Author name code: artzner
ADS astronomy entries on 2022-09-14
author:"Artzner, Guy" 
------------------------------------------------------------------------  

Title: Coronographie interferéntielle pour la mission spatuale
DARWIN: expérience de validation en laboratoire
Authors: Ollivier, Marc; Mariotti, Jean-Marie; Brunaud, Jacqueline;
   Michel, Guy; Bouchareine, Patrick; Léger, Alain; Artzner, Guy; Malbet,
   Fabien; Puget, Pascal; Coudé du Foresto, Vincent; Mennesson, Bertrand
Bibcode: 2018SPIE10570E..0PO
Altcode:
  This paper, "Coronographie interferéntielle pour la mission spatuale
  DARWIN: expérience de validation en laboratoire," was presented as
  part of International Conference on Space Optics—ICSO 1997, held in
  Toulouse, France.

Title: Time Evolution of the Altitude of an Observed Coronal Wave
Authors: Delannée, C.; Artzner, G.; Schmieder, B.; Parenti, S.
Bibcode: 2014SoPh..289.2565D
Altcode: 2014SoPh..tmp...49D; 2013arXiv1310.5623D
  The nature of coronal wave fronts is intensely debated. They are
  observed in several wavelength bands and are frequently interpreted as
  magnetosonic waves propagating in the lower solar atmosphere. However,
  they can also be attributed to the line-of-sight projection of the
  edges of coronal mass ejections. Therefore, estimating the altitude of
  these features is crucial for deciding in favor of one of these two
  interpretations. We took advantage of a set of observations obtained
  from two different view directions by the EUVI instrument onboard
  the STEREO mission on 7 December 2007 to derive the time evolution of
  the altitude of a coronal wave front. We developed a new technique to
  compute the altitude of the coronal wave and found that the altitude
  increased during the initial 5 min and then slightly decreased back to
  the low corona. We interpret the evolution of the altitude as follows:
  the increase in the altitude of the wave front is linked to the rise
  of a bubble-like structure depending on whether it is a magnetosonic
  wave front or a CME in the initial phase. During the second phase, the
  observed brightness of the wave front was mixed with the brightening
  of the underlying magnetic structures as the emission from the wave
  front faded because the plasma became diluted with altitude.

Title: A Multi-spacecraft View of a Giant Filament Eruption during
    2009 September 26/27
Authors: Gosain, Sanjay; Schmieder, Brigitte; Artzner, Guy; Bogachev,
   Sergei; Török, Tibor
Bibcode: 2012ApJ...761...25G
Altcode: 2012arXiv1210.6686G
  We analyze multi-spacecraft observations of a giant filament eruption
  that occurred during 2009 September 26 and 27. The filament eruption was
  associated with a relatively slow coronal mass ejection. The filament
  consisted of a large and a small part, and both parts erupted nearly
  simultaneously. Here we focus on the eruption associated with the
  larger part of the filament. The STEREO satellites were separated
  by about 117° during this event, so we additionally used SoHO/EIT
  and CORONAS/TESIS observations as a third eye (Earth view) to aid our
  measurements. We measure the plane-of-sky trajectory of the filament as
  seen from STEREO-A and TESIS viewpoints. Using a simple trigonometric
  relation, we then use these measurements to estimate the true direction
  of propagation of the filament which allows us to derive the true
  R/R <SUB>⊙</SUB>-time profile of the filament apex. Furthermore, we
  develop a new tomographic method that can potentially provide a more
  robust three-dimensional (3D) reconstruction by exploiting multiple
  simultaneous views. We apply this method also to investigate the 3D
  evolution of the top part of filament. We expect this method to be
  useful when SDO and STEREO observations are combined. We then analyze
  the kinematics of the eruptive filament during its rapid acceleration
  phase by fitting different functional forms to the height-time
  data derived from the two methods. We find that for both methods an
  exponential function fits the rise profile of the filament slightly
  better than parabolic or cubic functions. Finally, we confront these
  results with the predictions of theoretical eruption models.

Title: A Technique for Removing Background Features in SECCHI -
EUVI He II 304 Å Filtergrams: Application to the Filament Eruption
    of 22 May 2008
Authors: Artzner, G.; Gosain, S.; Schmieder, B.
Bibcode: 2010SoPh..262..437A
Altcode: 2010SoPh..tmp...41A; 2010SoPh..tmp...53A; 2010arXiv1001.4884A
  The STEREO mission has been providing a stereoscopic view of filament
  eruptions in the EUV. The clearest view during a filament eruption
  is seen in He II 304 Å observations. One of the main problems in
  visualizing filament dynamics in He II 304 Å is the strong background
  contrast due to surface features. We present a technique that removes
  background features and leaves behind only the filamentary structure, as
  seen by STEREO-A and -B. The technique uses a pair of STEREO He II 304
  Å images observed simultaneously. The STEREO-B image is geometrically
  transformed to a STEREO-A view so that the background images appear
  similar. Filaments, being elevated structures, i.e., not lying on the
  same spherical surface as background features, do not appear similar
  in the transformed view. Thus, subtracting the two images cancels
  the background but leaves behind the filament structure. We apply this
  technique to study the dynamics of the filament-eruption event of 22 May
  2008, which was observed by STEREO and followed by several ground-based
  observatories participating in the Joint Observing Programme (JOP 178).

Title: A 3D view of eruptive filaments by STEREO
Authors: Gosain, Sanjay; Schmieder, Brigitte; Venkatakrishnan, P.;
   Chandra, Ramesh; Artzner, Guy
Bibcode: 2010cosp...38.2916G
Altcode: 2010cosp.meet.2916G
  STEREO/SECHI/EUVI A and B observe different views of the eruption of a
  quiescent filament. We will concentrate on two events: (i) May 20 to 22,
  2008 event (A and B separated by 52.4 degrees from each other), and (ii)
  September 25 to 26, 2009 event (A and B more than 100 degrees from each
  other. After using different techniques of reconstruction we obtained
  a 3 dimensional view of untwisted flux ropes in He II 304 Angstrom,
  with fine structures. The entire disappearance phase lasted more than
  ten hours. The filament evolved very slowly ( 5 km/s) from a dense
  structure with a thick spine into fine threads. Individual threads are
  seen to be oscillating and rising to an altitude of about 150 Mm with
  velocities of about 100 km/s. The plasma disappears by diffusion in
  the corona. Weak CME events are recorded by LASCO at the beginning of
  the disappearance. In this paper we shall present the dynamics of the
  filament eruptions as viewed in 3D by STEREO using different methods. We
  shall explore the causes and consequences of the filament disappearance.

Title: 3D Evolution of a Filament Disappearance Event Observed
    by STEREO
Authors: Gosain, S.; Schmieder, B.; Venkatakrishnan, P.; Chandra,
   R.; Artzner, G.
Bibcode: 2009SoPh..259...13G
Altcode: 2009arXiv0910.0786G
  A filament disappearance event was observed on 22 May 2008 during
  our recent campaign JOP 178. The filament, situated in the Southern
  Hemisphere, showed sinistral chirality consistent with the hemispheric
  rule. The event was well observed by several observatories,
  in particular by THEMIS. One day, before the disappearance, Hα
  observations showed up- and down-flows in adjacent locations along the
  filament, which suggest plasma motions along twisted flux rope. THEMIS
  and GONG observations show shearing photospheric motions leading
  to magnetic flux canceling around barbs. STEREO A, B spacecraft
  with separation angle 52.4°, showed quite different views of this
  untwisting flux rope in He II 304 Å images. Here, we reconstruct the
  three-dimensional geometry of the filament during its eruption phase
  using STEREO EUV He II 304 Å images and find that the filament was
  highly inclined to the solar normal. The He II 304 Å movies show
  individual threads, which oscillate and rise to an altitude of about
  120 Mm with apparent velocities of about 100 km s<SUP>−1</SUP>
  during the rapid evolution phase. Finally, as the flux rope expands
  into the corona, the filament disappears by becoming optically thin to
  undetectable levels. No CME was detected by STEREO, only a faint CME
  was recorded by LASCO at the beginning of the disappearance phase at
  02:00 UT, which could be due to partial filament eruption. Further,
  STEREO Fe XII 195 Å images showed bright loops beneath the filament
  prior to the disappearance phase, suggesting magnetic reconnection
  below the flux rope.

Title: Optique active et optique adaptative.
Authors: Artzner, G.
Bibcode: 2006LAstr.120..349A
Altcode:
  No abstract at ADS

Title: An atlas of solar events: 1996 2005
Authors: Artzner, G.; Auchère, F.; Delaboudinière, J. P.; Bougnet, M.
Bibcode: 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.

Title: EIT Observations of the 15 November 1999 Mercury Transit
Authors: Auchère, F.; Artzner, G. E.
Bibcode: 2004SoPh..219..217A
Altcode:
  The Mercury transit of 15 November 1999 has been observed from space
  by the SOHO and TRACE spacecraft. We exploited the data recorded by
  EIT/SOHO to determine the stray-light level and the plate-scale of
  the instrument. The asymmetric distribution of stray light across the
  images is confirmed, but the absolute amount was found to be higher
  than previously estimated. The plate scale averaged over wavelengths
  was found to be 2.627±0.001 arc sec pixel<SUP>−1</SUP>, in excellent
  agreement with two previous and independent determinations.

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
Bibcode: 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: An atlas of solar events: 1997-2004
Authors: Artzner, G.; Auchère, F.; Delaboudinière, J. P.; Bougnet, M.
Bibcode: 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: Photon sieves as EUV telescopes for Solar Orbiter
Authors: Artzner, Guy E.; Delaboudiniere, Jean Pierre; Song, Xueyan
Bibcode: 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: 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.
Bibcode: 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: Transition region quiet sun velocity field evolution
Authors: Lemaire, P.; Artzner, G.; Vial, J. -C.; Curdt, W.; Schühle,
   U.; Wilhelm, K.
Bibcode: 2002AdSpR..30..487L
Altcode:
  The UV/EUV SUMER spectrometer aboard SOHO can record profiles of lines
  emitted by elements at different stages of ionization corresponding
  to several temperatures within the transition region temperature
  range. During the solar cycle minimum in July 1996, we were able to
  observe the quiet Sun during five consecutive days. From the line
  positions we have determined the velocity fields and follow their time
  variations at different temperatures in the transition region. The line
  intensity maps are used to separate supergranular cells and network and
  they allow to compare the behaviors of the velocity fields evolution in
  the two structures. The results are critically analyzed and discussed.

Title: Nulling interferometry for the DARWIN mission: experimental
    demonstration of the concept in the thermal infrared with high levels
    of rejection
Authors: Ollivier, Marc; Mariotti, Jean-Marie; Sekulic, Predrag;
   Michel, Guy; Leger, Alain M.; Bouchareine, Patrick; Brunaud,
   Jacqueline; Coudé du Foresto, Vincent; Mennesson, Bertrand P.; Borde,
   Pascal J.; Amy-Klein, A.; Vanlerberghe, A.; Lagage, Pierre-Olivier;
   Artzner, Guy E.; Malbet, Fabien
Bibcode: 2000SPIE.4006..354O
Altcode:
  Present projects of space interferometers dedicated to the detection
  and analysis of extrasolar planets (DARWIN in Europe, TPF in the United
  States) are based on the nulling interferometry concept. This concept
  has been proposed by Bracewell in 1978 but has never been demonstrated
  with high values of rejection, in the thermal infrared range, where
  the planet detection should be performed (6 - 18 micrometers ). We
  have thus built a two-beam laboratory interferometer to validate this
  concept in a monochromatic case (at 10 micrometers ). The keypoint
  of our interferometer is the use of optical filtering by pinhole and
  optical fibers to clean the interfering beams. We present in this
  paper the principle of the experimental setup, its realization, and
  the first measurements of rejection it allowed. We also present the
  future developments of this interferometer.

Title: In-Flight Determination of the Plate Scale of the
    Extreme-Ultraviolet Imaging Telescope
Authors: Auchère, F.; DeForest, C. E.; Artzner, G.
Bibcode: 2000ApJ...529L.115A
Altcode:
  Using simultaneous observations of the Michelson Doppler Imager
  and Extreme-Ultraviolet Imaging Telescope (EIT) on board the Solar
  and Heliospheric Observatory spacecraft, we determined in flight
  the plate scale of the EIT. We found a value of 2.629"+/-0.001"
  pixel<SUP>-1</SUP>, in fair agreement with the 2.627"+/-0.001"
  pixel<SUP>-1</SUP> value deduced from recent laboratory measurements
  of the focal length and much higher by 7 σ than the 2.622"
  pixel<SUP>-1</SUP> value of the preflight calibrations. The plate
  scale is found to be constant across the field of view, confirming
  the negligible distortion level predicted by the theoretical models
  of the EIT. Furthermore, the 2 σ difference between our results and
  the latest laboratory measurements, although statistically small, may
  confirm a recent work suggesting that the solar photospheric radius
  may be 0.5 Mm lower than the classically adopted value of 695.99 Mm.

Title: In Flight Determination of the Plate Scale of the EIT
Authors: Auchere, F.; DeForest, C. E.; Artzner, G.
Bibcode: 1999astro.ph.12213A
Altcode:
  Using simultaneous observations of the MDI and EIT instruments on
  board the SoHO spacecraft, we determined in flight the plate scale
  of the EIT. We found a value of 2.629+-0.001 arc seconds per pixel,
  in fair agreement with the 2.627+-0.001 arc seconds per pixel value
  deduced from recent laboratory measurements of the focal length, and
  much higher by 7 sigma than the 2.622 arc seconds per pixel value of
  the pre-flight calibrations. The plate scale is found to be constant
  across the field of view, confirming the negligible distortion level
  predicted by the theoretical models of the EIT. Furthermore, the 2 sigma
  difference between our results and the latest laboratory measurements,
  although statistically small, may confirm a recent work suggesting that
  the solar photospheric radius may be 0.5 Mm lower than the classically
  adopted value of 695.99 Mm.

Title: Spécial éclipse 11 aou^t 1999 - bilan.
Authors: Laurent, M.; Weulersse, P.; Delahaye, F.; Gredin, E.; Gredin,
   P.; Roy, M.; Roy, H.; Arioli, H.; Boust, D.; Meeus, J.; Guillermier,
   P.; Artzner, G.
Bibcode: 1999LAstr.113..340L
Altcode:
  No abstract at ADS

Title: An Eruptive Flare Observed by TRACE as a Test for the Magnetic
Authors: Aulaneir, G.; Deluca, E. E.; Golub, L.; Artzner, Guy; Sabine
   Coquillart; Hochedez, Jean-Francois; Delaboudinier, Jean-Pierre
Bibcode: 1999ESASP.446..131A
Altcode: 1999soho....8..131A
  No abstract at ADS

Title: Equivalent focal length measurements
Authors: Artzner, Guy E.; Auchere, Frederic; Delaboudiniere,
   Jean-Pierre; Hochedez, Jean-Francois E.
Bibcode: 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: Nulling Interferometry for the DARWIN Mission - Laboratory
    Demonstration Experiment
Authors: Ollivier, M.; Léger, A.; Sekulic, C. Anceau. P.; Brunaud,
   J.; Artzner, G.; Mariotti, J. -M.; Michel, G.; Coudé du Foresto,
   V.; Mennesson, B.; Bouchareine, P.; Lépine, T.; Malbet, F.
Bibcode: 1999ASPC..194..443O
Altcode: 1999wfoi.conf..443O
  The present projects of space interferometers dedicated to the detection
  and analysis of extrasolar planets (DARWIN/IRSI in Europe, TPF in
  the United States) are based on the nulling interferometry concept
  (interferometrical coronography). This concept has been proposed by
  Bracewell in 1979 but has never been demonstrated, with high values
  of rejection, in the thermal infrared range where planet detection
  should be performed (6-18 microns). We have thus built a two-beam
  laboratory interferometer to validate this concept in a monochromatic
  case (CO2 laser). We present the principle of the experimental setup,
  its realisation, its sub-systems and their servo-control. We present
  also the first results we got with this interferometer.

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

Title: 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.
Bibcode: 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: Aspherical wavefront measurements: Shack-Hartmann numerical
    and practical experiments
Authors: Artzner, Guy
Bibcode: 1998PApOp...7..435A
Altcode:
  No abstract at ADS

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

Title: 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.
Bibcode: 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.
Bibcode: 1997ApJ...484L..75W
Altcode:
  SOHO EIT spectroheliograms showing the polar coronal holes during the
  present sunspot minimum are compared with National Solar Observatory
  (Kitt Peak) magnetograms taken in Fe I λ8688 and Ca II λ8542. The
  chromospheric λ8542 magnetograms, obtained on a routine, near-daily
  basis since 1996 June, reveal the Sun's strong polar fields with
  remarkable clarity. We find that the Fe IX λ171 polar plumes occur
  where minority-polarity flux is in contact with flux of the dominant
  polarity inside each polar hole. Moreover, the locations of ``plume
  haze'' coincide approximately with the patterns of brightened He
  II λ304 network within the coronal hole. The observations appear
  to be consistent with mechanisms of plume formation involving
  magnetic reconnection between unipolar flux concentrations and nearby
  bipoles. The fact that minority-polarity fields constitute only a small
  fraction of the total magnetic flux within the polar holes suggests
  that plumes are not the main source of the high-speed polar wind.

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

Title: 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.
Bibcode: 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 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.
Bibcode: 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: 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.
Bibcode: 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.
Bibcode: 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.
Bibcode: 1996BAAS...28Q.821H
Altcode:
  No abstract at ADS

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.
Bibcode: 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.
Bibcode: 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: Fabrication and optical characteristics of microlens arrays
    engraved in photoresist coatings
Authors: Gex, Francoise; Roblin, Gerard; Artzner, Guy E.; Bernstein,
   L.; Horville, David; Serpette, V.
Bibcode: 1993SPIE.1781..287G
Altcode:
  We have developed a technique for fabricating microlens arrays by
  engraving photoresist coatings. These microlens arrays are designed for
  astronomical applications for atmospheric wavefront sensors. First,
  we describe the apparatus and the manufacturing process. Second, we
  review the characteristics of the different photoresist types used
  in this process. Third, we report on the different optical testing
  methods to measure the microlens' performances. Then we deduce the
  several inherent advantages and limitations of this method. Fourth,
  we show how to produce monolithic arrays using ion beam milling with
  photoresist microlens arrays as a pattern and we demonstrate how these
  arrays can improve upon the performances of photoresist arrays.

Title: Towards a dark matter experiment: performance of a 24g
    sapphire bolometer
Authors: de Marcillac, P.; Coron, N.; Artzner, G.; Leblanc, J.; Torre,
   J. P.; Goldbach, C.; Nollez, G.; Vidal-Madjar, A.; Mangin, J.
Bibcode: 1992daec.conf..403D
Altcode: 1992daec.conf..403M
  I review here the debate on the nature of compact groups of galaxies:
  are the compact groups catalogued by Hickson physically dense systems
  or are they caused by chance alignments within larger systems? Results
  of recent N-body simulations of loose groups are analyzed, showing
  that only 10% of compact configurations seen in projection are three
  dimensional dense systems (of which roughly half are bound), whereas
  the remaining 90% are one dimensional chance alignments. Moreover,
  these chance alignments turn out to be binary-rich (with a small
  fraction of triplets too). The arguments reviewed here and these last
  two results suggest that rather than being dense quartets and quintets,
  most compact groups are binary-rich chance alignments within larger
  systems, thus providing a natural explanation to the high level of
  physical interactions seen in compact groups. Moreover, it is suggested
  that the most distant compact groups may represent the bright-ends of
  rich evolved clusters.

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.
Bibcode: 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: Microlens arrays for Shack-Hartmann wavefront sensors
Authors: Artzner, Guy
Bibcode: 1992OptEn..31.1311A
Altcode:
  Microlens arrays are a component of atmospheric wavefront sensors
  used recently with success by ground-based astronomers to obtain
  diffraction-limited images of stars in spite of wavefront disturbances
  introduced by the earth's atmosphere. Typical requirements for
  individual lenses are a size measured in tenths of millimeters, a sag
  measured in micrometers, and no room left between lenses, i.e., square
  or hexagonal lenses rather than circular lenses. Actual monolithic
  square microlens arrays up to 20 x 20 mm in size for 0.18- to 1.5-mm
  individual contiguous lenses of 0.0035-mm maximum sag are engraved in
  photoresist coatings by a two-axes rastering process. These arrays have
  been used for diurnal and nocturnal atmospheric wavefront measurements.

Title: Rotational aperture synthesis: a proposal for ground-based
    observations.
Authors: Artzner, Guy
Bibcode: 1992ESASP.344..273A
Altcode: 1992spai.rept..273A
  Attention is drawn to the existence of three-axes equatorial mounts
  for ground-based observing. The additional third axis with respect
  to a conventional two axes equatorial or alt-az mount allows to set
  the position angle at almost any predetermined value when observing
  close to the zenith. In addition to that the quasi-total absence of
  cantilever parts is an asset for interferometric stability. If the
  SIMURIS strategy uses some breadboard for fine structure imaging
  on the ground in the visible domain as an intermediate step between
  laboratory developments and flight operations the author investigates
  tactics for solar or stellar interferometric observations.

Title: Solar Astrometry by Photolithography
Authors: Artzner, G.
Bibcode: 1990SoPh..128..281A
Altcode: 1990IAUCo.121P.281A
  Observed temporal variations of shape and size of the solar disk as
  viewed from Earth may act as constraints for theories of the interior of
  the Sun. In addition to existing programs of solar diameter measurements
  we investigate a ground-based photographic method.

Title: Massive composite bolometers for dark matter detection.
Authors: Coron, N.; de Marcillac, P.; Artzner, G.; Leblanc, J.;
   Jegoudez, G.; Dambier, G.; Lepeltier, J. P.; Barthelemy, M.;
   Rothenflug, R.; Pari, P.; Tarrius, A.; Amoudry, F.; Stroke, H.;
   Testard, O.
Bibcode: 1990qfcc.proc..275C
Altcode:
  Massive composite bolometers cooled below 0.1K can detect recoil
  energy of particles with a very high efficiency. By using different
  absorber materials (Al<SUB>2</SUB>O<SUB>3</SUB>, Ge, Si, LiF,
  Cr<SUB>2</SUB>O<SUB>3</SUB>, TiO<SUB>2</SUB>...) some identification
  of dark matter particles will be possible. Resolutions in the 10 eV
  range for 1 kg of absorber material are theoretically possible at 0.01K
  if the thermistor is well matched to the substrate. The authors have
  successfully developed and tested a 25 g sapphire bolometer at 0.1K
  and have obtained for a 60 keV gamm-line a resolution of 16 keV FWHM,
  limited by extraneous noise. First bolometric spectra of radioactivity
  and cosmic ray backgrounds obtained at sea level are presented.

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
Bibcode: 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: Static wavefront correction by Linnik interferometry.
Authors: Artzner, G.
Bibcode: 1989SPIE.1013..233A
Altcode:
  The author considers optical systems with residual peak to valley
  wavefront errors below 150 nm. The interference figure for λ =
  633 nm may then be adjusted and photographed as to hold out at every
  point of the image of the pupil a one to one relationship between the
  optical density of the interferogram and the magnitude of the wavefront
  error. An enduring interference figure is secured by means of a tiny
  reflecting aluminized spot on a bare substrate located on the image
  of a distant point source. The author investigates how subsequent
  photoreproduction of an interferogram upon a photoresist coating may
  act as a transmitting or reflecting wavefront corrector.

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.
Bibcode: 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: Astronomical optics: Zonal aberration correction - Laboratory
    experiments and extrapolations to space- and ground-based observations
Authors: Artzner, G.
Bibcode: 1987A&A...175..345A
Altcode:
  The author describes the results of a laboratory experiment with a
  143 mm diameter Cassegrainian telescope plagued by static irregular
  zonal aberrations with rotational symmetry and 620 nm peak to valley
  amplitude wavefront error. An adapted 16 mm useful diameter intrafocal
  corrector plate has been surfaced using a 2 μ-thickness photoresist
  coating on an optical substrate, ad-hoc non-uniform exposure via a
  two-axis computercontrolled scanning device and subsequent development
  and baking. The effect of losses by diffusion and absorption due to the
  corrector plate is small with respect to the increase of contrast due
  to the wavefront correction. Three extrapolations of this experiment
  are discussed: (1) How to use correctors in the UV range where the size
  of the Airy disk becomes smaller for a given aperture. (2) Correction
  of aberrations with no rotational symmetry. (3) Feasible correctors
  and relay optics adapted to large (4-8 m diameter) instruments have
  a 50 mm corrected field, well matched to modern image detectors.

Title: Aspherical surfaces engraved on photoresist coatings:
    manufacture of a zonal corrector plate for an aberrating Cassegrainian
    telescope.
Authors: Artzner, G.
Bibcode: 1987SPIE..805..162A
Altcode:
  We investigate how aspherical optical surfaces engraved in photoresist
  coatings avail against static wavefront aberrations up to 3 μ. The
  spherical aberration of a singlet lens is corrected for. The image
  given by a cassegrainian telescope of 143 mm diameter with a peak to
  valley 0,62 µ wavefront error and 7" slopes is improved by a 16 mm
  diameter intrafocal phase equalizer corrector plate. We then discuss
  extrapolations of our laboratory experiments.

Title: Bolometers as particle spectrometers
Authors: Stroke, H. H.; Artzner, G.; Coron, N.; Dambier, G.; Hansen,
   P. G.
Bibcode: 1986ITNS...33..759S
Altcode:
  A spectrometer based on low-temperature calorimetry has been under
  development since 1983. The present detector, capable of recording
  individual alpha and beta particles and X-ray photons, is based
  on a composite diamond-germanium bolometer. The advantage of a
  composite bolometer is that it separates the absorption and detection
  functions. Diamond, as an absorber, is of particular advantage
  because of its low heat capacity and high thermal diffusivity. The
  goal is a theoretical energy resolution of a few eV at 0.1 K. Initial
  experiments at 1.3 K and 0.9 K, which give resolutions in the keV range,
  are still noise-limited. High-resolution applications, such as in X-ray
  astronomy and nuclear physics (in particular, neutron mass measurements)
  are foreseen.

Title: Composite bolometers as spectrometers for X-ray astronomy
Authors: Coron, N.; Artzner, G.; Dambier, G.; Jegoudez, G.; Leblanc, J.
Bibcode: 1986SPIE..597..389C
Altcode:
  The detection of single events like the absorption of gamma or X-rays
  and alpha or beta particles with cooled thermal detectors is now
  well established and first resolutions obtained are promising. The
  paper investigates the possibilities of the composite bolometer which
  offers the advantage of separating the absorption, thermal diffusion
  and thermometric functions. An optimal configuration is the diamond
  composite bolometer with a monolithic thermistor. Experimental results
  are presented on the simultaneous detection of different kinds of events
  at 1 K temperature. These results confirm the high linearity of this
  detector and its ability to accept rather high counting rates. As a
  conclusion, an example of application to X-ray astronomy is presented
  and some problems or developments to be studied for a space mission
  are underlined.

Title: Bolometers as spectrometers for X-ray astronomy.
Authors: Coron, N.; Artzner, G.; Dambier, G.; Jegoudez, G.; Leblanc,
   J.; Deschamps, J. Y.; Rocchia, R.; Tarrius, A.; Testard, O.; Ravn,
   H. R.; Stroke, H. H.; Jonson, B.
Bibcode: 1985ESASP.239..229C
Altcode: 1985cxrs.work..229C
  The authors have investigated the possibility to use composite
  diamond-germanium bolometers, originally developed for I.R. astronomy,
  for the individual detection of X-ray photons.

Title: On the possible use of deep U.V. photoresists correctors to
    obtain the ultimate U.V. resolution of space borne telescopes.
Authors: Dame, L.; Bonnet, R. M.; Artzner, G. E.
Bibcode: 1984SPIE..445..318D
Altcode:
  Large space-borne telescopes are limited in their ultraviolet resolution
  by their large and medium scale (20 - 30 cm) surface irregularities
  (ripples). The authors present the principle, instrumentation and
  first results of a new interferometric method using a Michelson-Twyman
  configuration (diverging light beams) that allows to engrave on
  deep U.V. photoresists a phase compensating plate which permit to
  revocer, partly or entirely, the diffraction limited resolution of the
  telescope. The corrector that they obtain is a phase compensating plate
  in reflection with highs and lows on its surface perfectly conjugated
  in negative, with the primary mirror surface irregularities.

Title: Solar H-Lyman-α Flux and Profile Relative Measurements from
OSO-8: January 1976 to March 1978
Authors: Artzner, G.
Bibcode: 1983wcrs.proc...87A
Altcode:
  More than 1,900 monochromatic full solar disk raster images of the H
  Lyman-alpha 121.6-nm line have been calibrated by reference to nearly
  simultaneous profiles of the Lyman-alpha line emitted by small, quiet
  areas of the solar disk. The observations and the calibration procedures
  are described. Values of the full line flux vary in a relative range
  1 to 1.5 between January 1976 and March 1978. A hypothetical 35 to
  60 percent variation of the solar flux between July 1976 and October
  1977, as published with Atmosphere Explorer E results, is likely to
  be closer to 30 to 35 percent. Any variation of the shape of the full
  disk Lyman-alpha line profile is undetectable between December 9,
  1976 and May 10, 1978.

Title: Structure and Physics of Solar Faculae - Part Two - the
    Non-Thermal Velocity Field above Faculae
Authors: Mouradian, Z.; Dumont, S.; Pecker, J. -C.; Chipman, E.;
   Artzner, G. E.; Vial, J. C.
Bibcode: 1982SoPh...78...83M
Altcode:
  The OSO-8 satellite enabled us to study various characteristics of
  the profiles of Si II, Si IV, C IV, and O VI lines above active areas
  of the Sun, as well as above quiet areas, and to derive some physical
  properties of the transition region between chromosphere and corona
  (CCT): (i) The study of the lines shows a general tendency for the
  microvelocity fields on the average to be nearly constant for the
  heights corresponding to T &gt; 10<SUP>5</SUP> K; however they seem
  to slightly increase with height in quiet areas, and decrease in
  active areas. (ii) A multicomponent model of the CCT is however quite
  necessary, and its geometry is far from being a set of plane-parallel
  columns. It is similar to an association of moving knots within the
  non-moving principal component of the matter. (iii) The proportion
  of mass, in the knots relative to that in the non-moving component,
  is several times larger in active regions than in quiet regions. (iv)
  In the knots, the non-thermal microvelocity fields are smaller in active
  regions and seem to decrease for T increasing above 10<SUP>5</SUP> K,
  contrary to what happens in the steady principal component. Of course,
  we consider that microturbulence and Doppler shift are two aspects of
  the same distribution of velocity.

Title: Physical properties of the solar chromosphere deduced from
    optically thick lines. I - Observations, data reduction, and modelling
    of an average plage
Authors: Lemaire, P.; Gouttebroze, P.; Vial, J. C.; Artzner, G. E.
Bibcode: 1981A&A...103..160L
Altcode:
  Simultaneous Ca II H and K, Mg II h and k, and H I Lyman-alpha and
  Lyman-beta profiles have been recorded by the OSO-8/LPSP spectrometer on
  a quiet sun area and a part of plage, McMath 13738. After data reduction
  and filtering, a full set of calibrated profiles is obtained. Using
  a code developed at LPSP (Gouttebroze et al., 1978), profiles
  computed from VAL III model C (Vernazza et al., 1981) are compared
  to observations. A specific plage model has been computed to fit the
  observed profiles. This model reproduces successfully Ca II H and K,
  and H I Lyman-alpha and Lyman-beta, but partly fails with Mg II h and
  k. Atmospheric inhomogeneities and dynamical effects may contribute to
  this discrepancy, and it is proposed that the level number entering
  in the Mg II computation be increased to take account of a likely
  fluorescence induced by the H I Lyman-beta radiation field.

Title: Absorption feature observed on the H Lyman-alpha solar line -
    an interpretation
Authors: Artzner, G.; Cazes, S.; Emerich, C.; Vial, J. C.; Lemaire, P.
Bibcode: 1981A&A...100..205A
Altcode:
  A narrow absorption feature on the red part of the solar H Lyman-alpha
  profile has been observed by two instruments in 1975 and attributed
  to atomic hydrogen of the nearby interplanetary gas. This hypothesis
  implies that the absorption feature shifts with the position of the
  earth on its orbit. New measurements above active regions at other
  seasons rule out this hypothesis. On the other hand, appropriate
  laboratory calibrations indicate that the absorption feature is likely
  due to a ghost image of the geocoronal absorption.

Title: OSO-8 Observations of CAII H and K MGII H and K Lyman-Alpha
    and Lyman-Beta above a Sunspot
Authors: Kneer, F.; Scharmer, G.; Mattig, W.; Wyller, A.; Artzner,
   G.; Lemaire, P.; Vial, J. C.
Bibcode: 1981SoPh...69..289K
Altcode:
  Observations with the French (L.P.S.P.) experiment on board OSO-8 of
  a sunspot and nearby plage region are described. The behaviour of the
  emission cores of the Ca II H and K and Mg II h and k resonance lines is
  very similar and the correspondence in intensity between the four lines
  persists in all observed features. In contrast, the Lyman lines show
  little correlation with the other lines. Their emission regions appear
  broader in the spectroheliograms than the underlying sunspot structure
  and must not necessarily possess a counterpart in lower layers. From
  the central intensity of Lα above the umbra an electron density of
  4.3 × 10<SUP>10</SUP> cm<SUP>-3</SUP> ≲n<SUB>e</SUB><SUP>*</SUP>
  ≲2.3 × 10<SUP>11</SUP> cm<SUP>-3</SUP> at 20 000 K is estimated.

Title: Solar H I LY alpha far wing measurement
Authors: Jouchoux, A.; Vial, J. C.; Artzner, G. E.; Gouttebroze, P.;
   Lemaire, P.
Bibcode: 1981A&A....93..415J
Altcode:
  High spectral resolution photoelectric observations of the solar H I
  Ly alpha far wing are presented. Measurements above active regions and
  quiet sun center are compared to photographic observations of Basri
  et al. (1979).

Title: On VI (λ = 1032 Å) profiles in and above an active region
    prominence, compared to quiet Sun center and limb profiles
Authors: Vial, J. C.; Lemaire, P.; Artzner, G.; Gouttebroze, P.
Bibcode: 1980SoPh...68..187V
Altcode:
  O VI (λ = 1032 Å) profiles have been measured in and above a filament
  at the limb, previously analyzed in H I, Mg II, Ca II resonance lines
  (Vial et al., 1979). They are compared to profiles measured at the
  quiet Sun center and at the quiet Sun limb.

Title: Microturbulence near the edge of a solar plage
Authors: Simon, G.; Mouradian, Z.; Dumont, S.; Pecker, J. C.; Artzner,
   G.; Vial, J. C.
Bibcode: 1980A&A....89L...8S
Altcode:
  Observations of the Ca II K line at the edge of a solar plage show
  enhanced separation of the K2 peaks with respect to the measured value
  inside the plage and in the quiet sun. This effect may be interpreted as
  a variation of microturbulent motions at the height of formation of K2.

Title: Observations of Chromospheric Lines from OSO-8
Authors: Grossmann-Doerth, U.; Kneer, F.; Uexkuell, M.; Artzner,
   G. E.; Vial, J. C.
Bibcode: 1980SoPh...66....3G
Altcode:
  The line profiles of Lα, Ca II K and Mg IIk were measured with the
  spectrometer of the `Laboratoire de Physique Stellaire et Planétaire'
  on board of OSO-8. The results of these measurements are presented.

Title: Center-to-limb solar observations of the K<SUB>2</SUB>
    component of the Ca II K line with the OSO 8 satellite.
Authors: Dumont, S.; Mouradian, Z.; Pecker, J. -C.; Simon, G.; Artzner,
   G. E.; Vial, J. C.
Bibcode: 1980CRASB.290..365D
Altcode:
  OSO 8 spectrometer measurements of the separation between emission
  peaks in the K2 Ca II line across the solar disk in quiet and active
  regions are presented. The center-to-limb variation in emission peak
  separation is found to differ slightly for quiet and facula regions
  at distances greater than 0.2 solar radii from the limb, in agreement
  with previous observations. For a facula located at the solar limb,
  however, the peak separation is observed to be up to 35 percent greater
  than in quiet regions, indicating the presence of a region of enhanced
  chromospheric turbulence surrounding the faculae.

Title: Non thermal velocities in the chromosphere-corona transition
    zone of solar active regions.
Authors: Dumont, S.; Mouradian, Z.; Pecker, J. -C.; Chipman, E.;
   Artzner, G.; Vial, J. -C.
Bibcode: 1980CRASB.290..317D
Altcode:
  OSO 8 satellite observations of lines of the Si II, Si IV, C IV and
  O VI ions in the ultraviolet spectrum of active solar regions are
  considered. It is noted that for the case of pronounced physical
  dispersion of the data, there is no marked systematic variation from
  the center to the edge of the solar disk. The nonthermal velocities
  in the transition zone are, for a given temperature, the same as for
  quiet regions. In addition, the velocities tend to reach a constant
  value at temperatures above 100,000 deg K, and the observed physical
  dispersion is much higher than the inaccuracy of the data.

Title: Profiles of H I (Lalpha ), Mg II (h and k), Ca II (H and K)
    lines of an active filament at the limb, with the LPSP instrument
    aboard the OSO-8 satellite.
Authors: Vial, J. C.; Gouttebroze, P.; Artzner, G.; Lemaire, P.
Bibcode: 1979SoPh...61...39V
Altcode:
  We scanned the H I Lα, Mg II h and k, Ca II K and H lines
  simultaneously with the LPSP instrument on OSO-8, to investigate the low
  and moderate temperature regions of an `active region filament'. The
  Lα line is not reversed except for the innermost position in the
  prominence. Intensity (k/h), (K/H) ratios are respectively 2 and 1.1,
  indicating that the Mg II lines are optically thin, and that Ca II
  K is saturated, although not clearly reversed. The results obtained
  during the second sequence of observations (K saturated before Lα
  for example) indicate that within the size of the slit (1″ × 10″)
  we are not observing the same emitting features in the different lines.

Title: Profiles of H i (Lyα), MG II (h and K), CA II (h and k)
    Lines in an Active Filament at the Limb, Observed with the LPSP
    Instrument Onboard the OSO-8 Satellite.
Authors: Vial, J. C.; Gouttebroze, P.; Artzner, G.; Lemaire, P.
Bibcode: 1979phsp.coll..250V
Altcode: 1979IAUCo..44..250V
  No abstract at ADS

Title: The Solar H-Lyman-alpha Line
Authors: Artzner, G.
Bibcode: 1978A&A....70L..11A
Altcode:
  Summary A precise measurement of the solar H-Lya 121.6 nm profile
  is presented. A preliminary analysis indicates a) a 2.4 1 0.6 km/s
  redshift of the solar H-Lya emission over a moderately active region
  with respect to the geocoronal absorption ; and b) the presence of
  a faint absorption feature, redshif ted 32 km/s with respect to the
  geocoronal absorption line. Key words : Lyman-alpha - Solar spectrum -
  Chromosphere Downf low - Interstellar hydrogen.

Title: The solar hydrogen Lyman-beta and Lyman-alpha lines: disk
    center observations from OSO 8 compared with theoretical profiles.
Authors: Gouttebroze, P.; Lemaire, P.; Vial, J. C.; Artzner, G.
Bibcode: 1978ApJ...225..655G
Altcode:
  The solar La and Lfl lines of hydrogen have been measured at the center
  of the disk with the LPSP spectrometer aboard OSO 8. These line profiles
  are compared with theoretical profiles obtained with different solar
  atmospheric models, assuming either complete or partial frequency
  redistribution in scattering. The assumption of microturbulence for
  the velocity fields appears insufficient to account for the profiles
  of the line cores; better results are obtained with a blend of micro-
  and macroturbulence, which shows the need of a generalized treatment of
  the turbulent motions in the formation of these lines. If the effects
  of partial redistribution are taken into account, a good fit of the
  line wings requires higher temperatures, in the region under the
  plateau, than in the reference atmospheric model of Vernazza, Avrett,
  and Loeser. Subject headings: line formation - line profiles - Sun:
  chromosphere - Sun: spectra - ultraviolet: spectra

Title: Simultaneous time-resolved observations of the H Lalpha ,
    Mg k 2795 Å, and Ca K solar lines.
Authors: Artzner, G.; Leibacher, J.; Vial, J. C.; Lemaire, P.;
   Gouttebroze, P.
Bibcode: 1978ApJ...224L..83A
Altcode:
  No abstract at ADS

Title: Calibrated full disk solar H I Lyman-alpha and Lyman-beta
    profiles.
Authors: Lemaire, P.; Charra, J.; Jouchoux, A.; Vidal-Madjar, A.;
   Artzner, G. E.; Vial, J. C.; Bonnet, R. M.; Skumanich, A.
Bibcode: 1978ApJ...223L..55L
Altcode:
  Resolved solar H I Ly-alpha and -beta profiles have been recorded by the
  French LPSP experiment on OSO 8. Intensity observations at the center
  and the limb have been combined to obtain flux-equivalent profiles
  (5.46 plus or minus 30 percent and 0.078 plus or minus 25 percent
  erg/sq cm per sec for Ly-alpha and -beta, respectively). Comparison of
  the flux profiles with unresolved calibration rocket profiles allows
  one to obtain an absolute calibration.

Title: The LPSP instrument on OSO 8. II. In-flight performance and
    preliminary results.
Authors: Bonnet, R. M.; Lemaire, P.; Vial, J. C.; Artzner, G.;
   Gouttebroze, P.; Jouchoux, A.; Leibacher, J. W.; Skumanich, A.;
   Vidal-Madjar, A.
Bibcode: 1978ApJ...221.1032B
Altcode:
  The paper describes the in-flight performance for the first 18 months of
  operation of the LPSP (Laboratoire de Physique Stellaire et Planetaire)
  instrument incorporated in the OSO 8 launched June 1975. By means of
  the instrument, an absolute pointing accuracy of nearly one second
  was achieved in orbit during real-time operations. The instrument
  uses a Cassegrain telescope and a spectrometer simultaneously
  observing six wavelengths. In-flight performance is discussed with
  attention to angular resolution, spectral resolution, dispersion
  and grating mechanism (spectral scanner) stability, scattered light
  background and dark current, photometric standardization, and absolute
  calibration. Real-time operation and problems are considered with
  reference to pointing system problems, target acquisition, and L-alpha
  modulation. Preliminary results involving the observational program,
  quiet sun and chromospheric studies, quiet chromospheric oscillation
  and transients, sunspots and active regions, prominences, and aeronomy
  investigations are reported.

Title: Doppler Shifts measured in 0 VI line from OSO-B observations
    above and in the vicinity of plage Mc Math 13738.
Authors: Lemaire, P.; Skumanich, A.; Artzner, G.; Gouttebroze, P.;
   Vial, J. C.; Bonnet, R. M.; McWhirter, P.
Bibcode: 1978BAAS...10Q.440L
Altcode:
  No abstract at ADS

Title: OSO-8 Radio and X-ray observations of the 19 April 1977 flare.
Authors: Skumanich, A.; Jouchoux, A.; Castelli, J.; Lemaire, P.;
   Artzner, G.; Gouttebroze, P.; Vial, J. C.; Bonnet, R. M.
Bibcode: 1978BAAS...10..441S
Altcode:
  No abstract at ADS

Title: EUV observations of class-C X-ray flare by the LPSP
    (Laboratoire de Physique Stellaire et Planétaire du Centre National
    de la Recherche Scientifique) spectrometer on OSO-8.
Authors: Jouchoux, A.; Skumanich, A.; Bonnet, R. M.; Lemaire, P.;
   Artzner, G.; Leibacher, J.; Vial, J. C.; Vidal-Madjar, A.
Bibcode: 1977BAAS....9..432J
Altcode:
  No abstract at ADS

Title: The LPSP experiment on OSO-8. I - Instrumentation, description
    of operations, laboratory calibrations and pre-launch performances
Authors: Artzner, G.; Bonnet, R. M.; Vial, J. C.; Jouchoux, A.;
   Leibacher, J.; Vidal-Madjar, A.; Lemaire, P.
Bibcode: 1977SSI.....3..131A
Altcode:
  The characteristics of OSO-8, including its solar-pointed instrument
  assembly and rasters, are discussed, as well as the accompanying
  Laboratoire de Physique Stellaire et Planetaire (LPSP) instrumentation,
  which is designed to study the solar atmosphere with high spatial,
  spectral, and temporal resolution. The LPSP instrument, which consists
  of two subassemblies, a Cassegrainian telescope and a spectrometer,
  is described; main optical characteristics, including spectral lines
  observed, and means of correcting aberrations and eliminating stray
  light, are given for the spectrometer. Detectors and their capacities,
  and various filter wheel configurations available for detection of
  polarized light and discrimination of low orders of diffraction, are
  also described. The observation program, which consists of a study of
  solar prominences, flares, and dynamic and three-dimensional physical
  structures of the chromosphere, as well as determination of seasonal
  variations of some gases in earth's atmosphere, is reviewed. A detailed
  account of pre-launch tests and calibration procedures is also given.

Title: Extreme-Ultraviolet Observations of New Cycle Sunspots with
    the LPSP Spectrometer from OSO-8
Authors: Skumanich, A.; Jouchoux, A.; Artzner, G.; Bonnet, R. M.;
   Leibacher, J.; Lemaire, P.; Vial, J. C.; Vidal-Madjar, A.
Bibcode: 1977BAAS....9..340S
Altcode:
  No abstract at ADS

Title: On VI Profiles of Solar Quiet and Active Areas Recorded by
    OSO-8 LPSP Experiment".
Authors: Lemaire, P.; Artzner, G.; Vial, J. C.; Bonnet, R. M.;
   Gottebroze, P.; Jouchoux, A.; Vidal-Madjar, A.; McWhirter, P.;
   Leibacher, J.; Skumainich, A.
Bibcode: 1977uxsa.coll...46L
Altcode: 1977IAUCo..43...46L
  No abstract at ADS

Title: OSO-8 Observations of the EUV Chromospheric Network
Authors: Artzner, G.; Bonnet, R. M.; Leibacher, J.; Lemaire, P.;
   Skumanich, A.; Vial, J. C.; Vidal-Madjar, A.
Bibcode: 1976BAAS....8..332A
Altcode:
  No abstract at ADS

Title: Solar OVI Profiles as Observed by the French Experiment
    Aboard OSO-8
Authors: Lemaire, P.; Artzner, G.; Bonnet, R. M.; Vial, F. C.;
   Skumanich, A.; Leibacher, J.; Vidal-Madjar, A.
Bibcode: 1976BAAS....8R.331L
Altcode:
  No abstract at ADS

Title: Evolution of sunspot and active region morphology as observed
    on the resonance lines of Ca<SUP>+</SUP> (K, H), Mg<SUP>+</SUP>
    (k, h), hydrogen (Lalpha , Lbeta ), and O VI from OSO-8 (LPSP).
Authors: Artzner, G.; Skumanich, A.; Bonnet, R. M.; Vidal-Madjar,
   A.; Leibacher, J.; Lemaire, P.; Vial, J. C.
Bibcode: 1976BAAS....8..397A
Altcode:
  No abstract at ADS

Title: Periodic temporal phenomena in the solar chromosphere as
    observed from OSO-8 (LPSP).
Authors: Vial, J. C.; Leibacher, J.; Lemaire, P.; Artzner, G.; Bonnet,
   R. M.; Skumanich, A.; Vidal-Madjar, A.
Bibcode: 1976BAAS....8..397V
Altcode:
  No abstract at ADS

Title: Spatial variations of solar profiles of Ca<SUP>+</SUP> H and
    K, Mg<SUP>+</SUP> h and k, and Lyman alpha and beta (H I) resonance
    lines as observed from OSO-8 (LPSP).
Authors: Bonnet, R. M.; Artzner, G.; Leibacher, J.; Lemaire, P.;
   Skumanich, A.; Vial, J. C.; Vidal-Madjar, A.
Bibcode: 1976BAAS....8..397B
Altcode:
  No abstract at ADS

Title: Prominence Observations with the OSO-8 French Experiment
Authors: Vial, J. C.; Artzner, G.; Bonnet, R. M.; Lemaire, P.;
   Leibacher, J.; Skumanich, A.; Vidalmadjar, A.
Bibcode: 1976BAAS....8..344V
Altcode:
  No abstract at ADS

Title: High-Resolution Atmospheric Extinction Measurements from the
    French Experiment on Board the NASA Spacecraft OSO-8
Authors: Vidal-Madjar, A.; Roble, R. G.; Mankin, W. G.; Artzner, G.;
   Bonnet, R. M.; Lemaire, P.; Vial, J. C.
Bibcode: 1976ASSL...61..117V
Altcode: 1976aps..conf..117V
  No abstract at ADS

Title: High resolution atmospheric extinction measurements from the
    French experiment on board the NASA spacecraft OSO-8
Authors: Vidal-Madjar, A.; Artzner, G.; Bonnet, R. M.; Lemaire, P.;
   Vial, J. C.; Roble, R. G.; Mankin, W. G.
Bibcode: 1976atps.proc..117V
Altcode:
  The French instrument aboard OSO-8 is a multichannel, high-resolution UV
  spectrometer for observing very small areas of the sun simultaneously
  in the Ca II, Mg II, Lyman alpha, and Lyman beta lines. By observing
  extinction through the earth atmosphere, the spectrometer studies the
  three-dimensional structure and the composition of the atmosphere. The
  quality of data appears to give a 500 m vertical resolution both for
  O3 and O2; O3 is observed primarily from 55 to 75 km, while O2 is
  observed from 85 to 200 km. Data on the hydrogen absorption present a
  new method for evaluating exospheric temperature and atomic hydrogen
  density at each point of the exobase.

Title: High Resolution Spectroscopy of the Disk Chromosphere. III:
    Upward Moving Disturbances as Observed in the Ca II K-Line Wings
Authors: Beckers, J. M.; Artzner, G.
Bibcode: 1974SoPh...37..309B
Altcode:
  We describe the properties of dark structures which are seen in the
  K-line wings and which seem to propagate inward into the K-line core,
  or upward in the solar atmosphere. These so-called dark whiskers
  appear to be related to the bright disturbances (bright whiskers)
  described by Liu (1974). Both may be related to the shocks that heat
  the chromosphere and corona.

