p-mode luminosity spectrum with simultaneous velocity
  observations. Comparing this data, the adiabatic behaviour of solar
  atmosphere and theoretical expectations from solar models have been
  tested. Now, in order to increase the signal-to-noise ratio and reduce
  the sidebands due to the night-time data gaps, a second identical
  photometer was set-up in December 1987, at the Observatorio de San
  Pedro Mártir (Baja California Norte, Mexico). The first results of
  the observations of these two stations are analyzed and compared with
  simultaneous velocity measurements.

Title: IPHIR: The helioseismology experiment on the PHOBOS mission.
Authors: Fröhlich, C.; Bonnet, R. M.; Bruns, A. V.; Delaboudinière,
   J. P.; Domingo, V.; Kotov, V. A.; Kollath, Z.; Rashkovsky, D. N.;
   Toutain, T.; Vial, J. C.; Wehrli, C.
Bibcode: 1988ESASP.286..359F
Altcode: 1988ssls.rept..359F
  IPHIR (InterPlanetary Helioseismology by IRradiance measurements) is
  a solar irradiance experiment on the USSR planetary mission PHOBOS to
  Mars and its satellite Phobos. The experiment is a cooperative effort
  of PMOD/WRC, LPSP, SSD/ESA, KrAO and CRIP. The sensor is a three channel
  sunphotometer (SPM) which measures the solar spectral irradiance at 335,
  500 and 865 nm with a precision of better than 1 ppm. A two axis solar
  sensor (TASS) is added to monitor the moderate solar pointing of the
  spacecraft. A microprocessor based data processing unit controls the
  sensor operation, acquires the data, and performs the data compression
  for the transmission at a mean rate of 1 bit/s. The two spacecrafts
  have been launched on July 7th and 12th, 1988. The experiment on
  PHOBOS I gathered data during 45 days before the S/C was lost, the
  one on PHOBOS II is still operating. The data recovery is excellent
  with virtually 100% coverage. Although the signal is disturbed by the
  pointing of the spacecraft the results of a preliminary analysis in
  the range of the 5-minutes oscillations demonstrate the improvement
  achievable due to the fact that the time series is truly continuous
  and the instrumental and sampling noise is very low.

Title: Luminosity Oscillations Imager (LOI).
Authors: Andersen, Bo Nyborg; Domingo, V.; Jones, A. R.; Jimenez,
   A.; Palle, Pere L.; Regulo, C.; Roca Cortés, Teodoro
Bibcode: 1988ESASP.286..385A
Altcode: 1988ssls.rept..385A
  The VIRGO (Variability in Irradiance and Gravity Oscillations)
  investigation has been selected to fly on ESA's SOHO mission. One of
  the components of the VIRGO is a small imaging solar photometer. This
  instrument, the Luminosity Oscillations Imager (LOI), will observe
  the solar radiance with 12 pixels resolution. A prototype of the LOI
  has been developed at ESTEC. This prototype was built mainly to test
  possible detector configurations, the data acquisition system and the
  internal guider. The prototype has been operating at Izaña, Tenerife
  since April this year.

Title: SOHO: an observatory to study the solar interior and the
    solar atmosphere
Authors: Domingo, V.; Poland, A. I.
Bibcode: 1988sohi.rept....7D
Altcode:
  The Solar and Heliospheric Observatory (SOHO) is described. The two
  main objectives of SOHO are to improve understanding of solar coronal
  phenomena and to study solar structure and interior dynamics from
  its core to the photosphere. The primary goals of the coronal and
  solar wind studies are to understand the coronal heating mechanism
  and its expansion into the solar wind. These goals will be achieved
  both by remote sensing of the solar atmosphere with high resolution
  spectrometers and telescopes and by in situ measurement of the
  composition and energy of the resulting solar wind and the energetic
  particles that propagate through it. The structure and interior dynamics
  are to be studied by helioseismological methods and the measurement
  of solar irradiance variations. The SOHO spacecraft will be three-axis
  stabilized and located in a halo orbit around the L1 Lagrangian point
  (approximately 1 percent of the distance from the Earth to the Sun). It
  is currently scheduled for launch in July 1995.

Title: VIRGO: The solar monitor experiment on SOHO
Authors: Froehlich, C.; Andersen, B. N.; Berthomieu, G.; Crommelynck,
   D.; Delache, Ph.; Domingo, V.; Jimenez, A.; Jones, A. R.; Roca Cortes,
   T.; Wehrli, Ch.
Bibcode: 1988sohi.rept...19F
Altcode:
  The Variability of solar IRradiance and Gravity Oscillations (VIRGO)
  experiment contains two types of active cavity radiometers for
  monitoring of the solar constant, two three channel sunphotometers for
  the measurement of spectral irradiance at 335, 500 and 865 nm and a
  low resolution imager with 12 pixels. The main scientific objective
  is probing the solar interior by helioseismology with p and g mode
  solar oscillations determined from spectral irradiance and radiance
  variations on time scales of minutes to the mission time. Information
  about the convection zone is thus obtained. The comparison of the
  amplitudes and phases of the oscillations as manifested in irradiance
  and radiance (from VIRGO) and velocity as measured by the GOLF (global
  oscillations at low frequencies) experiment are also used in analyzing
  the convection zone.

Title: Diurnal photometric conditions at Teide observatory and
    long-term solar irradiance variations
Authors: Andersen, B.; Domingo, V.; Jiménez, A.; Jones, A.; Korzennik,
   S.; Pallé, P. L.; Pérez Hernández, F.; Régulo, C.; Roca Cortés,
   T.; Tomás, L. L.
Bibcode: 1988SoPh..116..391A
Altcode:
  Monochromatic extinction coefficients at four wavelengths have been
  obtained over a period of more than two years at the Observatorio del
  Teide (Izaña Tenerife) using a full disc, direct sunlight, quadruple
  photometer devoted to the detection of integral luminosity oscillations
  of the Sun. The mean extinction coefficients (0.13 at 500 nm) show
  a seasonal variation of about 15%, the best atmospheric conditions
  being in winter and autumn. Moreover, in anyone day the extinction
  coefficient in the afternoon is always lower than the one in the
  morning by ∼ 7%. A one-year period fluctuation, with an amplitude
  of ∼ 0.035 mag, has been identified in the instrumental magnitudes
  outside the atmosphere, and is interpreted as the variation produced
  by the different Sun-Earth distance from winter to summer. Finally,
  the study made to detect periodic time fluctuations in both, Sun's
  magnitude and extinction coefficients, has given null results at levels
  of ∼ 0.04 and ∼ 1.8%, respectively.

Title: ESA report to the 27th COSPAR meeting
Authors: Domingo, V.; Fisk, U. O.; Grard, R.; Jakobsen, P.; Kessler,
   M. F.; Lebreton, J. -P.; Marsden, R.; Peacock, A.; Pedersen, A.;
   Perryman, M. A. C.
Bibcode: 1988STIN...8830556D
Altcode:
  The ISEE, IUE, EXOSAT, and Giotto missions are described. The
  status of the Ulysses, Hubble Space Telescope, HIPPARCOS, ISO, and
  solar-terrestrial science programs is discussed. The high throughput
  X-ray spectroscopy mission, submillimeter spectroscopy mission, and the
  comet nucleus sample return mission are presented. The CASSINI, GRASP,
  Lyman, Quasat, Vesta, and Giotto extended missions are introduced. The
  EURECA and Columbus space station programs are reviewed.

Title: Low-energy particle events generated by solar disappearing
    filaments
Authors: Heras, A. M.; Sanahuja, B.; Domingo, V.; Joselyn, J. A.
Bibcode: 1988A&A...197..297H
Altcode:
  Five large low-energy (E less than 2 MeV) proton events associated
  with interplanetary shocks, observed at 1 AU by the ISEE-3 probe,
  appeared to be triggered by solar disappearing filaments instead of
  solar flare activity. These events will join the other six events of
  this kind already known. In this paper these events are identified and
  a comparative study of the interplanetary proton for the nonflare and
  flaring situations is provided. Proton events that are triggered by
  disappearing filaments appears not to be associated with the strong
  X-ray or radio radiation that characterizes solar flares.

Title: Diffuse Gamma Rays with Energies Greater than 1 X 10 14 eV
    Observed in the Southern Hemisphere
Authors: Suga, K.; Toyoda, Y.; Kamata, K.; Murakami, K.; Lapointe,
   M.; Gaebler, J.; Escobar, I.; Saavedra, O.; Domingo, V.; Shibata,
   S.; Akiyama, H.; Takano, M.; Uchino, K.
Bibcode: 1988ApJ...326.1036S
Altcode:
  The data of extensive air showers with a low content of muons and
  hadrons, observed in the period 1964-1966 at Mount Chacaltaya in
  Bolivia, have been reanalyzed. Arrival directions of those showers
  selected so as to favor small initiation depths in the atmosphere (to
  enhance the contribution from gamma-ray-initiated showers) reveal a
  3.8 sigma peak above an expected background from the region of alpha
  = 180-210 deg in the band of delta = 0 to -40 deg. The integral flux
  of diffuse gamma-rays above 1 x 10 to the 14th eV estimated from this
  excess is about 6.0 x 10 to the -12th/sq cm per sec per sr. In order
  to explain this very high flux, the possible contribution of gamma-rays
  from Loop 1 as well as the inverse Compton photons produced in the 2.7
  K photon background as progeny of gamma-rays from Cyg X-3-like sources.

Title: Cluster and SOHO: A joint endeavor by ESA and NASA to address
    problems in solar, heliospheric, and space plasma physics
Authors: Schmidt, Rudolf; Domingo, Vicente; Shawhan, Stanley D.;
   Bohlin, David
Bibcode: 1988EOSTr..69..177S
Altcode:
  The NASA/ESA Solar-Terrestrial Science Program, which consists of
  the four-spacecraft cluster mission and the Solar and Heliospheric
  Observatory (SOHO), is examined. It is expected that the SOHO spacecraft
  will be launched in 1995 to study solar interior structure and the
  physical processes associated with the solar corona. The SOHO design,
  operation, data, and ground segment are discussed. The Cluster mission
  is designed to study small-scale structures in the earth's plasma
  environment. The Soviet Union is expected to contribute two additional
  spacecraft, which will be similar to Cluster in instrumentation and
  design. The capabilities, mission strategy, spacecraft design, payload,
  and ground segment of Cluster are discussed.

Title: Correlation between velocity and luminosity measurements of
    solar oscillations
Authors: Jimenez, A.; Palle, P. L.; Roca Cortes, T.; Domingo, V.
Bibcode: 1988A&A...193..298J
Altcode:
  Following the work started in 1984 to detect the solar intensity
  oscillations from ground (Jimenez et al., 1986), simultaneous
  velocity and intensity observations of 16 contiguous days of very high
  atmospheric quality obtained at Izana (Tenerife) have been analyzed. The
  frequencies of the p-mode intensity spectrum at three channels
  (500, 680 and 870 nm) and those of the velocity spectrum have been
  obtained. Amplitude ratios in the intensity measurements give results
  of 1.6 and 2.2 when comparing the last two channels with the first one,
  and their relative phases give a null result at any frequency in the
  5 minute range. The relative phases between luminosity and intensity
  measurements give a mean result of -120 degrees. Finally, the ratio
  of the amplitudes of the intensity oscillations to the velocity ones
  correlates very well with theoretical expectations and it yields a
  fractional variation of the effective temperature of 2 x 10 to the -6th.

Title: Groundbased Observations of Solar Luminosity Oscillations
Authors: Andersen, B. N.; Domingo, V.
Bibcode: 1988IAUS..123...67A
Altcode:
  Results from ground based observations of low degree solar luminosity
  variations are presented. By using data from up to 15 consecutive
  excellent days the majority of the l = 0, 1 and 2 peaks in the region
  2.5 - 3.5 mHz may marginally be identified.

Title: The SOHO project: helioseismology investigations
Authors: Domingo, V.; Poland, A.
Bibcode: 1988AdSpR...8k.109D
Altcode: 1988AdSpR...8..109D
  The solar and heliospheric observatory, Soho, will be placed into a
  halo orbit around the L1 Sun-Earth Lagrangian point in 1995. It will
  carry a set of instruments to study the physical phenomena in the
  solar atmosphere that heat the solar corona, the mechanisms by which
  the solar corona expands into the solar wind, and investigate the
  structure of the solar interior by the study of solar oscillations,
  both in velocity and in intensity (Helioseismology). <P />In this paper
  we describe the mission and the investigations to be carried out with
  the helioseismology instruments in the payload. A solar oscillations
  imager will measure velocity oscillations of degree up to 4000, while
  two other instruments will measure very long series of low degree modes
  of oscillation, one of them in velocity and the other in irradiance. The
  data obtained will be used to study the radial stratification and the
  longitudinal variation of the physical characteristics of the Sun,
  as well as many dynamical phenomena of the upper layers of the solar
  atmosphere.

Title: Earthbased Observations of Solar Luminosity Oscillations
Authors: Jimenez, A.; Palle, P. L.; Perez-Hernandez, F.; Regulo, C.;
   Roca-Cortes, T.; Domingo, V.; Korzennik, S.
Bibcode: 1988IAUS..123...71J
Altcode:
  Earth based multichannel photometry of integral sunlight has been
  obtained at Izaña (Tenerife) during 1984 - 1986. Power spectra of the
  solar luminosity variations of individual days show power in the 5
  minute interval above noise at a level comparable to SMM data. When
  combining contigous days of data the signature of p mode solar
  oscillations spectrum appears, although individual peak identification
  is difficult.

Title: Helioseismology from Space - the SOHO Project
Authors: Domingo, V.
Bibcode: 1988IAUS..123..545D
Altcode:
  The Solar and Heliospheric Observatory (SOHO) has been proposed with
  the following aims: To investigate and understand the physical processes
  that form the solar corona, maintain it and give rise to the expanding
  solar wind, by high resolution spectroscopy of the chromosphere,
  transition region and corona in combination with "in situ" study of the
  resulting solar wind streams and associated fields; to investigate the
  solar interior structure by methods of helioseismology. It is foreseen
  that the spacecraft will be launched by the end of 1994.

Title: Current Understanding and Issues on Electron Beam Injection
    in Space
Authors: Poland, A. I.; Domingo, V.
Bibcode: 1988AdSpR...8k.101P
Altcode: 1988AdSpR...8Q.101P
  The Solar and Heliospheric Observatory (SOHO) satellite mission is
  planned to study the solar interior, to investigate the physical
  phenomena related to the formation of the solar corona and the solar
  wind, and to make in situ measurements of the solar wind. The SOHO
  instruments designed to study the solar atmosphere and the solar wind
  are described. The experiments include the study of solar UV radiation,
  a coronal diagnostic spectrometer, an extreme UV imaging telescope, a UV
  coronagraph spectrometer, a white light and spectrometric coronagraph,
  and a study of solar wind anisotropies.

Title: Soho and Cluster - the scientific instruments.
Authors: Domingo, V.; Schmidt, R.; Poland, A. I.; Goldstein, M. L.
Bibcode: 1988ESABu..56...24D
Altcode:
  The need to understand the complex processes that control the structure
  and dynamics of our daylight star and define the Earth's environment
  in space, has long been widely realised. Its continuing importance is
  reflected by the fact that twenty-three Principal Investigators and
  several hundred Co-Investigators from more than eighteen countries
  are now actively involved in the preparations for and execution of
  the Soho and Cluster missions.

Title: Low-energy protons associated with interplanetary shocks as
    a coherent population
Authors: Sanahuja, B.; Domingo, V.
Bibcode: 1987JGR....92.7280S
Altcode:
  We investigate the flow pattern of low-energy protons (35-1600 keV)
  associated with interplanetary shocks observed by ISEE-3 between August
  1978 and April 1980. The analysis of the shape of the distribution
  function in the solar wind frame and its temporal evolution indicates
  that the low-energy protons can behave as a coherent, independent
  population of particles in the solar wind. Ahead of the shock this
  population propagates along the magnetic field in the same direction as
  the solar wind flow, while after the passage of the perturbed region
  associated with the shock, it propagates in the opposite sense. The
  behavior of the flow pattern of this population through the shock
  front is discussed for the 17 largest events observed in this period.

Title: Extended Exposure for the Ultra Heavy Cosmic Ray Experiment
    on the LDEF Spacecraft
Authors: Thompson, A.; O'Sullivan, D.; Domingo, C.; Wenzel, K. -P.;
   Domingo, V.
Bibcode: 1987ICRC....2..402T
Altcode: 1987ICRC...20b.402T; 1987ICRC....2..402D
  No abstract at ADS

Title: UHE gamma-rays from Vela X-1 and Cen X-3.
Authors: Suga, K.; Toyoda, Y.; Kamata, K.; Murakami, K.; Lapointe,
   M.; Gaebler, J.; Escobar, I.; Saavedra, O.; Domingo, V.; Shibata,
   S.; Akiyama, H.; Takano, M.; Uchino, K.
Bibcode: 1987ICRC....1..277S
Altcode: 1987ICRC...20a.277S
  No abstract at ADS

Title: The solar-terrestrial science programme.
Authors: Wenzel, K. -P.; Domingo, V.; Schmidt, R.
Bibcode: 1987ESABu..50....8W
Altcode:
  The prime objective of the STSP (solar-terrestrial science programme)
  Cornerstone is to attack outstanding scientific problems in solar,
  heliospheric and space plasma physics in a unified and co-ordinated
  manner.

Title: Diffuse gamma-rays with energies greater than
    1×10<SUP>14</SUP>eV observed in the southern hemisphere.
Authors: Suga, K.; Toyoda, Y.; Kamata, K.; Murakami, K.; Lapointe,
   M.; Gaebler, J.; Escobar, I.; Saavedra, O.; Domingo, V.; Shibata,
   S.; Akiyama, H.; Takano, M.; Uchino, K.
Bibcode: 1987ICRC....1..310S
Altcode: 1987ICRC...20a.310S
  The data of extensive air showers with low content of muons and
  hadrons, observed in the period 1964 to 1966 at Mt. Chacaltaya have
  been reanalyzed. The authors try to explain the very high flux.

Title: Ground-based measurements of solar intensity oscillations
Authors: Jimenez, A.; Palle, P. L.; Roca Cortes, T.; Domingo, V.;
   Korzennik, S.
Bibcode: 1987A&A...172..323J
Altcode:
  Ground-based multichannel photometry of integral sunlight has been
  obtained at Izaña (Tenerife) during three months in 1984 with a
  photometer built at ESTEC. Power spectra of solar irradiance variations
  of individual days show power in the 5 min band just above noise at
  a level comparable to the one found from the SMM data (Woodard and
  Hudson, 1983). Previous similar ground work had never achieved the
  signal level required at the 5 min interval. When combining the best
  7 contiguous days of data, the signature of p mode solar oscillations
  spectra appears, but individual identification is difficult due to a
  low signal-to-noise ratio.

Title: Results of the solar constant experiment onboard Spacelab 1.
Authors: Crommelynck, D. A.; Brusa, R. W.; Domingo, V.
Bibcode: 1986SoPh..107....1C
Altcode: 1987SoPh..107....1C
  A cavity type absolute radiometer was flown on Spacelab 1 in
  December 1983. We obtain a value of the solar constant of 1361.5 W
  m<SUP>−2</SUP> with an estimated accuracy of ±2.3 W m<SUP>−2</SUP>
  or 0.17%. When comparing this with other recent determinations,
  we find discrepancies which we consider indicative of metrological
  problems in present day absolute radiometry.

Title: Low-energy particle events and solar filament eruptions
Authors: Sanahuja, B.; Heras, A.; Domingo, V.; Joselyn, J. A.
Bibcode: 1986AdSpR...6f.277S
Altcode: 1986AdSpR...6..277S
  Over the period from August 1978 to October 1982, several large
  low-energy (E &lt; 1.6 Mev) proton events associated with interplanetary
  travelling disturbances observed at 1 AU by ISEE-3, appeared not to be
  triggered by solar flares. Six of them can be associated with filament
  eruptions as the source of the disturbances. We have made a comparative
  study of the particle fluxes in the interplanetary medium, as well as
  of the available H-alpha observations and X-ray and radio emission,
  between these events and those associated with disturbances generated
  by solar flares.

Title: The Ultra Heavy Cosmic Ray Experiment on LDEF-1
Authors: Osullivan, D.; Thompson, A.; Wenzel, K. -P.; Domingo, V.
Bibcode: 1985crhe.work..302O
Altcode:
  The DIAS-ESTEC ultraheavy-cosmic-ray experiment was deployed
  in earth orbit aboard the LDEF by the Space Shuttle on April 6,
  1984. A large-area (12-sq m) solid-state nuclear-track-detector array,
  designed to study the charge spectrum of nuclei with Z = 30 or greater,
  is to remain in orbit until recovery of the LDEF by a second Shuttle
  mission in March 1985. Details of the background to the experiment,
  its astrophysical significance, analysis, and general expectations are
  discussed. The impact of recent results on the registration-temperature
  effect for ultraheavy nuclei on overall charge resolution is assessed.

Title: Solar Irradiance Observations
Authors: Crommelynck, D.; Domingo, V.
Bibcode: 1984Sci...225..180C
Altcode:
  The absolute radiometer on Spacelab 1 was used to obtain solar
  irradiance observations from space. A number of effects must be taken
  into account in the data reduction. A provisional value was obtained
  for the mean solar constant during the observation period (6 to 8
  December 1983).

Title: A high-resolution study of ultra-heavy cosmic-ray nuclei
    (A0178)
Authors: O'Sullivan, D.; Thompson, A.; O'Ceallaigh, C.; Domingo, V.;
   Wenzel, K. P.
Bibcode: 1984ldef.rept..101O
Altcode:
  The main objective of the experiment is a detailed study of the charge
  spectra of ultraheavy cosmic-ray nuclei from zinc (Z = 30) to uranium
  (Z = 92) and beyond using solid-state track detectors. Special emphasis
  will be placed on the relative abundances in the region Z or - 65, which
  is thought to be dominated by r-process nucleosynthesis. Subsidiary
  objectives include the study of the cosmic-ray transiron spectrum a
  search for the postulated long-lived superheavy (SH) nuclei (Z or =
  110), such as (110) SH294, in the contemporary cosmic radiation. The
  motivation behind the search for super-heavy nuclei is based on
  predicted half-lives that are short compared to the age of the Earth
  but long compared to the age of cosmic rays. The detection of such
  nuclei would have far-reaching consequences for nuclear structure
  theory. The sample of ultraheavy nuclei obtained in this experiment
  will provide unique opportunities for many tests concerning element
  nucleosynthesis, cosmic-ray acceleration, and cosmic-ray propagation.

Title: Low-Energy Protons Associated with the 14-18 August 1979 Events
    (smy/stip Event no.
Authors: Sanahuja, B.; Domingo, V.; Wenzel, K. -P.
Bibcode: 1984sii..conf..195S
Altcode:
  No abstract at ADS

Title: Low-Energy Protons Associated with the 4 April 1980 Event
    (smy/stip Event no. 2.)
Authors: Sanahuja, B.; Domingo, V.; Wenzel, K. -P.
Bibcode: 1984sii..conf..229S
Altcode:
  No abstract at ADS

Title: Energetics and Interplanetary Effects of the August 14 and 18,
1979 Solar Flares: Summary of Observations Made during the Smy/stip
    Event no.
Authors: Kane, S. R.; Bird, M. K.; Domingo, V.; Gapper, G. R.; Green,
   G.; Hewish, A.; Howard, R. A.; Iwers, B.; Jackson, B. V.; Koren, U.;
   Kunow, H.; McGuire, R. E.; Muller-Mellin, R.; Rompolt, B.; Sanahuja,
   B.; Sawant, H. S.; Stewart, R. T.; von Rosenvinge, T.; Wibberenz,
   G.; Zlobec, P.
Bibcode: 1984sii..conf..175K
Altcode:
  No abstract at ADS

Title: The L<SUB>1</SUB>-lagrangian point orbit as a suitable site
    for helioseismologic measurements
Authors: Domingo, V.; Wyn-Roberts, D.
Bibcode: 1984MmSAI..55..375D
Altcode:
  The orbit around the Earth - Sun Lagrangian point L<SUB>1</SUB>
  has the advantages of providing continuous solar viewing and
  eliminating the Earth rotation velocity when compared with ground-based
  observations. ESA has completed a study on a spacecraft (DISCO) which
  was to have been placed in this orbit, and is now studying a potential
  solar observatory (SOHO) to be placed in the same orbit. The aims of
  SOHO are the understanding of the solar wind origin and of the heating
  and energy balance of the corona and the investigation of the solar
  interior structure.

Title: An extensive solid state nuclear track detector array for the
    study of ultra heavy cosmic ray nuclei aboard the NASA Long Duration
    ExposureFacility (LDEF).
Authors: Thompson, A.; O'Sullivan, D.; Wenzel, K. -P.; Domingo, V.;
   O'Ceallaigh, C.; Daly, J.; Smit, A.
Bibcode: 1984NTRM....8..575T
Altcode:
  No abstract at ADS

Title: Low-Energy Protons Associated with the Events of 10 April,
    24 April and 8 may 1981 (stip Interval Xii)
Authors: Sanahuja, B.; Domingo, V.
Bibcode: 1984sii..conf..307S
Altcode: 1984STIA...8516082S
  One of the two flares of 10 April 1981 (1117 UT and 1650 UT) and the
  24 April (1400 UT) and 8 May (2232 UT) produced interplanetary shocks
  that were accompanied by a large increase of low-energy protons (35-1600
  keV). An interesting large shock event is observed on 11 April. Although
  the shocks are of very different characteristics, all have the common
  feature that the flow of particles up- and downstream is always from
  the shock, indicating the shock is the main proton acceleration source
  at this energy.

Title: Low-energy protons associated with interplanetary shocks as
    an independent population in the solar wind
Authors: Sanahuja, B.; Domingo, V.
Bibcode: 1984AdSpR...4b.319S
Altcode: 1984AdSpR...4..319S
  We investigate the large scale flow pattern of 36-1600 keV protons
  observed in association with several large interplanetary shocks on
  ISEE-3 between August 1978 and April 1980. The distribution function in
  the solar wind frame and its temperal evolution indicates that these
  particles can behave as a coherent population in the solar wind. This
  population propagates along the magnetic field in the same direction as
  the solar wind flow, ahead of the shock, and in the opposite direction
  after the passage of the perturbed region associated with the shock.

Title: The Ultra Heavy Cosmic Ray Experiments on the NASA Long
    Duration Exposure Facility (ldef)
Authors: O'Sullivan, D.; Thompson, A.; Daly, J.; O'Ceallaigh, C.;
   Wenzel, K. P.; Domingo, V.; Smit, A.
Bibcode: 1983ICRC....9..403O
Altcode: 1983ICRC...18i.403O
  A large array (≅20 m<SUP>2</SUP>sr) of solid state nuclear track
  detectors is being prepared for a twelve month exposure in earth orbit
  aboard the NASA LDEF. The experiment is designed to study the charge
  spectrum of cosmic ray nuclei with Z &gt; 30, particularly of those
  above Z ≡ 70.

Title: The Ultra Heavy Cosmic Ray Experiment on the NASA Long Duration
    Exposure Facility (ldef)
Authors: O'Sullivan, D.; Thompson, A.; Daly, J.; O'Ceallaigh, C.;
   Wenzel, K. P.; Domingo, V.; Smit, A.
Bibcode: 1983ICRC....8..126O
Altcode: 1983ICRC...18h.126O
  The experiment is designed primarily to investigate the charge spectrum
  of cosmic ray nuclei with Z greater than or equal to 30. This is
  to be done by obtaining a larger sample of events than has hitherto
  been possible by balloon or satellite exposures. A very large array
  of solid state nuclear track detectors is to be exposed in space for
  approximately one year. Special emphasis will be placed on the relative
  abundances in the region where Z is greater than or equal to 65, which
  is thought to be dominated by r-process nucleosynthesis. Among the
  subsidiary objectives of the experiment are the study of the cosmic
  ray transition spectrum and a search for the postulated long-lived
  superheavy nucley (Z greater than or equal to 110) in the contemporary
  cosmic radiation. It is noted that the search for super-heavy nuclei
  is based on predicted half-lives that are short in comparison with
  the age of the earth but long in comparison with the age of cosmic
  rays. The far-reaching consequences for nuclear structure theory that
  the detection of such nuclei would have are noted.

Title: Report on the scientific satellites of the European Space
    Agency
Authors: Burke, W. R.; Bennett, K.; Benvenuti, P.; Domingo, V.; Emery,
   R. J.; de Graauw, T.; Knott, K.; Macchetto, F.; Marsden, R. G.; Page,
   D. E.
Bibcode: 1983STIN...8332831B
Altcode:
  The missions and status of Cos-B Geos 1 and 2, ISEE, and IUE are
  outlined. The first Spacelab payload; EXOSAT; and the International
  Solar Polar Mission are described. The ESA contribution to the Space
  Telescope program; the Hipparcos astrometry program; the Giotto Halley's
  Comet mission; and the Infrared Space Observatory project are described.

Title: A Large Proton Event Associated with Solar Filament Activity
Authors: Sanahuja, B.; Domingo, V.; Wenzel, K. -P.; Joselyn, J. A.;
   Keppler, E.
Bibcode: 1983SoPh...84..321S
Altcode:
  We report observations made from several interplanetary spacecraft,
  of the large low-energy particle event of 23-27 April, 1979 associated
  with solar filament activity. We discuss the intensity, spectral and
  directional evolution of the event as observed in the energy range
  35-1600 keV on ISEE-3, located ∼ 0.99 AU from the Sun upstream of
  the Earth. We demonstrate that the shock disturbance propagating
  through the interplanetary medium and observed at ISEE-3 on 24/25
  April strongly controls the particle event. From a comparison of the
  ISEE-3 observations with those on other spacecraft, in particular on
  Helios-2, located at 0.41 AU heliocentric distance near the Sun-Earth
  line, we identify the solar filament erupting on late 22 April near
  central meridian as the trigger for the propagating shock disturbance.

Title: La magnetosfera terrestre. Un acelerador de partículas
    cargadas.
Authors: Domingo, V.
Bibcode: 1983POEM...14...83D
Altcode:
  No abstract at ADS

Title: Energetics and interplanetary effects of the August 14 and 18,
    1979 solar flares
Authors: Kane, S. R.; Bird, M. K.; Domingo, V.; Green, G.; Gapper,
   G. R.; Hewish, A.; Howard, R. A.; Iwers, B.; Jackson, B. V.; Koren, U.
Bibcode: 1983STIN...8329164K
Altcode:
  The STIP Event No. 1, which covered the time interval August 14 - 18,
  1979, was characterized by two energetic flares: one on August 14
  (approximately 1243 UT) and the other on August 18 (approximately
  1400 UT). The hard X-ray, soft X-ray, optical, radio and energetic
  particle emissions from these flares and their interplanetary effects
  were observed with many instruments in space and on the ground. A
  summary of some of these observations is presented. The results of
  a preliminary analysis relevant to the acceleration of particles,
  coronal transients and evolution of shocks are as follows: (1) During
  the August 14 flare energetic particles were probably accelerated
  but could not escape the Sun in large numbers. On the other hand,
  during the August 18 flare the acceleration of high energy particles
  occurred relatively high in the corona, from whence they could easily
  escape into interplanetary space but could not penetrate down to the
  lower altitudes in the solar atmosphere in large numbers. (2) The
  kinetic energy of the coronal transient associated with the August 14
  flare was much larger than the total energy of energetic electrons,
  indicating an additional energy source for the transient. (3) The shock
  associated with the August 18 flare extended to greater than 2 (3.14)
  steradians. The shock maintained its speed from the flare site to a
  distance of approximately 35 R and then decelerated to a distance of
  approximately 1 AU as approximately R to the minus 0.8 power.

Title: Disco - a solar-seismology and heliospheric-structure
    observatory.
Authors: Domingo, V.
Bibcode: 1982ESABu..32...16D
Altcode:
  No abstract at ADS

Title: Consequences of solar-related processes on the earth's
    environment and man's devices.
Authors: Gendrin, R.; Domingo, V.
Bibcode: 1982sspf.conf...71G
Altcode:
  No abstract at ADS

Title: Consequences of solar-related processes on the Earth's
    environment and man's devices
Authors: Gendrin, R.; Domingo, V.
Bibcode: 1982AdSpR...2a..71G
Altcode: 1982AdSpR...2...71G
  The effects of solar disturbances on the earth environment and on
  anthropogenic systems and devices are discussed. Attention is given
  to solar cosmic ray effects on the atmosphere, which may produce
  an increase in D region electron density giving rise to polar cap
  absorption events, modulations of galactic cosmic ray flux affecting
  atmospheric electric fields, and solar wind-ionosphere coupling which
  may exert an influence on terrestrial meteorology. Solar wind effects
  on the magnetosphere-ionosphere-atmosphere system as evidenced by the
  auroral electrojet, magnetospheric substorms and auroral heating are
  then considered in relation to their consequences for large, conducting
  man-made systems and geomagnetic surveys at high latitudes, spacecraft
  charging and performance and satellite lifetimes. The effects of human
  activities, both scientific and industrial, on the magnetosphere are
  also pointed out.

Title: The Solar Grazing Incidence / GRIST / and Optical / SOT =
    Solar Optical Telescope / Joint Accommodations
Authors: Domingo, V.
Bibcode: 1981SSRv...29..327D
Altcode:
  Some of the problems foreseen for the joint accommodation and operation
  of the Grazing Incidence Solar Telescope (GRIST) under study by ESA to
  operate in the extreme ultraviolet region (90 &lt; λ &lt; 1700 Å),
  and the Solar Optical Telescope (SOT), developed by NASA to operate
  in the ultraviolet, optical and infrared region (A &gt; 1100 Å)
  on a Spacelab mission are described.

Title: Physics of solar variations
Authors: Domingo, V.
Bibcode: 1981SoPh...74.....D
Altcode:
  Topics discussed include the sun (structure, oscillations, magnetic
  cycle, surface variations), solar radiation, solar radiation effects in
  the earth's atmosphere, long-term variations (climate and paleoclimate),
  and instrumentation. Papers are presented on short-period intensity
  fluctuations of integral sunlight, on the theory of the solar cycle,
  and on the nonsymmetric solar dynamo. Attention is also given to
  solar radiation and its variation in time, to the effects of solar
  variations on the upper atmosphere, and to the role of space techniques
  in understanding solar variability.

Title: Introduction - Physics of Solar Variations
Authors: Domingo, V.
Bibcode: 1981SoPh...74....7D
Altcode:
  No abstract at ADS

Title: On the location of the source for the energetic electron layer
    at the polar magnetopause and its relation to magnetic reconnection
Authors: Formisano, V.; Domingo, V.; Wenzel, K. -P.
Bibcode: 1981JGR....86.4579F
Altcode:
  The existence of a layer of energetic (&gt;20 keV) electrons
  along the magnetopause, extending from the polar cusp region to the
  distant magnetotail, has been established by measurements on various
  spacecraft. We have performed a statistical study of electron flux
  and spectral measurements above 0.5 MeV observed in different regions
  of the magnetopause accessible to HEOS 2, with the aim of identifying
  the source for this magnetopause electron layer. The measurements along
  the polar magnetotail (i. e., adjacent to the plasma mantle), along the
  mid-latitude dayside magnetopause (i.e.,adjacent to the dayside plasma
  boundary layer), and on both sides of the magnetosheath/polar cusp
  interface (i.e., in the exterior polar cusp and in the entry layer) have
  been separately analyzed and are statistically compared. We conclude
  that escape of electrons from the magnetosphere can be excluded as a
  significant source for the tail magnetopause layer on the basis of the
  observed intensities, of the spectra, and of the frequency of appearance
  of electrons outside those magnetopause regions which lie adjacent to
  the outer trapping zone. The electron intensities in the exterior polar
  cusp region are found to be correlated with the north/south component
  of the interplanetary magnetic field (IMF). High intensity levels
  are observed when the IMF is directed southward (B<SUB>z</SUB>&lt;0),
  and low levels when the IMF points northward (B<SUB>z</SUB>&gt;0). The
  electron flux in the exterior cusp region at times of southward IMF
  and at the near-earth polar magnetotail at times of northward IMF
  is well correlated with the number of field lines carried by the
  solar wind towards the magnetosphere (expressed by the product of
  solar wind speed and interplanetary field magnitude). We interpret
  this as strong evidence that acceleration processes associated with
  magnetic reconnection occur at the magnetopause at those times. Local
  acceleration near the high-latitude magnetopause appears therefore to
  be a prime source for the magnetopause electron layer.

Title: Non-Flare Injection of Protons Into Interplanetary Space
Authors: Domingo, V.; Sanahuja, B.; Wenzel, K. -P.
Bibcode: 1981ICRC....3..109D
Altcode: 1981ICRC...17c.109D
  The superimposition of a second proton population associated with a
  solar wind regime, and bounded by a pair of shocks, is found to be
  superimposed upon the first in an investigation of 35-1600 KeV solar
  protons observed during an April, 1979 nonflare event by ISEE-3. The
  source of the particles and the solar wind regime appear to be closely
  associated with intense solar filament activity near the central
  meridian. The temporal evolution of velocity spectra and anisotropy
  distributions during this period are discussed.

Title: Anisotropy Characteristics of Upstream Proton Events
Authors: Sanderson, T. R.; Domingo, V.; Reinhard, R.; Wenzel, K. -P.
Bibcode: 1981ICRC....3..483S
Altcode: 1981ICRC...17c.483S
  Results are presented of a detailed analysis of proton anisotropies
  observed during an upstream event when ISEE-3 was approximately
  80 earth radii upstream from the earth, and close to the sun-earth
  radial. During the first part of the event, particles were observed
  streaming mainly from the direction of the earth along the magnetic
  field. Later in the event, the angular distributions broadened until
  towards the end of the event, approximately equal intensities were
  observed with pitch angles from 0 deg up to 120 deg, with essentially
  no particles with pitch angles close to 180 deg. (Here a 0 deg pitch
  angle particle is defined as a particle moving upstream along the
  magnetic field.) Large amplitude low-frequency waves were observed
  in the magnetic field at ISEE-3 whenever enhanced fluxes of 90 deg
  protons were observed. It is argued that the 90 deg protons are the
  result of pitch angle scattering of the upstream moving protons in
  the region between the bow shock and ISEE-3.

Title: Propagation of upstream protons in the near-earth solar wind
Authors: Domingo, V.; Sanderson, T. R.; Wenzel, K. -P.
Bibcode: 1981AdSpR...1c.125D
Altcode: 1981AdSpR...1..125D
  The propagation of energetic protons (35-1600 keV) from the Earth's
  magnetosphere to the ISEE-3 spacecraft located about 240 earth radii
  (R<SUB>E</SUB>) upstream in the solar wind is used as a tool to study
  the interaction between these protons and the solar wind. In this
  preliminary study we present proton pitch angle distributions seen at
  different times during the development of upstream events that occur
  in relatively quiet interplanetary conditions. In general a highly
  anisotropic sunward flow is seen at the beginning of the events. During
  the course of the events pitch angle distributions may vary between
  streaming along the field lines (peaked around 0° pitch angle),
  a uniform intensity between 0° and 90°, and a peaked distribution
  around a preferred pitch angle that is often near 90°.

Title: Propagation of upstream protons in near-earth solar wind.
Authors: Domingo, V.; Sanderson, T. R.; Wenzel, K. -P.
Bibcode: 1981crh..conf..125D
Altcode:
  No abstract at ADS

Title: Control of Energetic Particle Flows by the Interplanetary
    Magnetic Field Structure
Authors: Reinhard, R.; Formisano, V.; Wenzel, K. P.; Domingo, V.
Bibcode: 1981sowi.conf..490R
Altcode:
  No abstract at ADS

Title: Intensity Decay Patterns for Proton Particle Increases
    Associated with Interplanetary Shock Waves
Authors: Hynds, R. J.; Domingo, V.
Bibcode: 1981ICRC....3..447H
Altcode: 1981ICRC...17c.447H
  At 1 AU the passage of interplanetary shock waves is associated with
  long-time, constant increases in intensity of low energy protons,
  called Energetic Storm Particle (ESP) events. The characteristc
  pattern involves an initial rise in particle intensity up to 12
  hours prior to the passage of the shock; the intensity peaks at or
  near the shock front, followed by a relative smooth decay after the
  passage of the shock. For protons of energies less than or equal to
  30 keV, the intensity decay after the passage of the shock can show
  considerable variation. The particle data are compared to interplanetary
  magnetic field and solar wind data, showing that these abrupt changes
  in intensity are associated with interplanetary plasma and field
  conditions. Data from the Energetic Proton Anisotropy Spectrometer
  on the ISEE-3 spacecraft is used to investigate a typical ESP event
  (February 17-23, 1979).

Title: Prediction of energetic particle disturbances
Authors: Paulikas, G. A.; Baker, D. N.; Barron, W. R.; Domingo, V.;
   Higbie, P. R.; Imhof, W. L.; Lyons, L. R.; McPherron, R. L.; Roelof,
   E. C.; Scholer, M.
Bibcode: 1979stp.....2..415P
Altcode:
  The prediction of fluxes of energetic particles of solar or
  magnetospheric origin is addressed. Topics include the prediction of
  the properties of the particle populations generated by magnetospheric
  storms and substorms, and the prediction of long term variations in
  the populations of magnetospheric particles.

Title: Energetic Electrons in the Cusp and in the High Latitude
    Plasma Sheet - Evidence for Source Regions
Authors: Formisano, V.; Domingo, V.
Bibcode: 1979P&SS...27.1479F
Altcode:
  HEOS-2 has observed energetic electrons (&gt; 40 keV) in the high
  latitude magnetosphere appearing as one or more peaks outside
  and often well separated from the trapping boundary. Most of the
  observations are between 70° and 80° invariant latitudes both in
  the day and nightside. The peaks are located in the dayside adjacent
  to the polar cusp and coincide in the nightside with the edge of the
  plasma sheet. The electron peak intensity on the nightside shows a
  clear correlation with AE. The electron peak intensities on the dayside
  exceed those on the nightside and are generally higher in the pre-noon
  than in the afternoon sector. Observations on the dayside in the distant
  cusp region and in the adjacent magnetosheath show high and fluctuating
  intensities of energetic electronswith an energy spectrum much harder
  than in the outermost trapping region. This observational evidence
  suggests different source regions for these energetic electrons: one
  in the distant geomagnetic tail and another one around the dayside
  cusp indentation.

Title: The three-dimensional shape of the magnetopause
Authors: Formisano, V.; Domingo, V.; Wenzel, K. -P.
Bibcode: 1979P&SS...27.1137F
Altcode:
  Nearly 1000 magnetopause crossings from HEOS-2, HEOS-1, OGO-5 and 5
  IMP space-craft covering most of the northern and part of the southern
  dayside and near-Earth tail magnetopause ( X &gt;-15 R<SUB>E</SUB>) have
  been used to perform a detailed study of the three-dimensional shape
  and location of the magnetopause. The long-term influence of the solar
  wind conditions on the average magnetopause geometry has been reduced by
  normalising the radial distances of the observed magnetopause crossings
  to an average dynamical solar wind pressure. Best-fit ellipsoids
  have been obtained to represent the average magnetopause surface in
  geocentric solar ecliptic (GSE) and (as a function of tilt angle) in
  solar magnetic (SM) coordinates. Average geocentric distances to the
  magnetopause for the 1972-1973 solar wind conditions (density 9.4 cm
  <SUP>-3</SUP>, velocity 450 km s <SUP>-1</SUP>) are 8.8 R<SUB>E</SUB>
  in the sunward direction, 14.7 R<SUB>E</SUB> in the dusk direction,
  13.4 R<SUB>E</SUB> in the dawn direction and 13.7 R<SUB>E</SUB> in
  the direction normal to the ecliptic plane. The magnetopause surface
  is tilted by 6.6° ± 2° in a direction consistent with that expected
  from the aberration effect of the radial solar wind. Our data suggest
  that the solar wind plasma density and the interplanetary magnetic
  field (IMF) orientation affect the distance to the polar magnetopause,
  larger distances corresponding to higher plasma density and southward
  fields. Our best-fit magnetopause surface shows larger geocentric
  distances than predicted by the model of Choe et al. [ Planet Space
  Sci. 21, 485 (1973).] normalised to the same solar wind pressure.

Title: Total Solar Energy Output and its Measurement
Authors: Domingo, V.
Bibcode: 1979BAAS...11..423D
Altcode:
  No abstract at ADS

Title: Total solar energy output and its measurement.
Authors: Domingo, V.
Bibcode: 1979BAAS...11..422D
Altcode:
  No abstract at ADS

Title: Magnetospheric Bursts at Proton Energies above 35 KEV. Observed
    from the ISEE-3 Spacecraft
Authors: Hynds, R. J.; Balogh, A.; Domingo, V.; Wenzel, K. -P.
Bibcode: 1979ICRC....3..154H
Altcode: 1979ICRC...16c.154H
  No abstract at ADS

Title: a High Resolution Study of Ultra Heavy Cosmic Ray Nuclei
    Using the Long Duration Exposure Facility (ldef)
Authors: Thompson, A.; O'Sullivan, D.; Daly, J.; O'Ceallaigh, C.;
   Domingo, V.; Smit, A.; Wenzel, K. -P.
Bibcode: 1979ICRC...11..103T
Altcode: 1980ICRC...11..103T; 1979ICRC...16k.103T
  A large array of nuclear track detectors is being prepared for a
  twelve month exposure in space aboard the LDEF which is scheduled to be
  launched by the NASA Space Shuttle in 1981. The experiment is designed
  to study the charge spectrum of cosmic ray nuclei with Z greater than
  30 by obtaining a large and more uniform sample of events than has
  hitherto been possible by balloon or satellite exposures. A summary
  of the astrophysical significance of the experiment and its current
  state of development is given.

Title: a Solar Proton Event of Possible Non-Flare Origin
Authors: Domingo, V.; Hynds, R. J.; Stevens, G.
Bibcode: 1979ICRC....5..192D
Altcode: 1979ICRC...16e.192D; 1980ICRC....5..192D
  The sun showed little activity in the period August 18-23, 1978. A
  filament, near central meridian passage, disappeared at approximately
  0120 U.T. on August 23, with a SSC recorded at earth at 0247 U.T. on
  August 27 that appears to be associated with it. On August 25, the
  low-energy proton detector on board the ISEE-3 spacecraft detected a
  particle increase which commenced prior to mid-day, and lasted until
  about 1730 U.T. on August 27. Data for the event are displayed and
  the possible origin of the particles is discussed.

Title: Rigidity-independent coronal propagation and escape of solar
    protons and α particles
Authors: Perron, C.; Domingo, V.; Reinhard, R.; Wenzel, K. -P.
Bibcode: 1978JGR....83.2017P
Altcode:
  A statistical study of 42 solar proton and α particle events has been
  performed in the energy range of 9-36MeV/nucleon (nuc) as measured by
  the Space Science Department/European Space Agency experiment on Heos 2
  during 1972-1974. From one event to another there is a high variability
  of the p/α ratio at equal energy per nucleon ranging from about 4
  to 1000 at 10 MeV/nuc. It is found that the lower value of the p/α
  ratios increases with azimuthal distance from the flare site. We show
  that this is not the result of rigidity-dependent coronal processes but
  that the increase follows rather as a consequence of two observations:
  (1) the p/α ratio is correlated with the size of the particle
  event (Van Hollebeke, 1975) and (2) the number of observed particle
  events decreases to the east as is found by numerous authors. A model
  calculation based on these observations is in good agreement with the
  data. The conclusion of rigidity-independent coronal propagation and
  escape also follows from other observations. First, the p/α ratios
  simultaneously measured by the University of Chicago experiment on
  board Pioneer 10 and 11, which have different connection longitudes, are
  generally the same as the Heos 2 values. Second, no systematic variation
  of the p/α ratio is found for the few cases of large individual events,
  when the p/α ratio can be followed over an extended time period, i.e.,
  over an extended range of connection longitudes. Third, the proton
  and α particle spectral exponents show no systematic variation with
  heliolongitude. It is concluded that the observed large variations of
  the p/α ratio from event to event are essentially due to different
  acceleration or storage conditons at the flare site.

Title: Where do charged particles enter in and exit from the
    magnetosphere? Some HEOS-2 measurements.
Authors: Domingo, V.; Page, D. E.; Wenzel, K. -P.
Bibcode: 1978JATP...40..279D
Altcode:
  The orbit of HEOS-2 through the northern polar magnetosphere was such
  that it was possible to monitor the motion of solar protons at the
  polar magnetopause and across the geomagnetic tail. The large-particle
  intensity was found to increase as the magnetopause was approached. The
  inner magnetosphere appears to be partially shielded by the magnetopause
  from solar particles. The characteristics of an essentially permanent
  layer of energetic and relativistic electrons were also monitored
  by HEOS-2. This layer was detected in about 90% of the orbits over a
  period of 25 months. It was located at or around the magnetopause. The
  electron intensity in the magnetopause spike seems to fall off with
  distance along the tail away from the earth. This is consistent with
  the idea that the electrons originate near the earth.

Title: On the mechanism of plasma penetration and energetic electron
    escape across the dayside magnetopause.
Authors: Formisano, V.; Domingo, V.; Wenzel, K. -P.
Bibcode: 1978JATP...40..293F
Altcode:
  A statistical study of correlated observations of plasma, energetic
  (above 40 keV) electrons and magnetic fields on HEOS-2 in the outer
  dayside magnetosphere and magnetosheath has been performed. It is found
  that on the dayside magnetosphere the occurrence of plasma inside
  the magnetopause is anticorrelated with the appearance of energetic
  electrons in the magnetosheath. A mechanism is derived that attempts
  to explain how plasma may penetrate across the magnetopause into the
  magnetosphere and how energetic electrons may escape from the (pseudo)
  trapping region in the dayside magnetosphere into the magnetosheath. The
  mechanism is an E X B drift across the magnetopause. The drift is
  directed inward or outward depending on the direction of the electric
  field at the magnetopause.

Title: Interplanetary magnetic field and geomagnetic activity.
Authors: Domingo, V.
Bibcode: 1978spre.conf..325D
Altcode: 1978spre.proc..325D
  The interaction between the interplanetary magnetic field (IMF) and the
  geomagnetic field is investigated using a compilation of 34,670 hr of
  data on IMF and solar-wind parameters, as well as the Kp index as an
  indicator of geomagnetic activity. Correlations between geomagnetic
  activity and solar-wind parameters are analyzed, and it is found that
  geomagnetic activity is apparently only indirectly related to the
  interaction between the IMF and the geomagnetic field. The results
  indicate that the interaction between the geomagnetic field and the
  IMF dominates the solar-wind interaction with the magnetosphere, is
  governed by folding of the IMF lines of force around the magnetosphere,
  and extends throughout the magnetopause.

Title: Energetic electrons in the outer magnetosphere at mid to
    high latitudes
Authors: Domingo, V.; Wenzel, K. -P.
Bibcode: 1978spre.conf..313D
Altcode: 1978spre.proc..313D
  Results are reported for coordinated HEOS 2 electron and magnetic-field
  observations in the zone of unstable (variable) radiation at middle
  to high latitudes in the northern magnetosphere. The observations
  are discussed in terms of dayside closed field lines, the flanks of
  the magnetotail, and the distribution of variable electron fluxes
  observed in the outer magnetosphere. It is found that: (1) the
  electron population of the dayside pseudotrapping region extends out
  to the magnetopause at medium and high latitudes; (2) in the flanks
  of the magnetotail the electron population extends to high latitudes
  along the horns discovered at low latitudes by Frank et al. (1963);
  (3) the horn on the morning side appears to be populated by higher
  electron intensities and to extend to higher latitudes than that on
  the evening side; and (4) the electron fluxes in the flanks of the
  magnetotail appear to be a continuation of those encountered in the
  dayside pseudotrapping region and exhibit properties similar to those
  observed for electrons encountered in the magnetopause electron layer
  and in the magnetosheath.

Title: Influence of the magnetosheath on solar proton penetration
    into the magnetosphere
Authors: Domingo, V.; Wenzel, K. -P.
Bibcode: 1977P&SS...25.1111D
Altcode:
  The observation of solar protons (1-9 MeV) aboard HEOS-2 in the
  high-latitude magnetotail and magnetosheath on 9 June 1972, and their
  comparison with simultaneous measurements on Explorers 41 and 43,
  both in interplanetary space, indicate the existence of a distinct
  region of the inner magnetosheath (about 3 Earth radii thick) near the
  high-latitude magnetopause in which the solar particle flow is almost
  reversed with respect to the flow observed in interplanetary space. The
  region can also be seen by comparing magnetic field measurements on the
  three spacecraft. The observations in the outer layer of the magnetotail
  show solar protons predominantly entering the magnetosphere somewhere
  near the Earth, perhaps the cusp region.

Title: Energetic and relativistic electrons near the polar
    magnetopause
Authors: Domingo, V.; Page, D. E.; Wenzel, K. -P.
Bibcode: 1977JGR....82.2327D
Altcode:
  More than 2 years of Heos 2 observations in the high-latitude outer
  magnetosphere and magnetosheath have confirmed the presence of a
  layer of energetic and relativistic electrons near the polar tail
  magnetopause. This layer, appearing as ‘electron spike’ on almost
  every magnetopause crossing, contains electrons over a wide range of
  energies up to relativistic energies of &gt;2 MeV. Their differential
  energy spectrum, if fitted by a power law, has an average spectral
  index between 3 and 4.5. The spikes are typically 1-2 R<SUB>E</SUB> wide
  extending more into the magnetosheath than into the magnetosphere. The
  electron intensity in the magnetopause layer decreases with distance
  along the tail, away from the polar cusp, and increases with increasing
  Kp values. It tends to be higher when the magnetosheath field is
  parallel or antiparallel to the tail magnetic field. In many cases
  the magnetopause spikes are accompanied by spikes in the magnetosheath
  which often follow closely the fluctuations of the magnetosheath field
  direction and/or intensity. A map of the average electron distribution
  in the polar magnetosphere and magnetosheath is presented.

Title: Interplanetary magnetic field and geomagnetic activity
Authors: Domingo, V.
Bibcode: 1977IA&A...29...11D
Altcode:
  A vectorial treatment of the geomagnetic field and interplanetary
  magnetic field (IMF) is attempted with the object of shedding light
  on interaction between the fields. Advantages and drawbacks of the
  three-hour planetary index Kp are considered; the Kp is relied upon
  in the analysis. Data referable to nearly 35,000 hours during which
  the velocity of the fields were observable are considered. The kinetic
  effects of the solar wind perceived in terms of solar wind velocity are
  found independent of electromagnetic effects. The interaction between
  the IMF and the geomagnetic field is found maximized when the fields
  are antiparallel in the equatorial zone and minimized when the angle
  formed between them is in the 30-50 deg range, and is an increasing
  function of the intensity of the IMF.

Title: The March 5, 1972 Solar Event: Coronal Control of Particle
    Release
Authors: Reinhard, R.; Domingo, V.; Perron, C.; Wenzel, K. -P.
Bibcode: 1977ICRC....5..107R
Altcode: 1978ICRC....5..107R; 1977ICRC...15e.107R
  The time-intensity profiles of 1-9-MeV and 9-36-MeV protons observed
  by the ESA/SSD detector system on HEOS 2 during the March 5, 1972,
  event display a number of unusual features. The most prominent is a
  plateaulike peak lasting for almost a day. When mapping the particle
  fluxes back to the sun, it is seen that the plateau is caused by a
  large chromospheric polarity cell which is 60 to 100 deg away from
  the acceleration region and uniformly populated with particles. A
  short-lived (3 h) particle intensity increase with strong sunward flow
  is observed during the decay phase and tentatively associated with a
  magnetic loop-type structure in the interplanetary medium.

Title: Rigidity Independent Coronal Propagation and Escape of Solar
    Protons and Alpha Particles
Authors: Perron, C.; Domingo, V.; Reinhard, R.; Wenzel, K. -P.
Bibcode: 1977ICRC....5..113P
Altcode: 1977ICRC...15e.113P
  No abstract at ADS

Title: Generation and propagation of charged particles in the solar
    event of 22 July 1972.
Authors: Morosova, E. I.; Pisarenko, N. F.; Volodichev, N. N.; Kolesov,
   G. Ia.; Kurt, V. G.; Domingo, V.; Page, D. E.; Wenzel, K. -P.; Smerd,
   S. F.
Bibcode: 1976spre.conf..775M
Altcode: 1976spre.proc..775M
  The increase of charged particles, protons with energies up to 500 MeV
  and electrons up to about 3.5 MeV, in the solar event on 22 July 1972
  is examined. The analysis of the data on the anisotropy of the charged
  particles, radio and X-ray observations, and the absence of an optical
  flare lead to the conclusion that the increase is associated with
  a sympathetic flare in the active region McMath 11958. The powerful
  shock wave from the flare, which occurred behind the limb apparently
  in the active region McMath 11976, moving along the sun's surface was
  the agent which caused this flare. The capture of some of the flare
  particles by a trap near the sun led to the possibility of their
  prolonged escape into the interplanetary space.

Title: Experimental evidence for solar protons following paths
    determined by solar wind flow regimes.
Authors: Wenzel, K. -P.; Domingo, V.; Page, D. E.
Bibcode: 1976spre.conf..719W
Altcode: 1976spre.proc..719W
  Experimental results are presented from the solar particle, plasma and
  magnetometer experiments on HEOS 2 indicating that solar protons are
  constrained to discrete solar wind flow regimes and only with difficulty
  move across magnetic field lines to neighboring regimes. An outstanding
  example was the period of 29 October-2 November 1972, during which time
  HEOS 2 appeared to remain close to a solar wind boundary lying roughly
  parallel to the ecliptic plane. Another example of proton collimation
  in solar wind regimes was observed during 3-5 November 1973.

Title: October 1972 solar event: The third dimension in solar
    particle propagation
Authors: Domingo, V.; Page, D. E.; Wenzel, K. -P.
Bibcode: 1976JGR....81...43D
Altcode:
  From late on October 29 until November 3, 1972, our experiment on
  the European Space Research Organization satellite Heos 2 recorded
  the arrival of an enhanced interplanetary particle intensity. A
  dramatic ‘slot’ in count rate and other sudden anisotropy and
  flux changes (measured in and perpendicular to the ecliptic plane)
  were found to coincide with changes in the θ (north-south) ecliptic
  direction of the interplanetary magnetic field. However, reorientation
  of strongly field-aligned particle distributions relative to the
  detectors was insufficient to explain the intensity changes recorded,
  and the conclusion had to be drawn that the spacecraft was repeatedly
  crossing a boundary between one regime and a neighboring one with a
  different particle population. Since the switching from one regime
  to the other continued for several days, it would seem reasonable to
  suggest that the boundary between regimes was roughly parallel to the
  ecliptic plane. This idea was reinforced by the discovery that each
  time that the particle regime changed, not only did B<SUB>θ</SUB>
  change, but the solar wind flow direction changed, the dip angle
  reversing sign. It would thus appear that when the solar wind blows
  three-dimensional snakelike tubes in interplanetary space, MeV
  particles obediently follow the field line bundles within such tubes
  and experience considerable difficulty in crossing from one tube to
  a neighboring tube which encloses a different regime. Because of the
  absence of cross-field particle movement, measurements made at higher
  solar latitudes, where most solar active regions occur, could reveal a
  somewhat different picture of the development of solar particle events.

Title: Solar Radiation Variation and Climate
Authors: Domingo, V.
Bibcode: 1976ASSL...61...21D
Altcode: 1976aps..conf...21D
  No abstract at ADS

Title: Multisatellite observations of solar protons penetrating
    the magnetopause.
Authors: Domingo, V.; Page, D. E.; Wenzel, K. -P.
Bibcode: 1976ASSL...57..225D
Altcode:
  Simultaneous observations of low-energy solar protons (1-40 MeV)
  by HEOS-2 in the northern high-latitude magnetotail and by other
  spacecraft in interplanetary space during the solar proton event of
  June 8, 1972 are presented. The results indicate that solar protons
  enter that magnetotail lobe which is not well connected to the
  interplanetary magnetic field - with respect to solar-particle entry -
  preferentially close to the earth rather than farther downtail. The
  particle density gradients measured in the tail lobe suggest that
  the particles enter there not only across the polar magnetopause,
  but also from the neutral sheet.

Title: On the Propagation of Low Energy Solar Protons in the
    Interplanetary Medium
Authors: Amata, E.; Domingo, V.; Page, D. E.; Wenzel, K. P.
Bibcode: 1975ICRC....5.1761A
Altcode: 1975ICRC...14.1761A
  The fluxes and anisotropies of low energy solar protons (less
  than 10 MeV) observed on two occasions when the HEOS-2 spacecraft
  encountered solar proton streams are studied taking into account the
  interplanetary magnetic field and plasma conditions existing at those
  times. (Plasma and magnetic field measurements are available from
  the same satellite). The variations in the streaming pattern are used
  to infer the topological structure of the interplanetary medium. The
  observed results are compared to existing models of particle propagation
  between the sun and the earth.

Title: Das solare Ereignis vom 29. Oktober 1972: MeV Protonen,
    Alphateilchen und Elektronen
Authors: Wenzel, K. -P.; Domingo, V.; Page, D. E.
Bibcode: 1974MitAG..35..266W
Altcode:
  No abstract at ADS

Title: MeV Electrons, Protons and Alpha Particles Observed August
    2-12 1972
Authors: Page, D. E.; Domingo, V.; Wenzel, K. -P.
Bibcode: 1974ASSL...42..573P
Altcode: 1974cimo.symp..573P
  An experiment was conducted on the ESRO satellite HEOS2 to monitor
  electrons, protons, and alpha-particles during specific solar particle
  events. Time constants of the decay and the anisotropies observed
  for different particle species were studied. Information was obtained
  concerning the interplanetary conditions. The conclusions derived from
  early particle data were in good agreement with more recent directly
  measured interplanetary data.

Title: Energetic Electrons at the Magnetopause
Authors: Domingo, V.; Page, D. E.; Wenzel, K. -P.
Bibcode: 1974ASSL...42..159D
Altcode: 1974cimo.symp..159D
  Results of observations of energetic and relativistic electrons made by
  the highly ecentric ESRO satellite HEOS 2 near the high-latitude tail
  magnetopause. There is generally a particle layer near the magnetopause,
  containing electrons up to about 1 MeV. The particle intensity shows
  a clear dependence on geomagnetic activity.

Title: Measurements of Solar Protons in the Near Earth Magnetotail
Authors: Domingo, V.; Page, D. E.; Wenzel, K. -P.
Bibcode: 1974ASSL...42..507D
Altcode: 1974cimo.symp..507D
  Preliminary results of the measurement of protons in the high latitude
  magnetosphere using the HEOS2 spin stabilized spacecraft. Data were
  obtained from the front solid state detector in anticoincidence with
  the back detector and the scintillator. The detector was operated
  on an angular mode while the channel measured protons of 1 to 9 MeV
  and electrons of about 0.4 to 0.6 MeV. Results indicated that the
  anisotropy measurement in the near earth magnetotail for protons of
  about 1 MeV showed a reasonable gradient of fluxes present in it. It
  is possible to use this measurement to map the penetration of protons
  into the polar cap.

Title: Solar particle penetration through the magnetosheath
Authors: Domingo, V.; Page, D. E.; Wenzel, K. -P.
Bibcode: 1974stp.....2...96D
Altcode:
  Data from HEOS-2 and from the NOAA experiment on Explorer 41 are
  presented which demonstrate that often the bow shock and magnetosheath
  seriously distort the flux of 1-MeV solar particles, so that it is no
  longer valid to assume that the magnetopause is the boundary between the
  interplanetary medium and the magnetotail. The change in absolute value
  and direction of the flux of particles that might be expected to occur
  at the magnetopause is not always seen exactly at that point. Rather,
  this change occurs sometimes further away in the magnetosheath, and
  sometimes the magnetopause looks completely transparent to arriving
  energetic particles as if the magnetotail were a continuation of the
  magnetosheath.

Title: Magnetosheath observations at high northern latitudes by Heos 2
Authors: Hedgecock, P. C.; Cerulli, P.; Coletti, A.; Egidi, A.;
   Marconero, R.; Domingo, V.; Köhn, D.; Page, D. E.; Taylor, B. G.;
   Wenzel, K. -P.
Bibcode: 1973JGR....78.1715H
Altcode:
  No abstract at ADS

Title: The April 17/18, 1972 Solar Event: Spectral and Directional
    Measurements of Protons, Alpha-Particles, and Electrons. (Abstract)
Authors: Wenzel, K. -P.; Domingo, V.; Page, D. E.; Taylor, B. G.
Bibcode: 1973ICRC....2.1438W
Altcode: 1973ICRC...13.1438W
  No abstract at ADS

Title: The April 17/18, 1972 Solar Event: Spectral and Directional
    Measurements of Protons, Alpha-Particles, and Electrons
Authors: Wenzel, K. P.; Domingo, V.; Page, D. E.; Taylor, B. G.
Bibcode: 1973ICRC....5.3151W
Altcode: 1973ICRC...13.3151W
  No abstract at ADS

Title: High energy electrons at the magnetopause above the north
    pole. Preliminary results from the HEOS 2 satellite.
Authors: Page, D. E.; Domingo, V.; Köhn, D.; Taylor, B. G.; Wenzel,
   K. -P.; Hedgecock, P. C.
Bibcode: 1973spre.conf..631P
Altcode: 1973spre....2..631P
  No abstract at ADS

Title: Northern Polar Cap Particle Flux Variations Following the 2
    November 1969 Event
Authors: Domingo, V.; Page, E. E.; Shaw, M. L.
Bibcode: 1972spen.conf..105D
Altcode:
  No abstract at ADS

Title: New Results in Particle Arrival at the Polar Caps
Authors: Page, D. E.; Domingo, V.
Bibcode: 1972ASSL...32..107P
Altcode: 1972emp..conf..107P
  No abstract at ADS

Title: Two-satellite observation of spatial and temporal particle
    flux variations over the polar caps
Authors: Domingo, V.; Page, D. E.
Bibcode: 1972JGR....77.1971D
Altcode:
  No abstract at ADS

Title: North-South Asymmetry in Polar Cap Regions. (Abstract)
Authors: Domingo, V.; Page, D. E.
Bibcode: 1971ICRC....2..825D
Altcode: 1971ICRC...12..825D
  No abstract at ADS

Title: North-South Asymmetry in Polar Cap Regions
Authors: Domingo, V.; Page, D. E.
Bibcode: 1971ICRC....5.2009D
Altcode: 1971ICRC...12.2009D
  No abstract at ADS

Title: North-south asymmetry of solar-particle fluxes in polar-cap
    regions
Authors: Domingo, V.; Page, D. E.
Bibcode: 1971JGR....76.8159D
Altcode:
  On January 24, 1969, an experiment on the Esro 1/Aurorae satellite
  recorded a flux over the central north pole that at times was a factor
  of 7 greater than that seen over the south pole. This asymmetry is
  discussed in relation to the interplanetary-field direction measured
  at the same time by the Heos spacecraft, and comparison is made with
  the opposite asymmetrical configuration observed by Evans and Stone
  (1969) on November 2, 1967. From the evidence of two events it would
  appear that a southward interplanetary field plays a significant role
  in permitting direct access, while the magnitude and polarity of the
  asymmetry are determined by, respectively, interplanetary-particle
  anisotropy and the ‘toward’ or ‘away’ nature of the field.

Title: Muons in air showers of energies above 10<SUP>17</SUP> eV
Authors: Suga, K.; Shibata, S.; Mikamo, S.; Toyoda, Y.; Murakami,
   K.; Lapointe, M.; Kamata, K.; Domingo, V.
Bibcode: 1970ICRC....3..423S
Altcode: 1969ICRC....3..423S; 1970ICRC...11c.423S
  No abstract at ADS

Title: Predominantly electromagnetic air showers of energy
    10<SUP>14</SUP> eV to 10<SUP>16</SUP> eV
Authors: Kamata, K.; Shibata, S.; Saavedra, O.; Domingo, V.; Suga,
   K.; Murakami, K.; Toyoda, Y.; Lapointe, M.; Gaebler, J.; Escobar, I.
Bibcode: 1968CaJPS..46...72K
Altcode: 1968CaJPh..46S..72K; 1968ICRC...10...72K
  No abstract at ADS

Title: Note on the primary energy spectrum
Authors: Lapointe, M.; Kamata, K.; Gaebler, J.; Escobar, I.; Domingo,
   V.; Suga, K.; Murakami, K.; Toyoda, Y.; Shibata, S.
Bibcode: 1968CaJPS..46...68L
Altcode: 1968ICRC...10...68L; 1968CaJPh..46S..68L
  No abstract at ADS

Title: Studies of primary cosmic rays in the energy region
    10<SUP>14</SUP> to 10<SUP>17</SUP> eV (Bolivian Air Shower Joint
    Experiment)
Authors: Toyoda, Y.; Suga, K.; Murakami, K.; Hasegawa, H.; Shibata,
   S.; Domingo, V.; Escobar, I.; Kamata, K.; Bradt, H.; Clark, G.;
   La Pointe, M.
Bibcode: 1965ICRC....2..708T
Altcode: 1965ICRC....9..708T
  No abstract at ADS

Title: The Primary energy spectrum from 8 x 10<SUP>14</SUP>-4 x
    10<SUP>17</SUP> eV
Authors: Bradt, H.; Clark, G.; La Pointe, M.; Domingo, V.; Escobar,
   I.; Kamata, K.; Murakami, K.; Suga, K.; Toyoda, Y.
Bibcode: 1965ICRC....2..715B
Altcode: 1965ICRC....9..715B
  No abstract at ADS

Title: Evidence for extensive air showers with extremely few
    penetrating particles
Authors: Suga, K.; Escobar, I.; Murakami, K.; Domingo, V.; Toyoda,
   Y.; Clark, G.; La Pointe, M.
Bibcode: 1963ICRC....4....9S
Altcode: 1963ICRC....8d...9S
  No abstract at ADS

Title: Primary energy spectrum from 6.10<SUP>14</SUP> ev to 4.10 ev
Authors: Clark, G.; Bradt, H.; La Pointe, M.; Domingo, V.; Escobar,
   I.; Murakami, K.; Suga, K.; Toyoda, Y.; Hersil, J.
Bibcode: 1963ICRC....4...65C
Altcode: 1963ICRC....8d..65C
  No abstract at ADS

Title: Character of air showers at 5200 m altitude
Authors: Escobar, I.; Domingo, V.; Murakami, K.; Suga, K.; Toyoda,
   Y.; Clark, G.; La Pointe, M.; Oda, M.; Bradt, H.; Miura, I.; Nagano,
   M.; Shibata, S.; Tanahashi, G.; Hasegawa, H.
Bibcode: 1963ICRC....4..168E
Altcode: 1963ICRC....8d.168E
  No abstract at ADS

Title: A general account of the various research activities at
    Chacaltaya
Authors: Domingo, V.
Bibcode: 1963ICRC....4....3D
Altcode: 1963ICRC....8d...3D
  No abstract at ADS

