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Author name code: delaboudiniere
ADS astronomy entries on 2022-09-14
author:"Delaboudiniere, Jean-Pierre" 

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Title: Sun Earth Connection Coronal and Heliospheric Investigation
    (SECCHI)
Authors: Howard, R. A.; Moses, J. D.; Vourlidas, A.; Newmark, J. S.;
   Socker, D. G.; Plunkett, S. P.; Korendyke, C. M.; Cook, J. W.; Hurley,
   A.; Davila, J. M.; Thompson, W. T.; St Cyr, O. C.; Mentzell, E.;
   Mehalick, K.; Lemen, J. R.; Wuelser, J. P.; Duncan, D. W.; Tarbell,
   T. D.; Wolfson, C. J.; Moore, A.; Harrison, R. A.; Waltham, N. R.;
   Lang, J.; Davis, C. J.; Eyles, C. J.; Mapson-Menard, H.; Simnett,
   G. M.; Halain, J. P.; Defise, J. M.; Mazy, E.; Rochus, P.; Mercier,
   R.; Ravet, M. F.; Delmotte, F.; Auchere, F.; Delaboudiniere, J. P.;
   Bothmer, V.; Deutsch, W.; Wang, D.; Rich, N.; Cooper, S.; Stephens,
   V.; Maahs, G.; Baugh, R.; McMullin, D.; Carter, T.
2008SSRv..136...67H    Altcode: 2008SSRv..tmp...64H
  The Sun Earth Connection Coronal and Heliospheric Investigation
  (SECCHI) is a five telescope package, which has been developed for
  the Solar Terrestrial Relation Observatory (STEREO) mission by the
  Naval Research Laboratory (USA), the Lockheed Solar and Astrophysics
  Laboratory (USA), the Goddard Space Flight Center (USA), the University
  of Birmingham (UK), the Rutherford Appleton Laboratory (UK), the
  Max Planck Institute for Solar System Research (Germany), the Centre
  Spatiale de Leige (Belgium), the Institut d’Optique (France) and the
  Institut d’Astrophysique Spatiale (France). SECCHI comprises five
  telescopes, which together image the solar corona from the solar disk to
  beyond 1 AU. These telescopes are: an extreme ultraviolet imager (EUVI:
  1 1.7 R<SUB>⊙</SUB>), two traditional Lyot coronagraphs (COR1: 1.5 4
  R<SUB>⊙</SUB> and COR2: 2.5 15 R<SUB>⊙</SUB>) and two new designs
  of heliospheric imagers (HI-1: 15 84 R<SUB>⊙</SUB> and HI-2: 66 318
  R<SUB>⊙</SUB>). All the instruments use 2048×2048 pixel CCD arrays
  in a backside-in mode. The EUVI backside surface has been specially
  processed for EUV sensitivity, while the others have an anti-reflection
  coating applied. A multi-tasking operating system, running on a PowerPC
  CPU, receives commands from the spacecraft, controls the instrument
  operations, acquires the images and compresses them for downlink
  through the main science channel (at compression factors typically
  up to 20×) and also through a low bandwidth channel to be used for
  space weather forecasting (at compression factors up to 200×). An
  image compression factor of about 10× enable the collection of images
  at the rate of about one every 2 3 minutes. Identical instruments,
  except for different sizes of occulters, are included on the STEREO-A
  and STEREO-B spacecraft.

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Title: The SECCHI Experiment on the STEREO Mission
Authors: Howard, R. A.; Moses, J. D.; Vourlidas, A.; Newmark, J. S.;
   Socker, D. G.; Wang, D.; Plunkett, S. P.; Baugh, R.; McMullin, D. R.;
   Davila, J. M.; Thompson, W. T.; Lemen, J. R.; Wuelser, J.; Harrison,
   R. A.; Waltham, N. R.; Davis, C. J.; Eyles, C. J.; Defise, J.; Halain,
   J.; Bothmer, V.; Delaboudiniere, J.; Auchere, F.; Mercier, R.; Ravet,
   M. F.
2007AGUSMSH33A..01H    Altcode:
  The Sun Earth Connection Coronal and Heliospheric Investigation
  (SECCHI) on the NASA Solar Terrestrial Relations Observatory (STEREO)
  mission is a suite of remote sensing instruments consisting of an
  extreme ultraviolet (EUV) imager, two white light coronagraphs, and
  two telescopes that comprise the heliospheric imager. SECCHI will
  observe coronal mass ejections (CMEs) from their birth at the sun,
  through the corona and into the heliosphere. A complete instrument
  suite is being carried on each of the two STEREO spacecraft, which
  will provide the first sampling of a CME from two vantage points. The
  spacecraft, launched 25 October 2006, are orbiting the Sun, one Ahead
  of the Earth and the other Behind, each separating from Earth at about
  22 degrees per year. The varying separation means that we will have
  different observational capabilities as the spacecraft separate and
  therefore differing science goals. The primary science objectives
  all are focused on understanding the physics of the CME process
  their initiation, 3D morphology, propagation, interaction with the
  interplanetary medium and space weather effects. By observing the CME
  from multiple viewpoints with UV and coronagraphic telescopes and by
  combining these observations with radio and in-situ observations from
  the other instruments on STEREO as well as from other satellites and
  ground based observatories operating at the same time, answers to some
  of the outstanding questions will be obtained. We will show some of
  the initial results.

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Title: Stereo Observations Of The Solar Corona Using The Secchi
    Experiment
Authors: Plunkett, Simon P.; Howard, R. A.; Moses, J. D.; Vourlidas,
   A.; Socker, D.; Newmark, J.; Wang, D.; Baugh, R.; Davila, J.;
   Thompson, W.; St. Cyr, O. C.; Lemen, J.; Wuelser, J. P.; Harrison,
   R. A.; Waltham, N.; Davis, C. J.; Eyles, C. J.; Defise, J. M.; Halain,
   J. P.; Bothmer, V.; Delaboudiniere, J. P.; Auchere, F.; Mercier, R.;
   Ravet, M. F.
2007AAS...21011901P    Altcode: 2007BAAS...39..243P
  The Sun Earth Connection Coronal and Heliospheric Investigation
  (SECCHI) on the NASA Solar Terrestrial Relations Observatory (STEREO)
  mission is a suite of remote sensing instruments consisting of an
  extreme ultraviolet (EUV) imager, two white light coronagraphs,
  and two telescopes that comprise the heliospheric imager. The main
  objective of SECCHI is to observe coronal mass ejections (CMEs) from
  their birth at the sun, through the corona and into the heliosphere. A
  complete instrument suite is being carried on each of the two STEREO
  spacecraft, which will provide the first sampling of a CME from two
  vantage points as the spacecraft separate from each other at the rate
  of about 45 degrees per year. We will show examples of some of the
  data and some of the initial stereo results.

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Title: The SECCHI Experiment on the STEREO Mission
Authors: Howard, R. A.; Moses, D.; Vourlidas, A.; Newmark, J.; Socker,
   D. G.; Plunkett, S.; Wang, D.; Baugh, R.; McMullin, D.; Davila, J.;
   St. Cyr, C.; Thompson, W. T.; Lemen, J.; Wuelser, J.; Harrison, R. A.;
   Waltham, N. R.; Davis, C.; Eyles, C. J.; Defise, J.; Halain, J.;
   Bothmer, V.; Delaboudiniere, J.; Auchere, F.; Mercier, R.; Ravet, M.
2006AGUFMSM12A..02H    Altcode:
  The Sun Earth Connection Coronal and Heliospheric Investigation
  (SECCHI) on the NASA Solar Terrestrial Relations Observatory (STEREO)
  mission is a suite of remote sensing instruments consisting of an
  extreme ultraviolet (EUV) imager, two white light coronagraphs, and
  two telescopes that comprise the heliospheric imager. SECCHI will
  observe coronal mass ejections (CMEs) from their birth at the sun,
  through the corona and into the heliosphere. A complete instrument
  suite is being carried on each of the two STEREO spacecraft, which
  will provide the first sampling of a CME from two vantage points. The
  spacecraft will orbit the Sun, one Ahead of the Earth and the other
  Behind, each separating from Earth at about 22 degrees per year. The
  varying separation means that we will have different observational
  capabilities as the spacecraft separate and therefore differing science
  goals. The primary science objectives all are focused on understanding
  the physics of the CME process their initiation, 3D morphology,
  propagation, interaction with the interplanetary medium and space
  weather effects. By observing the CME from multiple viewpoints with UV
  and coronagraphic telescopes and by combining these observations with
  radio and in-situ observations from the other instruments on STEREO as
  well as from other satellites and ground based observatories operating
  at the same time, answers to some of the outstanding questions will
  be obtained. STEREO follows the very successful SOHO mission. SOHO's
  success was primarily due to the highly complementary nature of the
  instruments, but it was partly due to the very stable platform. The
  L1 orbit enables an extremely stable thermal environment and thus
  very stable pointing, as well as uninterrupted solar viewing. The
  STEREO will have both of these characteristics, but in addition will
  have multi-viewpoint viewing of CMEs, which will greatly enhance the
  many discoveries that SOHO data have produced. We have been developing
  techniques to interpret the observations from multiple viewpoints and
  to perform 3-dimensional deconvolution of the CME observations using
  forward modeling and inversion techniques. A continuous downlink of
  STEREO data will provide a low-resolution, real- time view from all
  of the instruments. The full data are downlinked once a day and will
  be available about 24 hours later. We will present some preliminary
  results from the instrument, which is expected to be launched in
  October/November, 2006

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Title: A Spectroscopic Observation of a Magnetic Reconnection Site
    in a Small Flaring Event
Authors: Hara, Hirohisa; Nishino, Yohei; Ichimoto, Kiyoshi;
   Delaboudinière, Jean-Pierre
2006ApJ...648..712H    Altcode:
  We have observed two types of coronal bidirectional flows in a flare
  with a small energy release through a spectroscopic observation of
  the Fe X emission line at 6374 Å with a ground-based coronagraph
  at the Norikura Solar Observatory. We find a bidirectional flow of
  +/-3 km s<SUP>-1</SUP> above the top of a flare loop. Remarkable
  increases of the line intensity and line width are not observed in
  the flow. From the loop geometry and sign of the Fe X Doppler velocity
  we conclude that the bidirectional flow is reconnection inflow above
  the flare loop. We estimate the reconnection rate to be ~0.003 for
  this event. The other bidirectional flow is observed along postflare
  loops with significant increases of the line intensity and Doppler
  velocity. This flow is interpreted as a cooling upflow having a velocity
  of ~10 km s<SUP>-1</SUP> along a postflare loop from its lower part. We
  also find that the increase of the nonthermal line width in the loop-top
  region starts when the line intensity reaches its peak. This supports
  the presence of a mechanism to enhance turbulent plasma motions in
  the loop-top region.

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Title: An atlas of solar events: 1996 2005
Authors: Artzner, G.; Auchère, F.; Delaboudinière, J. P.; Bougnet, M.
2006AdSpR..38..390A    Altcode:
  Coronal mass ejections (CMEs) are observed in the plane of the sky in
  coronographic images. As the solar surface is masked by an occulting
  disk it is not clear whether halo CMEs are directed towards or away
  from the Earth. Observations of the solar corona on the solar disk
  by the extreme ultraviolet imaging telescope (EIT) on board the Solar
  Heliospheric Observatory SoHO can help to resolve this. Quasi-continuous
  observations of the solar corona were obtained from April 1997 up to
  the current date at a 12 min cadence in the coronal line of FeXII, as
  part of a “CME watch program”. At a slower 6 h cadence an additional
  synoptic program investigates the chromosphere and the corona at four
  different wavelengths. Large coronal solar events appear when viewing
  animations of the CME watch program. Fainter events do appear when
  viewing running difference animations of the CME watch program. When
  looking for additional spectral information from raw running differences
  of the synoptic program it is difficult to disentangle intrinsic solar
  events from the parasitic effect of the solar rotation. We constructed
  at www.ias.u-psud.fr/medoc/EIT/movies/ an atlas of more than 40,000
  difference images from the synoptic programme, corrected for an
  average solar rotation, as well as more than 200,000 instantaneous and
  difference images from the CME watch program. We present case studies
  of specific events in order to investigate the source of darkenings or
  dimmings in difference images, due to the removal of emitting material,
  the presence of obscuring material or large changes in temperature. As
  the beneficial effect of correcting for the solar rotation vanishes at
  the solar limb, we do not investigate the case of prominence Doppler
  dimming. As a by-product of the atlas of solar events we obtain a
  number of quiet time sequences well suited to precisely measure the
  differential solar rotation by the apparent displacement of tracers.

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Title: Observations of Solar EUV Radiation with the CORONAS-F/SPIRIT
    and SOHO/EIT Instruments
Authors: Slemzin, V. A.; Kuzin, S. V.; Zhitnik, I. A.; Delaboudiniere,
   J. -P.; Auchere, F.; Zhukov, A. N.; van der Linden, R.; Bugaenko,
   O. I.; Ignat'ev, A. P.; Mitrofanov, A. V.; Pertsov, A. A.; Oparin,
   S. N.; Stepanov, A. I.; Afanas'ev, A. N.
2005SoSyR..39..489S    Altcode:
  The SPIRIT complex onboard the CORONAS-F satellite has routinely
  imaged the Sun in the 171, 175, 195, 284, and 304 Å spectral bands
  since August 2001. The complex incorporates two telescopes. The
  Ritchey-Chretien telescope operates in the 171, 195, 284, and
  304 Å bands and has an objective similar to that of the SOHO/EIT
  instrument. The Herschel telescope obtains solar images synchronously
  in the 175 and 304 Å bands with two multilayer-coated parabolic
  mirrors. The SPIRIT program includes synoptic observations, studies of
  the dynamics of various structures on the solar disk and in the corona
  up to 5 solar radii, and coordinated observations with other spaceborne
  and ground-based telescopes. In particular, in the period 2002-2003,
  synoptic observations with the SPIRIT Ritchey-Chretien telescope were
  coordinated with regular 6-hour SOHO/EIT observations. Since June 2003,
  when EIT data were temporarily absent ( SOHO keyholes), the SPIRIT
  telescope has performed synoptic observations at a wavelength of 175
  A. These data were used by the Solar Influence Data Analysis Center
  (SIDC) at the Royal Observatory of Belgium for an early space weather
  forecast. We analyze the photometric and spectral parameters of the
  SPIRIT and EIT instruments and compare the integrated (over the solar
  disk) EUV fluxes using solar images obtained with these instruments
  during the CORONAS-F flight from August 2001 through December 2003.

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Title: Manifestations of Coronal Mass Ejections in the EUV Range
    from Data of the CORONAS-F/SPIRIT Telescope
Authors: Chertok, I. M.; Grechnev, V. V.; Slemzin, V. A.; Kuzin,
   S. V.; Bugaenko, O. I.; Zhitnik, I. A.; Ignat'ev, A. P.; Pertsov,
   A. A.; Delaboudiniere, J. -P.
2005SoSyR..39..462C    Altcode:
  We briefly overview results of our study of the large-scale
  solar activity associated with coronal mass ejections (CMEs). The
  observational material is constituted with data of the SPIRIT telescope
  aboard the CORONAS-F satellite in the three EUV channels 175, 284,
  and 304 Å. In particular, we consider a powerful geoeffective event
  of November 4, 2003, which was not observed by the SOHO/EIT telescope,
  a series of extremely powerful events of October 2003, and an event
  of November 18, 2003, with filament eruption. The efficiency of
  combined analysis of the SPIRIT and EIT data is demonstrated. The
  analysis confirms the coincidence of many dimmings in different
  spectral channels, including coronal lines with different excitation
  temperatures and the transition-region line, as well as the global
  character and homology of dimmings in recurrent events. The higher
  cadence SPIRIT observations at 304 Å reveal a slowly propagating
  large-scale darkening probably caused by absorption of emission in
  the dense, cold plasma of an eruptive filament.

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Title: CORONAS-F/SPIRIT EUV observations of October-November 2003
    solar eruptive events in combination with SOHO/EIT data
Authors: Grechnev, V. V.; Chertok, I. M.; Slemzin, V. A.; Kuzin, S. V.;
   Ignat'ev, A. P.; Pertsov, A. A.; Zhitnik, I. A.; DelaboudinièRe,
   J. -P.; AuchèRe, F.
2005JGRA..110.9S07G    Altcode: 2005JGRA..11009S07G
  The extraordinary solar activity of October-November 2003 manifested
  itself in many powerful eruptive events, including large coronal mass
  ejections (CMEs) and extremely powerful flares. A number of major
  events were accompanied by practically all known phenomena of the solar
  activity, both local and large-scale, and caused severe space weather
  disturbances. We study large-scale posteruptive activity manifestations
  on the Sun associated with CMEs, i.e., dimmings and coronal waves,
  observed with extreme-ultraviolet telescopes, the SPIRIT on the
  CORONAS-F spacecraft and the EIT on the SOHO. During that period,
  observations with a cadence of 15 to 45 min were carried out by the
  SPIRIT in the 175 Å and 304 Å bands simultaneously. The EIT observed
  with 12-min cadence in the 195 Å band as well as with 6-hour cadence
  in the 171, 284, and 304 Å bands. These data complement each other
  both in the temporal and spectral coverage. Our analysis reveals
  that largest-scale dimmings covered almost the whole southern part of
  the Sun's visible side and exhibited homology, with one homological
  structure being changed to another configuration on 28 October. These
  structures show connections between large superactive and smaller
  regions that constituted a huge activity complex responsible for the
  extraordinary solar activity of that period. Coronal waves were observed
  at 175 Å as well as at 195 Å in some events, in areas where there were
  no active regions, but in the 175 Å images they look fainter. They
  were not accompanied by deep, long-living dimmings. By contrast,
  such dimmings were observed in active regions, in their vicinity,
  and between them. These facts rule out the direct relation of the
  phenomena of long-term dimmings and coronal waves. On 18 November, a
  motion of an ejecta was observed at the solar disk as a propagation of
  a dark feature only in the 304 Å band, which can be interpreted as an
  absorption in a "cloud" formed from material of the eruptive filament,
  which probably failed to become a CME core.

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Title: Research on a complex CME event including Hα, LASCO, radio
    and MDI observations
Authors: Wang, S. J.; Maia, D.; Pick, M.; Aulanier, G.; Malherbe,
   J. -M.; Delaboudinière, J. -P.
2005AdSpR..36.2273W    Altcode:
  We present our research on a fast and decelerating partial halo
  coronal mass ejection (CME) event detected in multi-wavelengths
  in the chromosphere and the corona on 14 October, 1999. The event
  involved a whole complex active area which spanned more than 40°
  of heliolongitude. It included a strong solar flare (XI/1N) and a
  complex eruptive filament within an active region of the entire
  complex. Especially, several radio sources were detected in the
  decimetric range prior to the CME by the Nançay Radioheliograph
  (NRH). A linear force-free field extrapolation of the Michelson Doppler
  Imager (MDI) magnetogram was performed to calculate the magnetic
  topology of the complex prior to the triggering of the event. The
  presence of a coronal null point combined with the occurrence of two
  distant and nearly simultaneous radio sources put strong arguments
  in favor of the generalized breakout model for the triggering of the
  eruption. The analysis of the subsequent development of the event
  suggests that large interconnecting loops were ejected together with
  the CME.

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Title: Shock Wave Driven by an Expanding System of Loops
Authors: Raouafi, N. -E.; Mancuso, S.; Solanki, S. K.; Inhester, B.;
   Mierla, M.; Stenborg, G.; Delaboudinière, J. P.; Benna, C.
2005IAUS..226..127R    Altcode:
  We report on a Coronal Mass Ejection (CME) observed on June 27
  1999 by the UltraViolet Coronagraph Spectrometer (UVCS) telescope
  operating on board the SOHO spacecraft. The CME was also observed
  by LASCO (SOHO). Emission of hot material has been recorded by UVCS
  propagating in front of an opening system of loops generated by the
  CME. The evolution of the UVCS structure is highly correlated to the
  evolution of the opening loop. The data reveal excess broadening of
  the O VI doublet lines and an enhancement in the intensity of the Si
  XII λ 520.66 and λ499.37 lines due to the motion of the expanding hot
  gas. The hot gas emission seems to be due to a shock wave propagating in
  front of a very fast gas bubble traveling along the opening loop system.

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Title: HERSCHEL Suborbital Program: 3-D Applications for the STEREO
    Mission
Authors: Moses, J. D.; Newmark, J.; McMullin, D.; Antonucci, E.;
   Fineschi, S.; Gardiol, D.; Zangrilli, L.; Romoli, M.; Pace, E.; Gori,
   L.; Landini, F.; Gherardi, A.; da Deppo, V.; Naletto, G.; Nicolosi, P.;
   Pelizzo, M.; Malvezzi, M.; Auchere, F.; Delaboudiniere, J.; Howard, R.
2004AGUFMSH23A..08M    Altcode:
  The HERSCHEL (HElium Resonance Scatter in the Corona and HELiosphere)
  Suborbital Program is an international collaborative program between
  a consortium of Italian Universities &amp; Observatories led by
  Dr. E. Antonucci (and funded by the Italian Space Agency, ASI), the
  French IAS (funded in part by CNES) and the Solar Physics Branch of
  NRL (by NASA SEC and the Office of Naval Research). HERSCHEL will:
  investigate the slow and fast solar wind, determine the helium
  distribution and abundance in the corona, and test solar wind
  acceleration models; by obtaining simultaneous observations of
  the electron, proton and helium solar coronae. HERSCHEL will also
  establish proof-of-principle for the Ultra-Violet Coronagraph, which
  is in the ESA Solar Orbiter Mission baseline. The HERSCHEL launch date
  has been linked to the STEREO launch date to allow coordinated science
  between the two missions. One aspect of this scientific coordination is
  establishing the 3-D structure of the inner corona. HERSCHEL provides
  a third viewpoint for the inner corona covered by the A&amp;B STEREO
  SECCHI COR-1. HERSCHEL is the only scheduled, space-based asset that
  could provide this third viewpoint for the critical inner corona viewed
  by STEREO COR-1 (although lower resolution, ground-based cononagraphs
  will make a contribution). A third viewpoint dramatically increases
  one's ability to establish the 3-D structure of an optically thin object
  (e.g. the metric in Fig. 7 of Davila 1994, ApJ 423, 871). HERSCHEL will
  provide at least a snapshot of that viewpoint, plus a wide range of
  additional information on the H and He composition of the inner corona.

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Title: Shock wave driven by an expanding system of loops
Authors: Raouafi, N. -E.; Mancuso, S.; Solanki, S. K.; Inhester, B.;
   Mierla, M.; Stenborg, G.; Delaboudinière, J. P.; Benna, C.
2004A&A...424.1039R    Altcode:
  We report on a Coronal Mass Ejection (CME) observed on June 27, 1999 by
  the UltraViolet Coronagraph Spectrometer (UVCS) telescope operating on
  board the SOHO spacecraft. The CME was also observed by the Large Angle
  Spectroscopic Coronagraph (LASCO). Emission of hot material has been
  recorded by UVCS propagating in front of an opening system of loops
  generated by the CME. The evolution of the UVCS structure is highly
  correlated with the evolution of the opening loop. The data reveal
  excess broadening of the O VI doublet lines and an enhancement in the
  intensity of the Si XII λ520.66 and λ499.37 lines due to the motion
  of the expanding hot gas. The hot gas emission seems to be due to a
  shock wave propagating in front of a very fast gas bubble traveling
  along the opening loop system.

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Title: The August 11th, 1999 CME
Authors: Koutchmy, S.; Baudin, F.; Bocchialini, K.; Daniel, J. -Y.;
   Delaboudinière, J. -P.; Golub, L.; Lamy, P.; Adjabshirizadeh, A.
2004A&A...420..709K    Altcode:
  We present here a set of observations, space borne and ground based,
  at different wavelengths, of the solar corona at and after the time of
  the total solar eclipse of August 11{th}. It is used to consider some
  unusual features of the coronal dynamics related to a limb Coronal Mass
  Ejection (CME) observed after the total eclipse. The complementary
  aspect of simultaneous ground-based and space-borne observations
  of the corona is used to produce an accurate composite image of the
  White Light (W-L) corona before the CME. A high arch system (possibly
  a dome-like structure, with large cavities inside but without a cusp
  further out) which appeared on the eclipse W-L images, is suggested to
  be a large-scale precursor of the CME, well preceding the eruption of
  the top part of the brightest prominence recorded in W-L. This bright
  prominence is shown as a filament in absorption using the Transition
  Region And Corona Explorer (TRACE) images taken in different coronal
  lines. The analysis of the images of the Large Angle and Spectrometric
  Coronograph (LASCO) on board the Solar and Heliospheric Observatory
  (SoHO), showing the progression of the CME, is discussed in an attempt
  to make a connection with the surface event. A SoHO-EIT (Extreme
  UV Imager Telescope) image sequence details the prominence eruption
  and shows the sudden heating processes of the ejected parts. We found
  that there is no reason to assume that the huge cavity is significantly
  destabilised well before the eruption of the upper part of the low-lying
  bright twisted filament which coincides with the position of one of
  the legs of the high arch. Observations are still compatible with the
  assumption of both the break-out model and of the flux rope erupting
  model as a result of a shear or of an increasing poloıdal magnetic
  flux from below. We stress the possible role of buoyancy of the giant
  cavity as a destabilizing factor leading to the CME, noticing that some
  motion of coronal material back toward the surface can be seen during at
  least the first phase of the CME, from both EIT and LASCO observations.

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Title: Ion beam deposited Mo/Si multilayers for EUV imaging
    applications in astrophysics
Authors: Ravet, Marie-Francoise; Bridou, Francoise; Zhang-Song, Xueyan;
   Jerome, Arnaud; Delmotte, Franck; Mercier, Raymond; Bougnet, Marie;
   Bouyries, Philippe; Delaboudiniere, Jean-Pierre
2004SPIE.5250...99R    Altcode:
  Imaging of the solar corona by selecting Fe IX (λ=17.1nm,), Fe XII
  (λ=19.5nm), Fe XV (λ=28.4nm) and He II (λ=30.4nm) emission lines
  with a Ritchey-Chretien telescope requires to coat the optics with
  multilayers having a high accuracy in their layer thicknesses, a
  high reflectivity and an optimal bandpass. Multilayers were simulated
  in order to determine the most adequate formula for each wavelength
  channel. Mo/Si coatings were deposited by using the ion beam sputtering
  technique in a high vacuum chamber equipped with a micro balance and
  an in-situ reflectometer. The multilayers were studied by grazing angle
  reflectometry at 0.1541nm, and their reflectances around the operating
  wavelengths were measured on the SA62 IAS/LURE beam line of the SuperACO
  synchrotron facility located at Orsay. In addition, aging versus time
  and behavior of the multilayers under a rapid thermal annealing were
  investigated. Performances of the ion-beam deposited multilayers have
  been improved compared to the Mo/Si coatings obtained in the past
  by the e-beam evaporation technique for the SOHO mission Extreme UV
  Imaging Telescope (EIT). The EUVI telescopes for the STEREO mission
  are being proceduced by depositing these new generation of multilayers
  onto primary and secondary mirrors. The reflectivity measurements on
  a telescope are presented.

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Title: MAGRITTE: an instrument suite for the solar atmospheric
    imaging assembly (AIA) aboard the Solar Dynamics Observatory
Authors: Rochus, Pierre L.; Defise, Jean-Marc; Halain, Jean-Philippe;
   Jamar, Claude A. J.; Mazy, Emmanuel; Rossi, Laurence; Thibert,
   Tanguy; Clette, Frederic; Cugnon, Pierre; Berghmans, David; Hochedez,
   Jean-Francois E.; Delaboudiniere, Jean-Pierre; Auchere, Frederic;
   Mercier, Raymond; Ravet, Marie-Francoise; Delmotte, Franck; Idir,
   Mourad; Schuehle, Udo H.; Bothmer, Volker; Fineschi, Silvano; Howard,
   Russell A.; Moses, John D.; Newmark, Jeffrey S.
2004SPIE.5171...53R    Altcode:
  The Solar Atmospheric Imaging Assembly (AIA) aboard the Solar Dynamics
  Observatory will characterize the dynamical evolution of the solar
  plasma from the chromosphere to the corona, and will follow the
  connection of plasma dynamics with magnetic activity throughout the
  solar atmosphere. The AIA consists of 7 high-resolution imaging
  telescopes in the following spectral bandpasses: 1215Å. Ly-a,
  304 Å He II, 629 Å OV, 465 Å Ne VII, 195 Å Fe XII (includes Fe
  XXIV), 284 Å Fe XV, and 335 Å Fe XVI. The telescopes are grouped
  by instrumental approach: the MAGRITTE Filtergraphs (R. MAGRITTE,
  famous 20th Century Belgian Surrealistic Artist), five multilayer EUV
  channels with bandpasses ranging from 195 to 1216 Å, and the SPECTRE
  Spectroheliograph with one soft-EUV channel at OV 629 Å. They will be
  simultaneously operated with a 10-second imaging cadence. These two
  instruments, the electronic boxes and two redundant Guide Telescopes
  (GT) constitute the AIA suite. They will be mounted and coaligned on a
  dedicated common optical bench. The GTs will provide pointing jitter
  information to the whole SHARPP assembly. This paper presents the
  selected technologies, the different challenges, the trade-offs to be
  made in phase A, and the model philosophy. From a scientific viewpoint,
  the unique combination high temporal and spatial resolutions with the
  simultaneous multi-channel capability will allow MAGRITTE / SPECTRE
  to explore new domains in the dynamics of the solar atmosphere, in
  particular the fast small-scale phenomena. We show how the spectral
  channels of the different instruments were derived to fulfill the
  AIA scientific objectives, and we outline how this imager array will
  address key science issues, like the transition region and coronal waves
  or flare precursors, in coordination with other SDO experiments. We
  finally describe the real-time solar monitoring products that will be
  made available for space-weather forecasting applications.

---------------------------------------------------------
Title: EUVI: the STEREO-SECCHI extreme ultraviolet imager
Authors: Wuelser, Jean-Pierre; Lemen, James R.; Tarbell, Theodore
   D.; Wolfson, C. J.; Cannon, Joseph C.; Carpenter, Brock A.; Duncan,
   Dexter W.; Gradwohl, Glenn S.; Meyer, Syndie B.; Moore, Augustus S.;
   Navarro, Rosemarie L.; Pearson, J. D.; Rossi, George R.; Springer,
   Larry A.; Howard, Russell A.; Moses, John D.; Newmark, Jeffrey S.;
   Delaboudiniere, Jean-Pierre; Artzner, Guy E.; Auchere, Frederic;
   Bougnet, Marie; Bouyries, Philippe; Bridou, Francoise; Clotaire,
   Jean-Yves; Colas, Gerard; Delmotte, Franck; Jerome, Arnaud; Lamare,
   Michel; Mercier, Raymond; Mullot, Michel; Ravet, Marie-Francoise;
   Song, Xueyan; Bothmer, Volker; Deutsch, Werner
2004SPIE.5171..111W    Altcode:
  The Extreme Ultraviolet Imager (EUVI) is part of the SECCHI instrument
  suite currently being developed for the NASA STEREO mission. Identical
  EUVI telescopes on the two STEREO spacecraft will study the structure
  and evolution of the solar corona in three dimensions, and specifically
  focus on the initiation and early evolution of coronal mass ejections
  (CMEs). The EUVI telescope is being developed at the Lockheed Martin
  Solar and Astrophysics Lab. The SECCHI investigation is led by the
  Naval Research Lab. The EUVI"s 2048 x 2048 pixel detectors have a
  field of view out to 1.7 solar radii, and observe in four spectral
  channels that span the 0.1 to 20 MK temperature range. In addition to
  its view from two vantage points, the EUVI will provide a substantial
  improvement in image resolution and image cadence over its predecessor
  SOHO-EIT, while complying with the more restricted mass, power, and
  volume allocations on the STEREO mission.

---------------------------------------------------------
Title: Dynamics of the loop prominence and coronal mass ejection
    observed on March 2, 2002
Authors: Panasenco, O.; Veselovsky, I. S.; Zhukov, A. N.; Yakovchouk,
   O. S.; Koutchmy, S.; Delaboudiniere, J. -P.
2004cosp...35.2974P    Altcode: 2004cosp.meet.2974P
  SOHO/EIT and LASCO data are used for the case study of the coronal mass
  ejection initiation and development. The shape, velocity and temperature
  of the loop prominence before and during the ejection as well as the
  new arcade formation are well documented. The prominence consisted of
  two spirals interweaved on the semi-torus. Both spirals are clearly
  seen during the initial stage of the expansion with a velocity about
  300 km/s. Than, one of them is rapidly heated, when other remained
  cool. The number of curls is conserved during the expansion. The
  main axis of the torus is initially represented by the planar curve
  resembling a semi-circle. After some time, the summit of the torus
  is twisted in the manner that the main axis looks not planar at the
  top in the field of view of LASCO C3 when the velocity attains about
  1000 km/s. The topological connectivity of the loops to the Sun is
  preserved for more than three hours even after the new arcade formation.

---------------------------------------------------------
Title: An atlas of solar events: 1997-2004
Authors: Artzner, G.; Auchère, F.; Delaboudinière, J. P.; Bougnet, M.
2004cosp...35.2494A    Altcode: 2004cosp.meet.2494A
  Coronal mass ejections (CMEs) are observed in the plane of the sky
  from coronographic images. As the solar surface is then masked by an
  occulting disk, it is not clear wether halo CMEs are directed towards
  the Earth or in the opposite direction. Observations of the solar corona
  on the solar disk from the Extreme Ultraviolet Imaging Telescope EIT on
  board the Solar Heliospheric Observatory SoHO do help in order to make
  a choice. Quasi-continuous observations of the corona of the Sun have
  been therefore obtained from april 1997 up to now at a twelve minute
  cadence in the coronal line of FeXII, as a CME watch program. At a
  slower six hours cadence an additional synoptic program investigates
  the chromosphere and the corona at four different wavelengths. Large
  coronal solar events appear when viewing animations of the CME watch
  program. Fainter events do appear when viewing running difference
  animations of the CME watch program. When looking for additional
  spectral information from raw running differences of the synoptic
  program it is difficult to disentangle intrinsic solar events from
  the parasitic effect of the solar rotation. We constructed from the
  synoptic program observations an atlas of more than 20 000 difference
  images corrected for an average solar rotation. We present case studies
  of specific events in order to investigate the source of darkenings in
  difference images, either removal of emitting material, interposition
  of obscuring material or large changes of temperature. Statistics
  of brigtenings and darkenings along solar cycle 23 are presented. We
  speculate about future observations from the STEREO mission in order
  to obtain better diagnostics about darkenings. As a by product of the
  atlas of solar events we obtain a number of quiet time sequences well
  suited in order to precisely measure the differnetial solar rotation
  by the apparent displacement of tracers.

---------------------------------------------------------
Title: Multi-wavelength observations of CME-associated structures
    on the Sun with the CORONAS-F/SPIRIT EUV telescope
Authors: Slemzin, V.; Chertok, I.; Grechnev, V.; Ignat'ev, A.; Kuzin,
   S.; Pertsov, A.; Zhitnik, I.; Delaboudinière, J. -P.
2004IAUS..223..533S    Altcode: 2005IAUS..223..533S
  Multi-wavelength imaging of the solar corona is a powerful observational
  method to study CME-related dynamics of structures in spectral
  bands related to the solar corona and transition region. We analyze
  large-scale eruptive events caused by halo-type CMEs observed at the
  solar disk with the CORONAS-F/SPIRIT (175, 304, and 284 Å) and SOHO/EIT
  telescopes on November 4, 2001 and October-November, 2003. For most
  events, CME-associated dimmings coincide in different bands, but the 304
  Å dimming in November 4, 2001 event was delayed by &gt;1/2 hours. In
  October-November events, coronal waves were observed in 195 Å and some
  in 175 Å channel. In a CME event associated with a filament eruption
  on November 18, the SPIRIT images display a propagating disturbance
  seen as a darkening in 304 Å channel only. This phenomenon was not
  described earlier.

---------------------------------------------------------
Title: Interpretation of the Coronal EUV Signature of the CME Event
    on June 27 1999
Authors: Raouafi, N. -E.; Mancuso, S.; Solanki, S. K.; Inhester, B.;
   Benna, C.; Delaboudinière, J. P.; Stenborg, G.; Mierla, M.
2004ESASP.547..317R    Altcode: 2004soho...13..317R
  We report the observation of a Coronal Mass Ejection (CME) detected
  on June 27 1999 by the UltraViolet Coronagraph Spectrometer (UVCS)
  telescope operating on board the SOHO spacecraft. The CME, whose
  leading edge was expanding at a projected speed of about 1200 km s,
  was observed in white light by the Large Angle Spectroscopic Coronagraph
  (LASCO). The UVCS spectra reveal excess broadening of the O VI doublet
  lines and enhancement in the intensity of the Si XII lines due to the
  motion of expanding hot material. The evolution of the UVCS structure
  is highly correlated to the evolution of the CME observed by LASCO
  in white light, so that the hot gas emission could be attributable to
  the passage of a shock wave propagating just in front of the fast CME.

---------------------------------------------------------
Title: The Ultraviolet and Visible-light Coronagraph of the HERSCHEL
    experiment
Authors: Romoli, M.; Antonucci, E.; Fineschi, S.; Gardiol, D.;
   Zangrilli, L.; Malvezzi, M. A.; Pace, E.; Gori, L.; Landini, F.;
   Gherardi, A.; da Deppo, V.; Naletto, G.; Nicolosi, P.; Pelizzo, M. G.;
   Moses, J. D.; Newmark, J.; Howard, R.; Auchere, F.; Delaboudinière,
   J. P.
2003AIPC..679..846R    Altcode:
  The Herschel (HElium Resonant Scattering in the Corona and HELiosphere)
  experiment, to be flown on a sounding rocket, will investigate the
  helium coronal abundance and the solar wind acceleration from a
  range of solar source structures by obtaining the first simultaneous
  observations of the electron, proton and helium solar corona. The
  HERSCHEL payload consists of the EUV Imaging Telescope (EIT), that
  resembles the SOHO/EIT instrument, and the Ultraviolet and Visible
  Coronagraph (UVC).UVC is an imaging coronagraph that will image
  the solar corona from 1.4 to 4 solar radii in the EUV lines of HI
  121.6 nm and the HeII 30.4 nm and in the visible broadband polarized
  brightness. The UVC coronagraph is externally occulted with a novel
  design as far as the stray light rejection is concerned. Therefore,
  HERSCHEL will also establish proof-of-principle for the Ultraviolet
  Coronagraph, which is in the ESA Solar Orbiter Mission baseline.The
  scientific objectives of the experiment will be discussed, togetherwith
  a description of the UVC coronagraph.

---------------------------------------------------------
Title: Interpretation of a complex CME event: Coupling of scales in
    multiple flux systems
Authors: Maia, D.; Aulanier, G.; Wang, S. J.; Pick, M.; Malherbe,
   J. -M.; Delaboudinière, J. -P.
2003A&A...405..313M    Altcode:
  Using multi-wavelength observations, in particular in imagery, recorded
  by SOHO/LASCO-MDI, Yohkoh/SXT, the Meudon spectroheliograph and the
  Nançay radioheliograph, and performing a linear force-free field
  extrapolation, we analyzed the triggering and the development of a
  complex eruptive event in the chromosphere and in the corona. This
  event included an X1 class flare and an eruptive filament within an
  active region, but it also involved a whole active complex spanning over
  40 degrees of heliolongitude. It resulted in a fast and decelerating
  partial halo CME, associated with a Moreton wave and a complex series
  of metric, decimetric and microwave radio bursts. The presence of a
  coronal null point combined with the occurrence of two distant and
  nearly simultaneous radio sources give strong arguments in favor of
  the generalized breakout model for the triggering of the eruption. The
  observations are consistent with the occurrence of magnetic reconnection
  at the null point three minutes before the start of the eruption,
  which is consistent with other observed CME precursors. The analysis
  of the subsequent development of the event suggests that large
  interconnecting loops were ejected together with the CME, and that
  secondary reconnections at low altitude probably occurred remotely in
  the active complex. Our results show that the triggering and evolution
  of this complex CME involved multiple magnetic flux systems over a
  large coronal volume surrounding the flare site, and that it resulted
  from the coupling of scales from narrow reconnection current sheets
  to very large inter active region magnetic connections.

---------------------------------------------------------
Title: The solar high-resolution imager - coronagraph LYOT mission
Authors: Vial, Jean-Claude; Song, Xueyan; Lemaire, Philippe; Gabriel,
   Alan H.; Delaboudiniere, Jean-Pierre; Bocchialini, Karine; Koutchmy,
   Serge L.; Lamy, Philippe L.; Mercier, Raymond; Ravet, Marie Francoise;
   Auchere, Frederic
2003SPIE.4853..479V    Altcode:
  The LYOT (LYman Orbiting Telescope) solar mission is proposed to
  be implemented on a micro-satellite of CNES (France) under phase A
  study. It includes two main instruments, which image the solar disk
  and the low corona up to 2.5 R<SUB>o</SUB> in the H I Lyman-α line
  at 121.6 nm. The spatial resolution is about 1” for the disk and
  2.5” for corona. It also carries an EIT-type telescope in the He II
  (30.4 nm) line. The coronagraph needs a super polished mirror at the
  entrance pupil to minimize the light scattering. Gratings and optical
  filters are used to select the Lyman-α wavelength. VUV cameras with
  2048×2048 pixels record solar images up to every 10 seconds. The
  satellite operates at a high telemetry rate (more then 100 kb/s,
  after onboard data compression). The envisaged orbits are either
  geostationary or heliosynchronous. Possible launch dates could be end
  of 2006 - beginning of 2007.

---------------------------------------------------------
Title: Photon sieves as EUV telescopes for Solar Orbiter
Authors: Artzner, Guy E.; Delaboudiniere, Jean Pierre; Song, Xueyan
2003SPIE.4853..158A    Altcode:
  We elaborate about obtaining images of the solar disc and of the solar
  corona at discrete wavelengths along the EUV emission solar spectrum
  on board the Solar Orbiter spacecraft. Refractive optics cannot be
  used. The thermal load is twenty five times higher than on a near Earth
  orbit. As on one side the efficiency of a stenopeic device is too low,
  and as on the other side mirrors exposed directly to the light and
  to the particles emitted by the Sun may severely degrade during time,
  we investigated using the EUV analog of a Fresnel lens, i.e. a photon
  sieve. An opaque self supporting flat piece of heat resistant metal
  let the solar light shine through a large numbers of a few thousand
  holes properly designed in positions and diameters in order to obtain
  constructive interferences at some focus. We report about practical
  experiments in the visible.

---------------------------------------------------------
Title: Grazing incidence objective grating spectro-imagers for EUV
    observations of the solar corona
Authors: Delaboudiniere, Jean-Pierre; Zhitnik, Igor A.; Ravet,
   Marie-Francoise; Lepere, Didier
2003SPIE.4853..393D    Altcode:
  Objective grating spectrometers have been used previously to image the
  sun in the EUV proving simultaneous images at several wavelengths. The
  grazing incidence variant of this type of instrument seems well adapted
  for application to the future ‘Solar Orbiter’ mission planned by
  the ESA where thermal problems are expected to be severe. This type
  of optical arrangements also provide more flexibility for the optimal
  selection of performances.

---------------------------------------------------------
Title: MAGRITTE / SPECTRE : the Solar Atmospheric Imaging Assembly
    (AIA) aboard the Solar Dynamics Observatory
Authors: Rochus, P.; Defise, J. M.; Halain, J. P.; Mazy, E.; Jamar, C.;
   Clette, F.; Cugnon, P.; Berghmans, D.; Hochedez, J. F.; Delaboudiniere,
   J. P.; Artzner, G.; Auchere, F.; Mercier, R.; Ravet, M. F.; Delmotte,
   M.; Idir, M.; Fineschi, S.; Antonucci, E.; Harrison, R. A.; Howard,
   R. A.; Moses, J. D.; Newmark, J. S.
2002AGUFMSH21C..05R    Altcode:
  The Solar Atmospheric Imaging Assembly (AIA) aboard the Solar
  Dynamics Observatory will characterize the dynamical evolution of
  the solar plasma from the chromosphere to the corona, and will follow
  the connection of plasma dynamics with magnetic activity throughout
  the solar atmosphere. The AIA consists of 7 high resolution imaging
  telescopes in the following spectral bandpasses: 1215 \x8F Ly-a, 304
  \x8F He II, 629 \x8F OV, 465 \x8F Ne VII, 195 \x8F Fe XII (includes Fe
  XXIV), 284 \x8F Fe XV, and 335 \x8F Fe XVI. The telescopes are grouped
  by instrumental approach: the Magritte Filtergraphs (R. Magritte,
  famous 20th Century Belgian Surrealistic Artist), five multilayer EUV
  channels with bandpasses ranging from 195 to 1216 \x8F, and the SPECTRE
  Spectroheliograph with one soft-EUV channel at OV 629 \x8F. They will
  be simultaneously operated with a 10-second imaging cadence. These two
  instruments, the electronic boxes and two redundant Guide Telescopes
  (GT) constitute the AIA suite. They will be mounted and coaligned on a
  dedicated common optical bench. The GTs will provide pointing jitter
  information to the whole SHARPP assembly. This poster presents the
  selected technologies, the different challenges, the trade-offs to be
  made in phase A, and the model philosophy. From a scientific viewpoint,
  the unique combination high temporal and spatial resolutions with the
  simultaneous multi-channel capability will allow Magritte/SPECTRE
  to explore new domains in the dynamics of the solar atmosphere, in
  particular the fast small-scale phenomena. We show how the spectral
  channels of the different instruments were derived to fulfill the
  AIA scientific objectives, and we outline how this imager array will
  address key science issues, like the transition region and coronal waves
  or flare precursors, in coordination with other SDO experiments. We
  finally describe the real-time solar monitoring products that will be
  made available for space-weather forecasting applications.

---------------------------------------------------------
Title: SPIRIT X-ray telescope/spectroheliometer results
Authors: Zhitnik, I. A.; Bougaenko, O. I.; Delaboudiniere, J. -P.;
   Ignatiev, A. P.; Korneev, V. V.; Krutov, V. V.; Kuzin, S. V.; Lisin,
   D. V.; Mitrofanov, A. V.; Oparin, S. N.; Oraevsky, V. N.; Pertsov,
   A. A.; Slemzin, V. A.; Sobelman, I. I.; Stepanov, A. I.; Schwarz, J.
2002ESASP.506..915Z    Altcode: 2002ESPM...10..915Z; 2002svco.conf..915Z
  The SPIRIT X-ray telescope/spectroheliometer successively operates
  on-board the Coronas-F satellite since August 15, 2001. The
  instrument includes two XUV-solar telesocpes - one is a four-band
  Ritchey-Chretien telescope (171, 195, 284 and 304 Å) with the optics
  analogous to the EIT SOHO telesocpe, another - a Herschel two-band
  (175 and 304 Å) telescope with off-axis paraboloids. The last one can
  operate as an XUV-coronagraph with "artificial moons" in the field
  up to 3 R<SUB>Sun</SUB>. The spectroheliometer includes two Mg XII
  (8.42 Å) full-Sun imaging spectrometers, two XUV spectroheliometers
  with objective grazing incidence diffraction gratings, each has two
  selectable spectral bands 177-207 and 285-335 Å, and Bragg crystal
  Fe XXV (1.85-1.87 Å) imaging spectroheliometer. During the first year
  there were observed flares and highly variable active structures in hot
  10 MK Mg XII images, solar XUV-corona, full-Sun XUV spectral images,
  solar XUV-corona, full-Sun XUV spectral images, first separated images
  of solar disk and corona in the He II and Si XI lines (303.78 and
  303.32 Å).

---------------------------------------------------------
Title: Multi wavelength investigation of the eruption of a sigmoidal
    quiescent filament
Authors: Marqué, Ch.; Lantos, P.; Delaboudinière, J. P.
2002A&A...387..317M    Altcode:
  We report the first observation of a filament eruption in the metric and
  decimetric range, where the behavior of the filament can be followed
  during the event via thermal radio emission diagnostics. The event,
  occurring on February 28th 2001, involved a quiescent filament in a
  sigmoid magnetic configuration, whose eruption is triggered by the
  birth of a small parasitic polarity. Faint radio bursts mark the
  beginning of the event, which shows the appearance of a brightness
  temperature depression associated with the filament seen in F0B, and
  its propagation on the disk up to the limb. The event is associated
  with a halo CME observed with the coronagraphs LASCO C2 and C3, which
  shows a significant spatial and temporal continuity with the radio
  observations. Finally, static dimmings, similar to what is currently
  observed in EUV or SXR domains, are also detected in the radio band,
  around the site of the eruption. Movies of the event are attached
  to this article. The movies are available in electronic form at
  http://www.edpsciences.org

---------------------------------------------------------
Title: The August 11th, 1999 total eclipse CME
Authors: Koutchmy, S.; Baudin, F.; Bocchialini, K.; Delaboudinière,
   J. -P.; Adjabshirizadeh, A.
2002ESASP.477...55K    Altcode: 2002scsw.conf...55K
  We use spaceborne observations and ground-based eclipse observations
  to analyse the spectacular W-limb CME which occurred several hours
  after the totality in Iran. The underlying high arch system (possibly
  a dome-like structure with cavities inside) which appeared on the
  eclipse White-Light (W-L) images, is suggested to be a large scale
  precursor of the CME, taking into account the related coronal cavities
  (as measured from the broadening of the green Fe XIV line) and the
  properties of the inserted prominence which erupted during the CME.

---------------------------------------------------------
Title: Coronal Restructuring and Particle Acceleration During
    Relativistic Solar Proton Events
Authors: Klein, K. -L.; Trottet, G.; Delaboudinière, J. P.
2002EGSGA..27.3049K    Altcode:
  The early temporal evolution of four relativistic proton events of the
  current solar cy- cle is compared with broadband radio observations of
  nonthermal electrons and with images of coronal plasma structures (EIT,
  LASCO on SoHO). The events are accom- panied by fast and extended CMEs
  and flares. The data contradict the widely cited idea that flares -
  i.e. small-scale energy release in magnetically stressed structures of
  the corona - are irrelevant to the production of energetic particles
  detected at 1 AU during large "gradual" particle events: We show that
  radio sources at dm-m- (Nançay Radio Heliograph) cover angular ranges
  comparable to the CMEs. Even in cases where the flaring active region
  is poorly connected, a radio source is found close to the nominal
  Earth-connected interplanetary field line. The electron acceleration
  revealed by these sources lasts longer than the soft X-ray event. The
  accelerated electrons may attain mildly relativistic energies. The
  acceleration process is probably related with the re- structuring of
  the corona in the aftermath of the CME, at heights between 0.1 and 1
  solar radius above the photosphere, but clearly not with the front of
  the CME and its presumed shock wave. <P />Since the solar release of
  the relativistic protons is delayed with respect to the flare onset
  during these events, but occurs during the long lasting radio emission,
  we argue that the coronal sites of electron acceleration are plausible
  sources of the relativistic protons detected at 1 AU, too.

---------------------------------------------------------
Title: The Radiometric Calibration of the Extreme Ultraviolet
    Imaging Telescope
Authors: Clette, F.; Hochedez, J. -F.; Newmark, J. S.; Moses, J. D.;
   Auchère, F.; Defise, J. -M.; Delaboudinière, J. -P.
2002ISSIR...2..121C    Altcode: 2002ESASR...2..121C; 2002rcs..conf..121C
  After a five-year effort, the analysis of the pre-flight and in-flight
  calibrations of EIT is finally yielding firm results. In this
  introductory overview, we will summarize what we learned "internally"
  from EIT itself. This includes the interpretation of the pre-flight
  calibrations, the original flat-field components (CCD, grid), the
  in-flight determination of the point-spread function and straylight and
  the compensation of the in-orbit response degradation. Based on this
  experience, we conclude with some suggestions of possible improvements
  to future calibrations, on SOHO and other planned missions.

---------------------------------------------------------
Title: Measurement of coronal magnetic twists during loop emergence
    of NOAA 8069
Authors: Portier-Fozzani, F.; Aschwanden, M.; Démoulin, P.; Neupert,
   W.; EIT Team; Delaboudinière, J. -P.
2001SoPh..203..289P    Altcode:
  Emerging coronal loops were studied with extreme ultraviolet
  observations performed by SOHO/EIT on 5 and 6 August 1997 for NOAA
  8069. Physical parameters (size and twist) were determined by a new
  stereoscopic method. The flux tubes were measured twisted when first
  observed by EIT. After emerging, they de-twisted as they expanded,
  which corresponds to a minimization of the energy. Different scenarios
  which take into account the conservation of the magnetic helicity are
  discussed in relation with structure and temperature variations.

---------------------------------------------------------
Title: Erratum: Coronal electron acceleration and relativistic proton
    production during the 14 July 2000 flare and CME
Authors: Klein, K. -L.; Trottet, G.; Lantos, P.; Delaboudinière,
   J. -P.
2001A&A...377..687K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Coronal electron acceleration and relativistic proton
    production during the 14 July 2000 flare and CME
Authors: Klein, K. -L.; Trottet, G.; Lantos, P.; Delaboudinière,
   J. -P.
2001A&A...373.1073K    Altcode:
  The large solar flare of 14 July 2000 10 UT occurred in an active
  region near the central meridian. It was accompanied by the eruption
  of a filament and a rapid halo-type coronal mass ejection (CME). Large
  particle fluxes were detected up to relativistic energies at 1 AU. In
  this paper accelerated particles and plasma structures in the corona
  are traced using radio, X-ray, EUV and visible light observations,
  together with neutron monitor measurements of relativistic protons
  at 1 AU. Both the bulk of the radio emission at decimetric and longer
  waves and the escape of suprathermal electrons and relativistic protons
  from the Sun were delayed by 10-20 min with respect to the hard X-ray
  emission. Despite the delay and the association with a flare near the
  central meridian the neutron monitor time profile was impulsive. We show
  that the escape of the relativistic protons occurred in time coincident
  both with a coronal shock wave, which may be the bow shock of the CME,
  and with radio sources which trace electron acceleration and magnetic
  field reconfiguration in the western hemisphere. Three observations
  support the idea that the relativistic protons were accelerated
  during this reconfiguration, at heights between 0.1 and 1 R_sun above
  the photosphere, and not in the flaring active region or at the bow
  shock of the CME: (i) the rise of the neutron monitor count rates is
  simultaneous with the brightening of a new continuum radio source;
  (ii) the duration of the continuum emission is similar to the rise
  time of the neutron monitor count rates; (iii) the radio source is
  close to the Earth-connected interplanetary magnetic field line.

---------------------------------------------------------
Title: Calibration and flight of the NRL EIT CalRoc
Authors: Newmark, Jeffrey S.; Moses, J. Daniel; Cook, John W.;
   Delaboudiniere, Jean-Pierre; Song, Xueyan; Carabetian, Charles;
   Bougnet, Marie; Brunaud, Jacqueline; Defise, Jean-Marc; Clette,
   Frederic; Hochedez, Jean-Francois E.
2000SPIE.4139..328N    Altcode:
  The ability to derive physical parameters of the Sun from observations
  by the Solar and Heliospheric Observatory (SOHO) Extreme Ultraviolet
  Imaging Telescope (EIT) greatly increases the scientific return of the
  mission. The absolute and time variable calibration of EIT therefore is
  of extreme interest. The NRL EIT Calibration Sounding Rocket (CalRoc)
  program was initiated to provide well calibrated, contemporaneous
  observations in support of SOHO EIT. These observations provide
  three benefits to the SOHO EIT data, absolute calibration points,
  temporal and spatial information of the EIT EUV response variability
  in flight via flat field information and clues to the physics of the
  degradation. Details of the bandpasses of the multilayered optics and
  the total telescope photometry are presented. Comparisons are shown
  with the contemporaneous images from SOHO EIT. Plans for the second
  CalRoc flight are discussed. Loss of reflectivity in the multilayer
  mirrors has been identified as a new component to the SOHO EIT and
  CalRoc degradation.

---------------------------------------------------------
Title: The Preflight Photometric Calibration of the
    Extreme-Ultraviolet Imaging Telescope EIT
Authors: Dere, K. P.; Moses, J. D.; Delaboudinière, J. -P.; Brunaud,
   J.; Carabetian, C.; Hochedez, J. -F.; Song, X. Y.; Catura, R. C.;
   Clette, F.; Defise, J. -M.
2000SoPh..195...13D    Altcode:
  This paper presents the preflight photometric calibration of the
  Extreme-ultraviolet Imaging Telescope (EIT) aboard the Solar and
  Heliospheric Observatory (SOHO). The EIT consists of a Ritchey-Chrétien
  telescope with multilayer coatings applied to four quadrants of the
  primary and secondary mirrors, several filters and a backside-thinned
  CCD detector. The quadrants of the EIT optics were used to observe
  the Sun in 4 wavelength bands that peak near 171, 195, 284, and 304
  Å. Before the launch of SOHO, the EIT mirror reflectivities, the filter
  transmissivities and the CCD quantum efficiency were measured and these
  values are described here. The instrumental throughput in terms of an
  effective area is presented for each of the various mirror quadrant
  and filter wheel combinations. The response to a coronal plasma as
  a function of temperature is also determined and the expected count
  rates are compared to the count rates observed in a coronal hole,
  the quiet Sun and an active region.

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

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

---------------------------------------------------------
Title: The STEREO-SECCHI Extreme Ultraviolet Imager
Authors: Wülser, J. -P.; Lemen, J. R.; Tarbell, T. D.; Wolfson,
   C. J.; Howard, R. A.; Moses, J. D.; Delaboudinière, J. -P.
2000SPD....31.0294W    Altcode:
  The Extreme Ultraviolet Imager (EUVI) is part of the SECCHI
  investigation selected for flight on the STEREO mission. The twin EUVI
  telescopes on the two STEREO spacecraft will study the structure and
  evolution of the solar corona in three dimensions, and specifically
  focus on the initiation and early evolution of coronal mass ejections
  (CMEs). The EUVI's 2048 x 2048 pixel detectors will have a full sun
  field of view, and will observe in four spectral channels that cover
  the 0.1 to 2 MK temperature range. The EUVI's major advance is its
  view from two vantage points in space. It will allow it to investigate
  the structure of CMEs in three dimensions, while the EUVI's high image
  cadence capability will allow it to resolve the CME's initiation and
  early evolution.

---------------------------------------------------------
Title: The STEREO-SECCHI extreme ultraviolet imager.
Authors: Wülser, J. -P.; Lemen, J. R.; Tarbell, T. D.; Wolfson,
   C. J.; Howard, R. A.; Moses, J. D.; Delaboudinière, J. -P.
2000BAAS...32..827W    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Observation of the origin of CMEs in the low corona
Authors: Delannée, C.; Delaboudinière, J. -P.; Lamy, P.
2000A&A...355..725D    Altcode:
  The aim of the main observing program with EIT on board SOHO,
  is to monitor the whole Sun surface in the Fe xii emission line
  at 195 Ä, every 17 minutes. The very beginning of some CMEs can
  be observed. We interpret Fe xii images in conjunction with He ii,
  Hα and coronagraph observations over a period of 6 days. We find
  that 7 prominences produced ejections. An active region produced 9
  ejections. Five ejections are seen as dark bubbles propagating above
  the solar limb while 9 are seen as dimmings on the solar surface. The
  3 other ejections are bright bubbles observed rising up above the
  limb. Thirteen of the 17 observed ejections are related to a CME. Two
  CMEs of the 15 CMEs observed with LASCO C2 are not related to Fe xii
  low corona events. Probably, these CMEs have their origin behind the
  limb. Prominences give rise to quite slow CMEs, 50-120 km s<SUP>-1</SUP>
  while fast CMEs, 110-1000 km s<SUP>-1</SUP>, originate close to active
  regions. We conclude that CMEs start in the low corona and that large
  scale coronal structures reconfigurations occur when these disturbances
  propagate outward.

---------------------------------------------------------
Title: CMEs Observed Continuously from the Lower Corona to the
    Far Corona
Authors: Delannée, C.; Delaboudinière, J. -P.; Lamy, P.
2000AdSpR..26...67D    Altcode:
  A campaign of observations with EIT on board SOHO called “CME watch”,
  is designed to observe the whole sun surface in 195 A&amp;ring i.e. in a
  Fe XII emission line, every 17 minutes. In order to analyze the events,
  we also used He II and coronagraph observations of 97/11/03. By this
  way, the very beginning of some CMEs was observed. The ejections
  were seen in Fe XII as a dark bubble propagating in the corona
  above a prominence, and dimmings produced near an active region and
  propagating on the solar surface. Two of the ejections coming from
  the active region were produced with a very short time of delay (1
  hour). All the ejections were associated to a CME. However, one CME
  was not related to a Fe xII low corona event, but maybe this CME had
  its origin behind the limb. The CME associated with the prominence
  was quite slow (50 km s<SUP>-1</SUP>) and the ones associated with
  the active region were quite fast (114-490 km s<SUP>-1</SUP>). This
  analysis permitted a better identification of the different CMEs
  appearing in the coronagraph field of view

---------------------------------------------------------
Title: Eclipse of August 11, 1999: White-light Images and Simultaneous
    EIT/SOHO Observations
Authors: Adjabshirizadeh, A.; Baudin, F.; Bocchialini, K.;
   Delaboudinière, J. -P.; Grorod, P. -A.; Koutchmy, S.; Laal Aaly,
   M.; Lamy, P.; Lochard, J.; Mouette, J.
1999ESASP.448.1283A    Altcode: 1999ESPM....9.1283A; 1999mfsp.conf.1283A
  No abstract at ADS

---------------------------------------------------------
Title: The Prolate Solar Chromosphere
Authors: Koutchmy, S.; di Folco, E.; Auchere, F.; Baudin, F.;
   Delaboudinière, J. -P.; Koutchmy, O.; Noëns, J. -C.; Rondi, S.;
   Jimemez, R.; Smartt, R. N.
1999ESASP.446..385K    Altcode: 1999soho....8..385K
  The solar prolateness above h=2Mm is now well established from
  measurements performed during the years of solar minimum in HeII, Hα
  and K3CaII lines. Low level coronal emissions usually penetrate deep
  enough to completely mask this effect and show CH, quite similarly to
  the behaviour of the HeI lines (D3; 1083nm) which does not show the
  prolateness. We discuss the most recent observations for 1999 given
  by a new facility developped at Pic du Midi Observatory (HACO II)
  and we compare the results with EIT results in HeII. We also brielfly
  discuss the possible interpretations of the prolateness effect. We
  favor topological effects implying a large number of nano-flares
  and ejecta during the interactions of small-scale low level network
  magnetic fields with the more static large-scale magnetic field.

---------------------------------------------------------
Title: Helical Magnetic Structure Of EUV Polar Plumes
Authors: Veselovsky, I. S.; Zhukov, A. N.; Koutchmy, S.; Delannée,
   C.; Delaboudinière, J. -P.
1999ESASP.446..675V    Altcode: 1999soho....8..675V
  The results of an analysis of joint CDS of SOHO and SXT of Yohkoh
  observations of a decaying post-flare loop system are presented. The SXT
  images were used to explain some peculiar structural features visible
  in the examined CDS raster, resulting from the rapid evolution of the
  observed system and from the way the CDS rasters are built. The SXT
  data was also used to determine the time evolution of the temperature
  and the emission measure of the hot part of the system during its
  decay. The CDS data, with a very good temperature coverage, contains
  a density sensitive line pair of Fe XIV which was used for electron
  density analysis and a temperature sensitive line pair of Fe XVI and
  Si XII which was used to study the temperature structure of the loop
  system. From the integrated intensities of selected lines the emission
  measures were calculated. From these measurements we estimated the
  filling factor of the loop system in Fe XIV line.

---------------------------------------------------------
Title: Simultaneous LASCO/1998-Eclipse Observations Of A Large-Scale
    Polar Event
Authors: Zhukov, A.; Koutchmy, S.; Lamy, Ph.; Delaboudinière,
   J. -P.; Delannée, C.; Bocchialini, K.; Guisard, S.; Filippov, B.;
   Veselovsky, I.
1999ESASP.446..731Z    Altcode: 1999soho....8..731Z
  A relatively faint but large scale polar region event was observed
  in Aug. 1996 by Boulade et al. 1998 (SoHO SP 404, 217); we first
  reconsider this event which has been related to a high latitude
  filament disappearance. We continue the study of this class of events by
  analyzing the large scale restructuring which occurred above the N-Pole
  region at the time of the last Feb. 26, 1998 total solar eclipse. Well
  calibrated WL-eclipse images are used to provide the absolute values
  of electron densities of the quasi-radial structure appearing at
  the feet of the event. This structure can also be considered as a
  type of abnormally broad and curved polar plume, a type of activity
  already reported in the literature. Unfortunately, the examination
  of sequences of EIT images taken at that time seems to indicate that
  the roots of the structure are on the back side of the Sun. However
  the most impressive effects are seen in the high polar region, at
  several radii, based on the analysis of processed Lasco-C2 difference
  images. Large proper motions are deduced over density structures. Both
  these events confirm that polar regions are indeed showing a new class
  of CME activity (possibly related to the Hewish's CMEs), which is seen
  inside coronal holes. A whole set of interesting questions is then
  appearing to understand the occurrence of a polar CME propagating in
  the heart of a large unipolar magnetic region of the corona.

---------------------------------------------------------
Title: Resonance Scattering of 30.4 NM Chromospheric Radiation by
    Coronal Singly Ionized Helium Observed with EIT
Authors: Delaboudinière, J. P.
1999SoPh..188..259D    Altcode:
  A diffuse emission is observed above the solar limb in the `304 Å'
  channel of the Extreme-Ultraviolet Imaging Telescope (EIT) onboard
  the SOHO spacecraft. Part of this emission is attributed to the
  presence of residual singly-ionized helium in the solar corona,
  which resonantly scatters the intense helium `Lyman alpha' radiation
  of the chromosphere. This emission can be distinguished from other
  coronal emissions in the EIT bandpass. Maps of the helium ion density
  integrated along the line of sight are derived. These agree well with
  models in the low latitude, closed magnetic field regions of the solar
  corona. However, the helium ions' abundance seems to be enhanced in
  the polar, open field regions above coronal holes. This may be related
  to acceleration processes of the fast solar wind close to the Sun.

---------------------------------------------------------
Title: Equivalent focal length measurements
Authors: Artzner, Guy E.; Auchere, Frederic; Delaboudiniere,
   Jean-Pierre; Hochedez, Jean-Francois E.
1999SPIE.3737...32A    Altcode:
  Converting linear coordinates in the plane of the detector of
  an astronomical instrument to celestial coordinates involves in
  principle the equivalent focal length of the instrument. However,
  most methods in astrometry manage to reduce observations in a global
  manner without actually measuring a focal length. We point out a case
  for solar space observations where the long term stability of angular
  distance measurements is better than the ground calibration of the
  angular value of a pixel. We report and discuss this ground calibration.

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

---------------------------------------------------------
Title: LASCO and EIT Observations of Helical Structure in Coronal
    Mass Ejections
Authors: Dere, K. P.; Brueckner, G. E.; Howard, R. A.; Michels, D. J.;
   Delaboudiniere, J. P.
1999ApJ...516..465D    Altcode:
  Observations of coronal mass ejections (CMEs) by the Large Angle
  Spectrometric Coronagraph (LASCO) on the Solar and Heliospheric
  Observatory (SOHO) show a significant fraction with circular intensity
  patterns. In the past, these would have been called “disconnection”
  events, but we suggest that these are evidence of CMEs containing
  helical magnetic flux ropes that are often central to many theoretical
  models of CMEs and have been observed in magnetic clouds near
  1 AU. Three examples are examined in detail with the LASCO and
  Extreme-Ultraviolet Imaging Telescope (EIT) data sets, which provide
  observations from their initiation through 30 R<SUB>solar</SUB>.

---------------------------------------------------------
Title: Three-dimensional Stereoscopic Analysis of Solar Active
    Region Loops. I. SOHO/EIT Observations at Temperatures of (1.0-1.5)
    × 10<SUP>6</SUP> K
Authors: Aschwanden, Markus J.; Newmark, Jeffrey S.; Delaboudinière,
   Jean-Pierre; Neupert, Werner M.; Klimchuk, J. A.; Gary, G. Allen;
   Portier-Fozzani, Fabrice; Zucker, Arik
1999ApJ...515..842A    Altcode:
  The three-dimensional structure of solar active region NOAA 7986
  observed on 1996 August 30 with the Extreme-Ultraviolet Imaging
  Telescope (EIT) on board the Solar and Heliospheric Observatory
  (SOHO) is analyzed. We develop a new method of dynamic stereoscopy to
  reconstruct the three-dimensional geometry of dynamically changing
  loops, which allows us to determine the orientation of the mean
  loop plane with respect to the line of sight, a prerequisite to
  correct properly for projection effects in three-dimensional loop
  models. With this method and the filter-ratio technique applied
  to EIT 171 and 195 Å images we determine the three-dimensional
  coordinates [x(s), y(s), z(s)], the loop width w(s), the electron
  density n<SUB>e</SUB>(s), and the electron temperature T<SUB>e</SUB>(s)
  as a function of the loop length s for 30 loop segments. Fitting the
  loop densities with an exponential density model n<SUB>e</SUB>(h)
  we find that the mean of inferred scale height temperatures,
  T<SUP>λ</SUP><SUB>e</SUB>=1.22+/-0.23 MK, matches closely that of EIT
  filter-ratio temperatures, T<SUP>EIT</SUP><SUB>e</SUB>=1.21+/-0.06
  MK. We conclude that these cool and rather large-scale loops (with
  heights of h~30-225 Mm) are in hydrostatic equilibrium. Most of the
  loops show no significant thickness variation w(s), but we measure
  for most of them a positive temperature gradient (dT/ds&gt;0) across
  the first scale height above the footpoint. Based on these temperature
  gradients we find that the conductive loss rate is about 2 orders of
  magnitude smaller than the radiative loss rate, which is in strong
  contrast to hot active region loops seen in soft X-rays. We infer a
  mean radiative loss time of τ<SUB>rad</SUB>~40 minutes at the loop
  base. Because thermal conduction is negligible in these cool EUV
  loops, they are not in steady state, and radiative loss has entirely
  to be balanced by the heating function. A statistical heating model
  with recurrent heating events distributed along the entire loop can
  explain the observed temperature gradients if the mean recurrence time
  is &lt;~10 minutes. We computed also a potential field model (from
  SOHO/MDI magnetograms) and found a reasonable match with the traced
  EIT loops. With the magnetic field model we determined also the height
  dependence of the magnetic field B(h), the plasma parameter β(h),
  and the Alfvén velocity v<SUB>A</SUB>(h). No correlation was found
  between the heating rate requirement E<SUB>H0</SUB> and the magnetic
  field B<SUB>foot</SUB> at the loop footpoints.

---------------------------------------------------------
Title: Evolution of Chromospheric Structures: How Chromospheric
    Structures Contribute to the Solar HE II 30.4 Nanometer Irradiance
    and Variability
Authors: Worden, John; Woods, Thomas N.; Neupert, Werner M.;
   Delaboudinière, Jean-Pierre
1999ApJ...511..965W    Altcode:
  The bright He II 30.4 nm solar emission is an important energy source
  for ionization and heating of the Earth's upper atmosphere. The analysis
  of the Solar and Heliospheric Observatory (SOHO) Extreme-Ultraviolet
  Imaging Telescope (EIT) He II 30.4 nm images provides an improved
  understanding of how the solar surface structures, i.e., plage,
  enhanced network (plage remnants), active network, and the quiet
  chromosphere, contribute to the solar He II 30.4 nm irradiance and
  its variability. We first normalize the intensities of each image
  to the background quiet-chromosphere intensity with a global fit
  that preferentially weights network cell intensities. The resulting
  quiet-chromosphere intensity scale is stable to within 0.7% (1 σ)
  over the 2 yr data set. The plage, enhanced-network, active-network,
  and quiet-chromosphere structures are then identified on each EIT
  He II image with an algorithm that uses criteria of intensity,
  size, filling factor, and continuity. This decomposition leads to
  time series of structure area and integrated intensity, their spatial
  distribution on the solar disk, and their intensity contrast relative to
  the quiet-chromosphere intensity; thus, these time series show how the
  solar surface structures contribute to the He II 30.4 nm irradiance. For
  example, we find that the active network contributes as much as the
  plage and enhanced network to the solar He II 30.4 nm irradiance
  variability during solar minimum. Conversely, the quiet-chromosphere
  irradiance does not vary during this time period; thus we conclude that
  long-term He II 30.4 nm irradiance variations can be traced purely
  to magnetic activity during this time period. We also find that the
  plage, enhanced-network, active-network, and quiet-network intensity
  contrasts, relative to the quiet chromosphere and averaged over the
  full area of each structure, are 4.8, 3.3, 2.1, and 1.6, respectively,
  and these contrasts remain essentially constant with time.

---------------------------------------------------------
Title: Eruptive filament of May 31, 1997, observed by SOHO.
Authors: Schmieder, B.; Heinzel, P.; Vial, J. -C.; Delaboudinière,
   J. -P.; Delannée, C.
1999joso.proc..147S    Altcode:
  In the frame of the SUMER/CDS Joint Programme (JOP 17) the authors
  have detected the four Lyman lines in an erupting filament. The
  strong self-absorption in these lines, already reported for quiescent
  filaments, is still present in this highly dynamical event, but the
  authors observe a significant red asymmetry in the intensities of the
  two peaks. They ascribe it to an upward bulk motion of the filament,
  which they can actually see on a series of EIT images taken in the
  Fe XII line. Both sets of observations can lead to a determination
  of the velocity vector. The Doppler velocities are also derived from
  other lines detected by SUMER/CDS and can be correlated with the
  observations of the Pic-du-Midi MSDP obtained for this event. The
  filament eruption was also well observed by other GBO instruments in
  the Hα line (Meudon and Ondřejov).

---------------------------------------------------------
Title: CME observed continuously from the lower corona to the far
    corona (CME's onset on November 3, 1997).
Authors: Delannée, C.; Delaboudinière, J. -P.; Lamy, P.
1999joso.proc..162D    Altcode:
  A program of observations with EIT on board SOHO, is to observe the
  whole sun surface in 195 Å, i.e. in a Fe XII emission line, every
  17 minutes. The very beginning of some CMEs is observed. The authors
  correlate each Fe XII observation with He II, Hα and coronagraph
  observations on 97/11/03 and 97/11/04. They found that three prominences
  were ejected, and that an active region produced 4 ejections. The
  ejections are dark bubbles propagating above the sun limb, and dimmings
  propagating on the solar surface in Fe XII. They each produced an
  associated CME. One CME was not correlated to a Fe XII low corona
  event. Maybe, this CME had its origin behind the limb. The prominence
  gave a quite slow CME, i.e. about 50 km s<SUP>-1</SUP> and the active
  region produced some quite fast CMEs, i.e. about 300 km s<SUP>-1</SUP>.

---------------------------------------------------------
Title: Observations of Correlated White-Light and Extreme-Ultraviolet
    Jets from Polar Coronal Holes
Authors: Wang, Y. -M.; Sheeley, N. R., Jr.; Socker, D. G.; Howard,
   R. A.; Brueckner, G. E.; Michels, D. J.; Moses, D.; St. Cyr, O. C.;
   Llebaria, A.; Delaboudinière, J. -P.
1998ApJ...508..899W    Altcode:
  Time-lapse sequences of white-light images recorded with the Large
  Angle Spectrometric Coronagraph (LASCO) on the Solar and Heliospheric
  Observatory (SOHO) frequently show long, narrow structures moving
  outward over the Sun's polar regions at high apparent speeds. By
  comparing the LASCO observations with Fe XII λ195 spectroheliograms
  made with the Extreme-ultraviolet Imaging Telescope (EIT) on SOHO
  between 1997 April and 1998 February, we have identified 27 correlated
  white-light and extreme-ultraviolet (EUV) jet events. In each case,
  the EUV jet was observed near the limb of the polar coronal hole 20-60
  minutes before the corresponding white-light jet was registered in the
  coronagraph's 2-6 R<SUB>⊙</SUB> field of view. The jets originate
  near flaring EUV bright points and are presumably triggered by field
  line reconnection between magnetic bipoles and neighboring unipolar
  flux. The leading edges of the white-light jets propagate outward at
  speeds of 400-1100 km s<SUP>-1</SUP>, whereas the bulk of their material
  travels at much lower velocities averaging around 250 km s<SUP>-1</SUP>
  at heliocentric distances of 2.9-3.7 R<SUB>⊙</SUB>. These lower
  velocities may reflect the actual outflow speeds of the background
  polar wind.

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

---------------------------------------------------------
Title: The prolate solar chromosphere
Authors: Auchere, F.; Boulade, S.; Koutchmy, S.; Smartt, R. N.;
   Delaboudiniere, J. P.; Georgakilas, A.; Gurman, J. B.; Artzner, G. E.
1998A&A...336L..57A    Altcode:
  We present a comparative analysis of the chromospheric solar
  limb prolateness, using strictly simultaneous H_alpha ground-based
  observations and Heriptsize{II} space-based observations. The typical
  prolateness is found to be Delta D/D=5.5*E(-3) in Heriptsize{II}
  and 1.2*E(-3) in H_alpha . The first measurements in the 30.4 nm
  Heriptsize{II} line over a period of two years, as well as coronal
  data, are discussed to explore further the origin of the prolateness
  and its possible consequences.

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

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

---------------------------------------------------------
Title: Statistical analysis of solar bright points observed with
    the SOHO spacecraft.
Authors: Régnier, S.; Bocchialini, K.; Vial, J. -C.; Delaboudinière,
   J. -P.; Thompson, W.
1998CRASB.326..211R    Altcode: 1998CR2...326..211R
  Bright points, small and short lifetime structures, appear permanently
  in the atmosphere and could be associated with magnetic reconnections,
  potential sources of coronal heating. Such structures have been
  observed with the coronal instruments on-board SOHO and a statistical
  analysis was carried out in order to find the signature of very small
  scale structures.

---------------------------------------------------------
Title: The polar extension of the solar chromosphere
Authors: Auchère, F.; Delaboudinière, J. P.; Koutchmy, S.;
   Boulade, S.
1998ESASP.421..245A    Altcode: 1998sjcp.conf..245A
  No abstract at ADS

---------------------------------------------------------
Title: 3D-Stereoscopic Analysis of Solar Active Region Loops Observed
    with SOHO/EIT
Authors: Aschwanden, M. J.; Newmark, J. S.; Delaboudiniere, J. -P.;
   Neupert, W. M.; Klimchuk, J. A.; Gary, G. Allen; Portier-Fozzani,
   F.; Zucker, A.
1998cee..workE..19A    Altcode:
  The three-dimensional (3D) structure of solar active region NOAA
  7986 observed on 1996 August 30 with the Extrem-ultraviolet Imaging
  Telescope (EIT) onboard the Solar and Heliospheric Observatory
  (SoHO) is analyzed. We develop a new method of Dynamic Stereoscopy to
  reconstruct the 3D geometry of dynamically changing loops, which allows
  us to determine the orientation of the loop plane with respect to
  the line-of-sight, a prerequisite to correct properly for projection
  effects in 3D loop models. With this method and the filter-ratio
  technique applied to EIT 171 angle and 195 angle images we determine
  the 3D coordinates [x(s),y(s),z(s)], the loop width w(s), the electron
  density n_e(s), and the electron temperature T_e(s) as function of
  the loop length s for 30 loop segments. Fitting the loop densities
  with an exponential density model n_e(h) we find that the mean of
  inferred scale height temperatures, T_e<SUP>lambda</SUP> = 1.22 plus or
  minus 0.23 MK, matches closely that of EIT filter-ratio temperatures,
  T_e<SUP>EIT</SUP> = 1.21 plus or minus 0.06 MK. We conclude that these
  cool and rather large-scale loops (with heights of h ~30-225 Mm), which
  dominate the EIT 171 angle images, are in hydrostatic equilibrium. Most
  of the loops show no significant thickness variation w(s), but we can
  measure for most of them a positive temperature gradient (dT/ds &gt;
  0) across the first scale height above the footpoint. Based on these
  temperature gradients we find that the conductive loss rate is about
  two orders of magnitude smaller than the radiative loss rate, which is
  in strong contrast to hot active region loops seen in SXR. We infer a
  mean radiative loss time of τ<SUB>rad</SUB> ~40 minutes. For steady
  state models, the heating rate has to balance the radiative loss,
  i.e. the heating rate has to scale with the squared density (E_H
  propto n_e^2). From potential-field extrapolations we determine also
  the magnetic field strength B(s), the plasma beta-parameter beta(s),
  and the Alfven velocity v_A(s) along the loops, and discuss the findings
  in the context of coronal heating models.

---------------------------------------------------------
Title: About polar ejection events and surges
Authors: Loucif, M. L.; Koutchmy, S.; Stellmacher, G.; Georgakilas,
   A.; Bocchialini, K.; Delaboudinière, J. -P.
1998ESASP.421..299L    Altcode: 1998sjcp.conf..299L
  No abstract at ADS

---------------------------------------------------------
Title: EUV and Microwave Observations of a Filament
Authors: Chiuderi-Drago, F.; Bocchialini, K.; Lamartinie, S.;
   Vial, J. -C.; Bastian, T.; Alissandrakis, C. E.; Harrison, R.;
   Delaboudiniere, J. -P.; Lemaire, P.
1998ASPC..150...55C    Altcode: 1998IAUCo.167...55C; 1998npsp.conf...55C
  No abstract at ADS

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

---------------------------------------------------------
Title: Spicules and Macrospicules: Simultaneous Hα and He II (304
    Å) Observations
Authors: Georgakilas, A. A.; Dara, H.; Zachariadis, Th.; Alissandrakis,
   C. E.; Koutchmy, S.; Delannée, C.; Delaboudinière, J. -P.; Hochedez,
   J. -F.
1998ASPC..155..376G    Altcode: 1998sasp.conf..376G
  No abstract at ADS

---------------------------------------------------------
Title: European Plans for the Solar/Heliospheric Stereo Mission
Authors: Bothmer, V.; Bougeret, J. -L.; Cargill, P.; Davila, J.;
   Delaboudiniere, J. -P.; Harrison, R.; Koutchmy, S.; Liewer, P.;
   Maltby, P.; Rust, D.; Schwenn, R.
1998ESASP.417..145B    Altcode: 1998cesh.conf..145B
  No abstract at ADS

---------------------------------------------------------
Title: Velocity Fields of a Filament Region Observed with Ground-Based
    Telescopes and from SOHO
Authors: Mein, P.; Schmieder, B.; Malherbe, J. -M.; Wiik, J. E.;
   Engvold, O.; Brekke, P.; Zirker, J. B.; Poland, A. I.; Delaboudiniere,
   J. -P.; Staiger, J.
1998ASPC..150..135M    Altcode: 1998npsp.conf..135M; 1998IAUCo.167..135M
  No abstract at ADS

---------------------------------------------------------
Title: Polar jets and plasmoids:Results from JOP 57
Authors: Delannee, C.; Koutchmy, S.; Delaboudiniere, J. -P.; Hochedez,
   J. -F.; Vial, J. -C.; Dara, H.; Georgakilas, A.
1998ESASP.421..129D    Altcode: 1998sjcp.conf..129D
  No abstract at ADS

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

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

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

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

---------------------------------------------------------
Title: EIT and LASCO Observations of the Initiation of a Coronal
    Mass Ejection
Authors: Dere, K. P.; Brueckner, G. E.; Howard, R. A.; Koomen, M. J.;
   Korendyke, C. M.; Kreplin, R. W.; Michels, D. J.; Moses, J. D.;
   Moulton, N. E.; Socker, D. G.; St. Cyr, O. C.; Delaboudinière, J. P.;
   Artzner, G. E.; Brunaud, J.; Gabriel, A. H.; Hochedez, J. F.; Millier,
   F.; Song, X. Y.; Chauvineau, J. P.; Marioge, J. P.; Defise, J. M.;
   Jamar, C.; Rochus, P.; Catura, R. C.; Lemen, J. R.; Gurman, J. B.;
   Neupert, W.; Clette, F.; Cugnon, P.; Van Dessel, E. L.; Lamy, P. L.;
   Llebaria, A.; Schwenn, R.; Simnett, G. M.
1997SoPh..175..601D    Altcode:
  We present the first observations of the initiation of a coronal mass
  ejection (CME) seen on the disk of the Sun. Observations with the EIT
  experiment on SOHO show that the CME began in a small volume and was
  initially associated with slow motions of prominence material and a
  small brightening at one end of the prominence. Shortly afterward,
  the prominence was accelerated to about 100 km s<SUP>-1</SUP> and
  was preceded by a bright loop-like structure, which surrounded an
  emission void, that traveled out into the corona at a velocity of
  200-400 km s<SUP>-1</SUP>. These three components, the prominence,
  the dark void, and the bright loops are typical of CMEs when seen at
  distance in the corona and here are shown to be present at the earliest
  stages of the CME. The event was later observed to traverse the LASCO
  coronagraphs fields of view from 1.1 to 30 R⊙. Of particular interest
  is the fact that this large-scale event, spanning as much as 70 deg in
  latitude, originated in a volume with dimensions of roughly 35" (2.5
  x 10<SUP>4</SUP> km). Further, a disturbance that propagated across
  the disk and a chain of activity near the limb may also be associated
  with this event as well as a considerable degree of activity near the
  west limb.

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

---------------------------------------------------------
Title: EIT and LASCO observations of the initiation of a coronal
    mass ejection
Authors: Dere, K.; Brueckner, G. E.; Delaboudiniere, J. -P.
1997SPD....28.0502D    Altcode: 1997BAAS...29R.908D
  We present the first observations of the initiation of a coronal mass
  ejection (CME) seen on the disk of the Sun. Observations with the EIT
  experiment on SOHO show that the CME began in a small volume and was
  initially associated with slow motions of prominence material and a
  small brightening at one end of the prominence. Shortly afterward,
  the prominence was accelerated to about 200 kms and was preceded by
  a bright loop-like structure, which surrounded an emission void,
  that traveled out into the corona at a velocity of 400 kms. These
  three components, the prominence, the dark void, and the bright loops
  are typical of CMEs when seen at distance in the corona and here are
  shown to be present at the earliest stages of the CME. The event was
  later observed to traverse the LASCO coronagraphs fields of view from
  1.1 to 30 R_⊙. Of particular interest is the fact that this large
  scale event, spanning as much as 70 degrees in latitude, originated
  in a volume with dimensions of roughly 35" (2.5 x 10(4) km). Further,
  a disturbance that propagated across the disk and a chain of activity
  near the limb may also be associated with this event as well as a
  considerable degree of activity near the west limb.

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

---------------------------------------------------------
Title: Imaging the solar corona in the EUV
Authors: Delaboudiniere, J. -P.; Stern, R. A.; Maucherat, A.;
   Portier-Fozzani, F.; Neupert, W. M.; Gurman, J. B.; Catura, R. C.;
   Lemen, J. R.; Shing, L.; Artzner, G. E.; Brunaud, J.; Gabriel, A. H.;
   Michels, D. J.; Moses, J. D.; Au, B.; Dere, K. P.; Howard, R. A.;
   Kreplin, R.; Defise, J. M.; Jamar, C.; Rochus, P.; Chauvineau, J. P.;
   Marioge, J. P.; Clette, F.; Cugnon, P.; van Dessel, E. L.
1997AdSpR..20.2231D    Altcode:
  The SOHO (SOlar and Heliospheric Observatory) satellite was launched on
  December 2nd 1995. After arriving at the Earth-Sun (L1) Lagrangian point
  on February 14th 1996, it began to continuously observe the Sun. As
  one of the instruments onboard SOHO, the EIT (Extreme ultraviolet
  Imaging Telescope) images the Sun's corona in 4 EUV wavelengths. The
  He II filter at 304 A˚ images the chromosphere and the base of the
  transition region at a temperature of 5 - 8 x 10^4 K; the Fe IX-X
  filter at 171 A˚ images the corona at a temperature of ~ 1.3 x 10^6 K;
  the Fe XII filter at 195 A˚ images the quiet corona outside coronal
  holes at a temperature of ~ 1.6 x 10^6 K; and the Fe XV filter at 284
  A˚ images active regions with a temperature of ~ 2.0 x 10^6 K. About
  5000 images have been obtained up to the present. In this paper,
  we describe also some aspects of the telescope and the detector
  performance for application in the observations. Images and movies
  of all the wavelengths allow a look at different phenomena present in
  the Sun's corona, and in particular, magnetic field reconnection.

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

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

---------------------------------------------------------
Title: Coronal EUV and Radio Variability and Heating
Authors: Krucker, S.; Benz, A. O.; Delaboudinière, J. -P.
1997ESASP.404..465K    Altcode: 1997cswn.conf..465K
  No abstract at ADS

---------------------------------------------------------
Title: EIT and LASCO Observations of the Initiation of a Coronal
    Mass Ejection
Authors: Dere, K. P.; Brueckner, G. E.; Howard, R. A.; Koomen, M. J.;
   Korendyke, C. M.; Michels, D. J.; Moses, J. D.; Moulton, N. E.; Socker,
   D. G.; Delaboudiniere, J. P.; Hochedez, J. F.; Lamy, P. L.; Schwenn,
   R.; Simnett, G. M.; Defise, J. M.; Catura, R. C.
1997IAUJD..19E..18D    Altcode:
  We present the first observations of the initiation of a corona mass
  ejection (CME) seen on the disk of the Sun. Observations with the EIT
  and LASCO experiments on SOHO show that the CME starts in a small volume
  and is associated with slow motions of prominence material. At about
  the same time, a shock wave is created that travels out into the corona
  at a velocity of 400 km s^{-1} ahead of an eruptive prominence. This
  shock wave is clearly the event that is later seen as a classical CME
  when observed in the coronagraph above 1.5 solar radii. Although the
  CME clearly starts in a small region, a chain of activity near the
  limb may also be associated with this event.

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

---------------------------------------------------------
Title: First Results from EIT
Authors: Clette, F.; Delaboudiniere, J. -P.; Artzner, G. E.; Brunaud,
   J.; Gabriel, A. H.; Hochedez, J. -F.; Millier, F.; Song, X. Y.; Au, B.;
   Dere, K. P.; Howard, R. A.; Kreplin, R.; Michels, D. J.; Moses, J. D.;
   Defise, J. -M.; Jamar, C.; Rochus, P.; Chauvineau, J. -P.; Marioge,
   J. -P.; Catura, R. C.; Lemen, J. R.; Shing, L.; Stern, R. A.; Gurman,
   J. B.; Neupert, W. M.; Maucherat, A.; Cugnon, P.; van Dessel, E. L.
1997ASPC..118..268C    Altcode: 1997fasp.conf..268C
  The Extreme-UV Imaging telescope has already produced more than 15000
  wide-field images of the corona and transition region, on the disk
  and up to 1.5R_⊙ above the limb, with a pixel size of 2.6\arcsec. By
  using four different emission lines, it provides the global temperature
  distribution in the quiet corona, in the range 0.5 to 3*E(6) K. Its
  excellent sensitivity and wide dynamic range allow unprecedented views
  of low emission features, even inside coronal holes. Those so-called
  “quiet” regions actually display a wide range of dynamical phenomena,
  in particular at small spatial scales and at time scales going down
  to only a few seconds, as revealed by all EIT time sequences of
  full- or partial-field images. The initial results presented here
  demonstrate the importance of this wide-field imaging experiment for
  a good coordination between SOHO and ground-based solar telescopes,
  as well as for science planning.

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

---------------------------------------------------------
Title: Observations of the South coronal hole from EIT and YOHKOH
Authors: Handy, B. N.; Catura, R.; Freeland, S.; Lemen, J.; Stern,
   R.; Gurman, J. B.; Delaboudiniere, J. P.; Artzner, G.; Gabriel, A.;
   Maucherat, A.; Defise, J. M.; Jamar, C.; Rochus, P.; Clette, F.;
   Cugnon, P.; Howard, R.; Michels, D.; Moses, J. D.; Dere, K.; Cyr,
   O. C. St.; Catura, R.; Freeland, S.; Lemen, J.; Stern, R.; Neupert,
   W.; Einfalt, E.; Newmark, J.
1996AAS...188.0206H    Altcode: 1996BAAS...28..821H
  The Extreme ultraviolet Imaging Telescope (EIT) on board the
  SOHO spacecraft is capable of studying solar transition region,
  chomospheric and coronal plasmas over bandpasses optimized for He II
  304 Angstroms (0.08 MK), Fe IX/X 171, 173 Angstroms (0.8 - 1.0 MK),
  Fe XII 195 Angstroms (1.5 MK), and Fe XV 284 Angstroms (2.0 - 2.5
  MK) with 2.5 arcsecond spatial resolution. This telescope in concert
  with the Yohkoh/SXT instrument allows us to simultaneously observe
  solar structures at temperatures ranging from less than 0.1MK in the
  transition region to over 3MK in the solar corona. EIT has had several
  opportunities to observe the South coronal hole with high spatial and
  temporal resolution. We compare observations from EIT and SXT with
  an eye towards correlating temporal variations over the range of
  wavelengths, activity of polar crown filament systems and relating
  large-scale morphology of the X-ray corona to the transition region
  in He II.

---------------------------------------------------------
Title: There's No Such Thing as the Quiet Sun: EUV Movies from SOHO
Authors: Gurman, J. B.; Delaboudiniere, J. P.; Artzner, G.; Gabriel,
   A.; Maucherat, A.; Defise, J. M.; Jamar, C.; Rochus, P.; Clette, F.;
   Cugnon, P.; Howard, R.; Michels, D.; Moses, J. D.; Dere, K.; Cyr,
   O. C. St.; Catura, R.; Freeland, S.; Lemen, J.; Stern, R.; Neupert,
   W.; Einfalt, E.; Newmark, J.
1996AAS...188.3718G    Altcode: 1996BAAS...28..880G
  We present unique time series of high-resolution solar images from the
  normal-incidence Extreme ultraviolet Imaging Telescope (EIT) on board
  the SOHO spacecraft. With a pixel scale of 2.6 arc sec and a detector
  dynamic range of &gt; 10(4) , the EIT can be used to study the dynamics
  of chromospheric and coronal features in multilayer bandpasses optimized
  for He II 304 Angstroms (0.08 MK), Fe IX/X 171, 173 Angstroms (0.8 -
  1.0 MK), Fe XII 195 Angstroms (1.5 MK), and Fe XV 284 Angstroms (2.0 -
  2.5 MK). Among the most striking features of the digital movies we will
  display are: the dynamic nature of small-scale loop features in the
  polar coronal holes, the constant activity of the polar crown filament
  systems, the locations of the bases of polar plumes, the presence
  of dark (scattering) filament material in the coronal emission line
  images, and the evolution of a unique, linear, dark feature in a young
  active region. The latter feature is suggestive of the “coronal void”
  observed in the electron scattering corona by Macqueen et al./ (1983).

---------------------------------------------------------
Title: Observations of the south coronal hole from EIT and Yohkoh.
Authors: Handy, B. N.; Catura, R.; Freeland, S.; Lemen, J.; Stern,
   R.; Gurman, J. B.; Delaboudinière, J. P.; Artzner, G.; Gabriel,
   A.; Maucherat, A.; Defise, J. M.; Jamar, C.; Rochus, P.; Clette, F.;
   Cugnon, P.; Howard, R.; Michels, D.; Moses, J. D.; Dere, K.; St. Cyr,
   O. C.; Neupert, W.; Einfalt, E.; Newmark, J.
1996BAAS...28Q.821H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: EIT Images of the EUV Solar Atmosphere
Authors: Portier-Fozzani, F.; Moses, J. D.; Delaboudiniere, J. P.;
   Gurman, J. B.; Clette, F.; Maucherat, A.
1996ASPC..111..402P    Altcode: 1997ASPC..111..402P
  The Extreme-ultraviolet Imaging Telescope (EIT) was one of several
  instruments launched on board SOHO on 1995 Dec 2. It has already
  produced thousands of wide-field images of the low corona at 4
  wavelengths (171, 195, 284 and 304 Å). These wavelengths correspond
  to different emission lines, formed over a wide range of plasma
  temperatures. The first EIT images and movies reveal how this sensitive
  instrument will provide unprecedented information about the dynamics
  of small scale phenomena in the quiet solar corona and inside coronal
  holes. Results of a local deconvolution method, used to correct a grid
  pattern present in raw EIT images, are also presented.

---------------------------------------------------------
Title: EIT: Extreme-Ultraviolet Imaging Telescope for the SOHO Mission
Authors: Delaboudinière, J. -P.; Artzner, G. E.; Brunaud, J.; Gabriel,
   A. H.; Hochedez, J. F.; Millier, F.; Song, X. Y.; Au, B.; Dere, K. P.;
   Howard, R. A.; Kreplin, R.; Michels, D. J.; Moses, J. D.; Defise,
   J. M.; Jamar, C.; Rochus, P.; Chauvineau, J. P.; Marioge, J. P.;
   Catura, R. C.; Lemen, J. R.; Shing, L.; Stern, R. A.; Gurman, J. B.;
   Neupert, W. M.; Maucherat, A.; Clette, F.; Cugnon, P.; Van Dessel,
   E. L.
1995SoPh..162..291D    Altcode:
  The Extreme-ultraviolet Imaging Telescope (EIT) will provide wide-field
  images of the corona and transition region on the solar disc and up to
  1.5 R⊙ above the solar limb. Its normal incidence multilayer-coated
  optics will select spectral emission lines from Fe IX (171 å), Fe
  XII (195 å), Fe XV (284 å), and He II (304 å) to provide sensitive
  temperature diagnostics in the range from 6 × 10<SUP>4</SUP> K to 3
  × 10<SUP>6</SUP> K. The telescope has a 45 x 45 arcmin field of view
  and 2.6 arcsec pixels which will provide approximately 5-arcsec spatial
  resolution. The EIT will probe the coronal plasma on a global scale,
  as well as the underlying cooler and turbulent atmosphere, providing
  the basis for comparative analyses with observations from both the
  ground and other SOHO instruments. This paper presents details of the
  EIT instrumentation, its performance and operating modes.

---------------------------------------------------------
Title: Calibration of the EIT instrument for the SOHO mission
Authors: Defise, Jean-Marc; Song, Xueyan Y.; Delaboudiniere,
   Jean-Pierre; Artzner, Guy E.; Carabetian, Charles; Hochedez,
   Jean-Francois E.; Brunaud, Jacqueline; Moses, John D.; Catura,
   Richard C.; Clette, Frederic; Maucherat, Andre J.
1995SPIE.2517...29D    Altcode:
  Optical characteristics in the wavelength range 15 - 75 nm of the
  EUV imaging telescope to be launched soon on the SOHO mission are
  discussed. Bandpasses and photometric sensitivity of the multilayered
  optics telescope have been measured by a dedicated synchrotron light
  source at Orsay, France.

---------------------------------------------------------
Title: EIT: The Extreme Ultraviolet Imaging Telescope. Synoptic
    Observations of Small and Large-Scale Coronal Structures
Authors: Clette, F.; Delaboudinière, J. P.; Dere, K. P.; Cugnon,
   P.; EIT Science Team
1995LNP...444..251C    Altcode: 1995cmer.conf..251C
  The EIT will provide wide-field images of the corona and transition
  region, on the solar disc and up to 1 R<SUB>⊙</SUB> above the
  limb. Its normal incidence multilayer-coated optics will select the
  spectral emission lines of four ions (Fe IX, 171 Å; Fe XII, 195
  Å; Fe XV, 284 Å; Hell, 304 Å), providing a sensitive temperature
  diagnostic in the range 6.10<SUP>4</SUP> to 3.10<SUP>6</SUP>K. This
  SOHO instrument will thus probe the coronal plasma on a global scale,
  as well as the underlying cooler and turbulent atmosphere. The EIT's
  characteristics and performances are presented, and prospects for
  coordinated observations with ground-based radio observatories are
  outlined.

---------------------------------------------------------
Title: EUVITA — An extreme UV imaging telescope array with spectral
    capability
Authors: Courvoisier, T. J. -L.; Orr, A.; Bühler, P.; Zchnder,
   A.; Henneck, R.; Stauffacher, F.; Biakhowski, J.; Schlumpf, N.;
   Schoeps, W.; McHedlishvili, A.; Sunyaev, R.; Arefev, V.; Yascovich,
   A.; Babalyan, G.; Pavlinsky, M.; Delaboudinière, J. P.; Carone, T.;
   Siegmund, O.; Warren, J.; Leahy, D.; Salaschenko, N.; Platonov, J.
1993AdSpR..13l.299C    Altcode: 1993AdSpR..13..299C
  EUVITA is a set of 8 extreme UV normal incidence imaging telescopes,
  each of them sensitive in a narrow band (λ/Δλ = 15 to 80), centered
  at wavelengths between 50 and 175Å. Each telescope has an effective
  area of a few cm<SUP>2</SUP>; a field of view of 1.2° and a spatial
  resolution of 10 arcsec.EUVITA will be flown on the Russian mission
  SPECTRUM X-G. This satellite will be launched in a highly eccentric
  orbit with a period of 4 days, allowing long, uninterrupted observations
  (e.g. 10<SUP>5</SUP> seconds). EUVITA's narrow spectral bands allow
  the measurement of source parameters such as temperature or power law
  index as well as interstellar absorption, and will resolve groups of
  strong lines emitted by optically thin hot plasmas.

---------------------------------------------------------
Title: Performance of back-illuminated Tektronix CCDs in the extreme
    ultraviolet
Authors: Moses, John D.; Howard, Russell A.; Wang, Dennis; Catura,
   Richard C.; Lemen, J. R.; Shing, Lawrence; Stern, Robert A.; Hochedez,
   Jean-Francois E.; Delaboudiniere, Jean-Pierre
1993SPIE.2006..252M    Altcode:
  The quantum efficiency (QE) and flat field characteristics of
  back-illuminated 1024 X 1024 Tektronix CCDs have been measured in the
  extreme ultraviolet (EUV) between 44 and 1216 angstroms. These CCDs have
  been fabricated for the focal plane detector of the Extreme-ultraviolet
  Imaging Telescope (EIT) on the Solar and Heliospheric Observing
  spacecraft. The back-side surface of the EIT CCDs have been specially
  processed to enhance and stabilize the EUV QE. All requirements for
  QE are met by these devices, although a poorly understood variation
  of QE with temperature will complicate data analysis.

---------------------------------------------------------
Title: EUVITA - an extreme UV imaging telescope array with spectral
    capability
Authors: Courvoisier, J. -L.; Orr, A.; Bühler, P.; Zehnder, A.;
   Henneck, R.; Stauffacher, F.; Biakhowski, J.; Schlumpf, N.; Schoeps,
   W.; McHedlishvili, A.; Sunyaev, R.; Aref'ev, V.; Yascovich, A.;
   Babalyan, G.; Pavlinsky, M.; Delaboudinière, J. P.; Carone, T.;
   Siegmund, 0.; Warren, J.; Leahy, D.; Salaschenko, N.; Platonov, J.
1993ExA.....4..117C    Altcode:
  EUVITA is a set of 8 extreme UV and soft X-ray normal incidence imaging
  telescopes, each of them sensitive in a narrow band (λ/Δλ=15 to
  80), centered at wavelengths between 50 and 175 Å. Each telescope
  has an effective area of a few cm<SUP>2</SUP>, a field of view of
  1.2° and an angular resolution of 10 arcseconds. EUVITA will be Sown
  on the Russian mission SPECTRUM X-G. This satellite will be launched
  in a highly eccentric orbit with a period of 4 days, allowing long,
  uninterrupted observations (e.g. 10<SUP>5</SUP> seconds). The present
  paper includes an overview of EUVITA's scientific capabilities and a
  short description of the instrument. Simulations of various types of
  sources show EUVITA's capability to detect galactic and extragalactic
  EUV sources. EUVITA's narrow spectral bands allow the measurement
  of source parameters such as temperature or power law index as well
  as interstellar absorption, and will resolve groups of strong lines
  emitted by optically thin hot plasmas.

---------------------------------------------------------
Title: Tuning multilayered mirror light traps for rejection of
    30.4-nm radiation
Authors: Delaboudiniere, Jean-Pierre; Hochedez, Jean-Francois;
   Chauvineau, Jean-Pierre; Valiergue, Laurence
1993SPIE.1742..296D    Altcode:
  Very efficient mirrors designed for rejection of the 30.4 nm HeII line
  while transmitting the 28.4 nm FeXV line are needed for observations
  of the solar corona. Light traps, based on multilayered structures,
  using moderately absorbing diffractor layers of SiO2 and aluminum
  as spacer material, have been successfully fabricated providing
  dramatically high rejection ratios. However, accurate tuning at the
  desired wavelength has proven to be extremely difficult to achieve in
  combination with high nominal reflectivity. Very slight deviations
  of thicknesses or optical constants can easily destroy the desired
  antiresonance effect. Classical Mo/Si structures, although somewhat
  less selective, can also be specially designed for this application
  and they prove more amenable to proper adjustment.

---------------------------------------------------------
Title: Solar corona synoptic observations from SOHO with an Extreme
    Ultraviolet Imaging Telescope.
Authors: Delaboudinière, J. P.; Gabriel, A. H.; Artzner, G. E.;
   Dere, K.; Howard, R.; Michels, D.; Catura, R.; Lemen, J.; Stern, R.;
   Gurman, J.; Neupert, W.; Cugnon, P.; Koeckelenbergh, A.; van Dessel,
   E. L.; Jamar, C.; Maucherat, A.
1992ESASP.348...21D    Altcode: 1992cscl.work...21D
  The major scientific objective of the EUV Imaging Telescope (EIT)
  is to study the evolution of coronal structure over a wide range
  of spatial and temporal scales and temperatures. A second strategic
  objective is to provide full disk synoptic maps of the global corona
  to aid in unifying SOHO (Solar and Heliospheric Observatory)/Cluster
  investigations. EIT will also provide images to support the planning
  of detailed spectroscopic investigations by the CDS (Coronal Diagnostic
  Spectrometer) and SUMER spectrometers in SOHO. EIT observations will be
  made in four narrow spectral bands, centered at 171 A (Fe 9), 195 A(Fe
  12), 284 A (Fe 15), and 304 A (He 2) representing restricted temperature
  domains within a wide temperature range from 40,000 to 3,000,000
  K. The results will be images of the solar atmosphere from the upper
  chromosphere and transition region to the active region corona. These
  maps, made at appropriate time intervals, will be used to study the fine
  structures in the solar corona and to relate their dynamic properties
  to the underlying chromosphere and photosphere. Dynamic events in the
  inner corona will be related to white light transients in the outer
  corona, and observations of the internal structure of coronal holes
  will be used to investigate origins of the solar wind.

---------------------------------------------------------
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.
1991BCrAO..83...18F    Altcode:
  No abstract at ADS

---------------------------------------------------------
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.
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: Use of thinned backside illuminated CCD from the extreme
    ultraviolet to the soft ultraviolet
Authors: Hochedez, Jean-Francois E.; Lemaire, Philippe; Delaboudiniere,
   Jean-Pierre; Cougrand, Bernard; Barba, Julien
1989SPIE.1070...53H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Extreme ultraviolet imaging telescope on board the Solar
    Heliospheric Observatory
Authors: Delaboudiniere, Jean-Pierre; Gabriel, Alan H.; Artzner,
   Guy E.; Millier, F.; Michels, Donald J.; Dere, Kenneth P.; Howard,
   Russell A.; Kreplin, Robert W.; Catura, Richard C.; Stern, Robert A.;
   Lemen, James R.; Neupert, Werner M.; Gurman, Joseph B.; Cugnon, P.;
   Koeckelenbergh, A.; van Dessel, E. L.; Jamar, Claude A.; Maucherat,
   Andre J.; Chauvineau, Jean-Pierre; Marioge, Jean-Paul
1989SPIE.1160..518D    Altcode: 1989xeoa.conf..518D
  The design of the multibandpass Extreme-Ultraviolet Imaging Telescope
  designed for 1996 launch on board the Solar Heliospheric Observatory
  is described. The telescope will observe simultaneously distinct
  temperature ranges in the solar corona, defined by well chosen emission
  lines. Images in four narrow bandpasses at wavelengths ranging from 17
  to 31 nm will be obtained using normal-incidence multilayered optics
  deposited on quadrants of a Ritchey-Chretien telescope. Results are
  presented on the performances measured on a 2/3 scale mock-up. The
  bandpasses could be adjusted to better than 1 percent in wavelength.

---------------------------------------------------------
Title: Metal oxide multilayers with narrow band-passes.
Authors: Delaboudiniere, J. P.; Vien, T. K.; Chauvineau, J. P.
1989SPIE.1160..260D    Altcode: 1989xeoa.conf..260D
  Metal oxide multilayers provide reflecting coatings in the 15 - 50
  nm range with exceptionnal properties. The authors discuss filters
  featuring narrow band-passes and/or very sharp cut-offs. Possible
  effects of degraded manufacturing processes are also evaluated.

---------------------------------------------------------
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.
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: EIT: Solar corona synoptic observations from SOHO with an
    Extreme-ultraviolet Imaging Telescope
Authors: Delaboudiniere, J. P.; Gabriel, A. H.; Artzner, G. E.;
   Michels, D. J.; Dere, K. P.; Howard, R. A.; Catura, R.; Stern, R.;
   Lemen, J.; Neupert, W.
1988sohi.rept...43D    Altcode:
  The Extreme-ultraviolet Imaging Telescope (EIT) of SOHO (solar and
  heliospheric observatory) will provide full disk images in emission
  lines formed at temperatures that map solar structures ranging from
  the chromospheric network to the hot magnetically confined plasma in
  the corona. Images in four narrow bandpasses will be obtained using
  normal incidence multilayered optics deposited on quadrants of a
  Ritchey-Chretien telescope. The EIT is capable of providing a uniform
  one arc second resolution over its entire 50 by 50 arc min field of
  view. Data from the EIT will be extremely valuable for identifying
  and interpreting the spatial and temperature fine structures of the
  solar atmosphere. Temporal analysis will provide information on the
  stability of these structures and identify dynamical processes. EIT
  images, issued daily, will provide the global corona context for aid
  in unifying the investigations and in forming the observing plans for
  SOHO coronal instruments.

---------------------------------------------------------
Title: Progress with LSM optics for solar observations within the
    French space program.
Authors: Delaboudiniere, J. P.
1987RALR...43..133D    Altcode:
  Development of Layered Synthetic Microstructures for XUV optics has
  begun a few years ago in several French laboratories. The author's
  laboratory has been concerned with potential applications of this new
  technique to observations of the solar corona in the EUV wavelength
  range with normal incidence optical systems. This activity was recently
  bolstered by perspectives opened by the projected ESA solar mission
  SOHO.

---------------------------------------------------------
Title: Space qualification of multilayered optics.
Authors: Delaboudiniere, J. -P.; Chauvineau, J. -P.; Marioge, J. -P.
1985SPIE..563...44D    Altcode:
  The feasibility for the ESA SOHO mission, of spectrally selected normal
  incidence telescopes in the XUV wavelength range is demonstrated in
  an evaluation of multilayered mirrors illuminated by the sun. Worst
  case solar vacuum tests of unprotected telescopes illuminated by
  a xenon arc lamp simulator indicate less than 10 percent decrease
  in reflectivity of the exposed section of the Hf/Si sample for the
  secondary mirrors. Primary mirror tests are currently being performed
  aboard the NASA Long Duration Exposure Facility. Results of protecting
  filter tests suggest a growth from 40-100 A in the thickness of the
  two aluminum oxide layers protecting the aluminum, in contradiction
  to previous findings (Hunter et al., 1973).

---------------------------------------------------------
Title: Aspherization and multilayer coating of a Ritchey-Chrétien
    telescope for λ = 30.4 nm.
Authors: Chauvineau, J. P.; Decanini, D.; Mullot, M.; Valiergue, L.;
   Delaboudiniere, J. P.
1985SPIE..563..275C    Altcode:
  A high vaccum system designed for the deposition of multilayers for
  soft X-ray mirrors is described. It is applied to the aspherization
  and multilayer coating of the mirrors of a solar Ritchey-Chretien
  telescope. In a first step, laterally graded boron layers are
  deposited on flat polished silica substrate in order to determine
  their thickness profile by visible light interferometry. The next step
  consists in the characterization of multilayers deposited on top of the
  boron layer. Grazing incidence X-ray interferometry is applied to the
  measurement of interface roughness; the results are used to predict the
  performances of W/Si multilayers; it is found that reflectivity values
  of about 25 percent could be obtained for normal reflection at 30.4 nm.

---------------------------------------------------------
Title: Compact resonance absorption spectrometer to monitor the
    profile of the solar He 58.4 nanometer line
Authors: Crifo, J. F.; Seidl, P.; Delaboudinière, J. P.; Schmidtke, G.
1980RScI...51..321C    Altcode:
  A miniature resonance absorption spectrometer is able to perform a
  routine monitoring in space of the line profile and intensity of the
  He i resonance line from the solar disk with a time resolution of about
  1 min and a spectral resolution of 105. It consists of a predispersive
  spectrometer incorporating a helium gas absorption cell. The instrument
  has been designed to meet a small size and weight. It was tested on a
  rocket flight in June 1976. The construction, principles of operation,
  and laboratory calibration of the instrument are presented. Its
  capability to resolve details of the order of 0.3 pm FWHM and its
  sensitivity to the intensity of line wings three order of magnitudes
  fainter than the peak of the line have been established by laboratory
  investigation.

---------------------------------------------------------
Title: Multiple scattering effects in a cylindrical helium absorption
    cell operating close to the resonance line at lambda 584 Å.
Authors: Delaboudiniere, J. P.
1979JQSRT..22..411D    Altcode:
  The departure from Beer's law due to multiple scattering in a helium
  absorption cell is investigated. A complete description of the relevant
  scattering mechanisms, within the frame of a Monte Carlo simulation,
  is used to evaluate the effects of polarization, collisional line
  broadening and frequency redistribution. A cylindrical geometry is
  studied which includes optical reflection effects at the boundaries
  of the enclosure.

---------------------------------------------------------
Title: Intercomparison/compilation of relevant solar flux data
    related to aeronomy/Solar Cycle 20/
Authors: Delaboudiniere, J. P.; Donnelly, R. F.; Hinteregger, H. E.;
   Schmidtke, G.; Simon, P. C.
1978cosp.conf.....D    Altcode:
  The intercomparison of solar irradiance (in the UV/XUV spectra)
  is presented graphically for Solar Cycle 20. The smoothed sunspot
  number is chosen over the more fluctuating F sub 10.7 radio flux to
  demonstrate solar activity. Attention is given to variations in solar
  irradiance in terms of duration, i.e., short-, medium-, and long-term.

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Title: Possible contribution of radiation from the 2s2p
    <SUP>4</SUP><SUP>2</SUP>P level of O II in dayglow measurements of
    the He I line at 584 Å
Authors: Delaboudiniere, J. P.
1977P&SS...25..193D    Altcode:
  Intensity of dayglow emmisions in the lines of 0 II at 537 and 581
  Å is evaluated from presently accepted atomic parameters, EUV solar
  fluxes and atmospheric models. An improvement of the experimental
  techniques used up to now is suggested to identify these emissions
  and provide new data on ionospheric processes.

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Title: Preliminary results obtained from the solar EUV experiment
    on board the D2B Aura satellite.
Authors: Delaboudiniere, J. P.; Millier, F.
1977spre.conf..519D    Altcode: 1977spre.proc..519D
  The solar EUV experiment on board D2B has been operating successfully
  since November 1, 1975. Three main sets of data are being gathered:
  (1) spectroheliograms at a resolution of one arcmin within prominent
  solar lines formed at temperatures between 20,000 and 3 million K,
  providing detailed observations of individual active regions; (2)
  disk-integrated values of the solar flux in the range 17-127 nm at a
  resolution of 0.8 to 0.6 nm suitable for defining the spectral energy
  input to the upper atmosphere; and (3) simultaneous measurements of
  solar extinction at sunset and sunrise at eight different wavelengths,
  providing a partially redundant set of information for remote sounding
  of atmospheric composition and temperature between 100 and 400 km.

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Title: The profile of the helium I 584 Å solar line. Preliminary
    results from rocket-borne resonance absorption spectrometer.
Authors: Delaboudiniere, J. P.; Crifo, J. F.
1976spre.conf..803D    Altcode: 1976spre.proc..803D
  A measurement of the line profile of the He I 584 A line from the
  sun has been made on board a rocket on 20 January 1975. Wavelength
  resolution is obtained by the resonance absorption method. The
  instrument is described, and its performance in flight is analysed. The
  principles of data reduction are given, and preliminary results are
  presented and compared with available data from other sources. The width
  of the solar He I resonance line is found to be larger than 110 mA.

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Title: A rocket borne absorption cell for high resolution spectroscopy
    of the He I line at 584 Å.
Authors: Delaboudiniere, J. P.; Carabetian, C.
1975SSI.....1...91D    Altcode:
  A rocket instrument designed to measure the profile of the 584 A line
  of helium emitted by the sun, has been constructed. The most original
  part of this instrument is a resonant absorption cell for use in the
  extreme ultraviolet. Filled with rare gases such a device allows the
  spectral analysis of a wide range of line shapes because a very high
  optical thickness can be reached. The flexibility of the absorption
  cell method has been demonstrated both by numerical analysis and by
  laboratory experiment. Although the planned experiment has not been
  successful yet, it has been proven that absorption cells, can be used
  for space applications and several have been tested successfully in
  flight on board rockets.