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Author name code: dame
ADS astronomy entries on 2022-09-14
author:"Dame, Luc" 

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Title: SoSWEET solar activity and space weather mission for extreme
    events prediction, solar flares and CMEs, and solar ultraviolet
    variability influence on climate
Authors: Damé, Luc; Meftah, Mustapha
2022cosp...44.3214D    Altcode:
  SoSWEET (Solar ultraviolet variability & Space Weather Extreme
  EvenTs Microsatellite Mission) is an innovative small satellite mission
  proposed in response to the ESA Call for an F mission that aims to
  address, on one part, Space Weather extreme events prediction, solar
  flares and coronal mass ejections (CMEs) onset and, on the other,
  the solar ultraviolet variability influence on climate. Space Weather
  extreme events early detection/prediction is better observed in Lyman
  Alpha with 3 orders more sensitivity than in H Alpha and a resolution
  and contrast on eruptions largely superior to the commonly used He II
  line at 30.4 nm. Previsions are possible hours in advance by following
  flux ropes rising and deforming in the solar atmosphere. However, Lyman
  Alpha is a delicate spectral line to observe due to contamination
  and degradation of the transmission of instruments, as observed
  in the past. A disruptive telescope is developed to address this
  issue. Concerning climate and solar variability, it is worth recalling
  that UV is the only wavelength band with energy absorbed in the
  high atmosphere (stratosphere), creating ozone (Herzberg continuum,
  200-242 nm), and that high variability is most probably at the origin
  of a climate influence. A simultaneous observation of the incoming UV
  and of the ozone production, would bring an invaluable information on
  this process of solar-climate forcing (we recommend the simultaneous
  observation, by a constellation of cubesats, of ozone and of the Earth
  radiation budget: the GAIA-y78 constellation mission). To address these
  objectives and flares and CMEs observations, a small satellite of less
  than 150 kg on a PROBA or similar platform (OneWeb Arrow, etc.), and
  on a polar orbit for an almost continuous solar following, is chosen
  (a polar orbit is also essential to understand the relation between
  solar UV variability and stratospheric ozone on arctic and Antarctic
  regions); alternately, having the satellite at L1 Lagrange point would
  be a definitive advantage. The SoSWEET polar satellite model payload
  definition includes the disruptive SUAVE telescope (Solar Ultraviolet
  Advanced Variability Experiment), an optimized heavy-duty thermally
  stable off-axis SiC telescope for FUV (Lyman-Alpha) and MUV (200-242
  nm Herzberg continuum) imaging (sources of variability, extreme events
  detection), and the SOLSIM spectrometer (SOLar Spectral Irradiance
  Monitor), a newly designed double-monochromator instrument covering
  the 170-340 nm ultraviolet spectral range (absolute measurements)
  and providing 0.65 nm resolution still in within a limited mass-power
  budget. The payload is completed by a small but performing coronagraph,
  new UVC detectors (optimized for Herzberg continuum), Electron-Proton
  detectors and a vector magnetometer. Science objectives, mission
  profile and model payload will be presented.

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Title: HiRISE - High-Resolution Imaging and Spectroscopy Explorer
    - Ultrahigh resolution, interferometric and external occulting
    coronagraphic science
Authors: Erdélyi, Robertus; Damé, Luc; Fludra, Andrzej; Mathioudakis,
   Mihalis; Amari, T.; Belucz, B.; Berrilli, F.; Bogachev, S.; Bolsée,
   D.; Bothmer, V.; Brun, S.; Dewitte, S.; de Wit, T. Dudok; Faurobert,
   M.; Gizon, L.; Gyenge, N.; Korsós, M. B.; Labrosse, N.; Matthews,
   S.; Meftah, M.; Morgan, H.; Pallé, P.; Rochus, P.; Rozanov, E.;
   Schmieder, B.; Tsinganos, K.; Verwichte, E.; Zharkov, S.; Zuccarello,
   F.; Wimmer-Schweingruber, R.
2022ExA...tmp...21E    Altcode:
  Recent solar physics missions have shown the definite role of waves and
  magnetic fields deep in the inner corona, at the chromosphere-corona
  interface, where dramatic and physically dominant changes occur. HiRISE
  (High Resolution Imaging and Spectroscopy Explorer), the ambitious new
  generation ultra-high resolution, interferometric, and coronagraphic,
  solar physics mission, proposed in response to the ESA Voyage 2050
  Call, would address these issues and provide the best-ever and most
  complete solar observatory, capable of ultra-high spatial, spectral,
  and temporal resolution observations of the solar atmosphere, from the
  photosphere to the corona, and of new insights of the solar interior
  from the core to the photosphere. HiRISE, at the L1 Lagrangian
  point, would provide meter class FUV imaging and spectro-imaging,
  EUV and XUV imaging and spectroscopy, magnetic fields measurements,
  and ambitious and comprehensive coronagraphy by a remote external
  occulter (two satellites formation flying 375 m apart, with a
  coronagraph on a chaser satellite). This major and state-of-the-art
  payload would allow us to characterize temperatures, densities, and
  velocities in the solar upper chromosphere, transition zone, and inner
  corona with, in particular, 2D very high resolution multi-spectral
  imaging-spectroscopy, and, direct coronal magnetic field measurement,
  thus providing a unique set of tools to understand the structure and
  onset of coronal heating. HiRISE's objectives are natural complements
  to the Parker Solar Probe and Solar Orbiter-type missions. We present
  the science case for HiRISE which will address: i) the fine structure
  of the chromosphere-corona interface by 2D spectroscopy in FUV at
  very high resolution; ii) coronal heating roots in the inner corona by
  ambitious externally-occulted coronagraphy; iii) resolved and global
  helioseismology thanks to continuity and stability of observing at the
  L1 Lagrange point; and iv) solar variability and space climate with,
  in addition, a global comprehensive view of UV variability.

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Title: Origin of the Solar Rotation Harmonics Seen in the EUV and
    UV Irradiance
Authors: Giono, G.; Zender, J. J.; Kariyappa, R.; Damé, L.
2021SoPh..296..172G    Altcode:
  Long-term periodicities in the solar irradiance are often observed
  with periods proportional to the solar rotational period of 27
  days. These periods are linked either to some internal mechanism
  in the Sun or said to be higher harmonics of the rotation without
  further discussion of their origin. In this article, the origin of
  the peaks in periodicities seen in the solar extreme ultraviolet (EUV)
  and ultraviolet (UV) irradiance around the 7, 9, and 14 days periods is
  discussed. Maps of the active regions and coronal holes are produced
  from six images per day using the Spatial Possibilistic Clustering
  Algorithm (SPoCA), a segmentation algorithm. Spectral irradiance at
  coronal, transition-region/chromospheric, and photospheric levels are
  extracted for each feature as well as for the full disk by applying
  the maps to full-disk images (at 19.3, 30.4, and 170 nm sampling in
  the corona/hot flare plasma, the chromosphere/transition region, and
  the photosphere, respectively) from the Atmospheric Imaging Assembly
  (AIA) on board the Solar Dynamics Observatory (SDO) from January 2011
  to December 2018. The peaks in periodicities at 7, 9, and 14 days as
  well as the solar rotation around 27 days can be seen in almost all
  of the solar irradiance time series. The segmentation also provided
  time series of the active regions and coronal holes visible area
  (i.e. in the area observed in the AIA images, not corrected for the
  line-of-sight effect with respect to the solar surface), which also show
  similar peaks in periodicities, indicating that the periodicities are
  due to the change in area of the features on the solar disk rather than
  to their absolute irradiance. A simple model was created to reproduce
  the power spectral density of the area covered by active regions also
  showing the same peaks in periodicities. Segmentation of solar images
  allows us to determine that the peaks in periodicities seen in solar
  EUV/UV irradiance from a few days to a month are due to the change in
  area of the solar features, in particular, active regions, as they are
  the main contributors to the total full-disk irradiance variability. The
  higher harmonics of the solar rotation are caused by the clipping of
  the area signal as the regions rotate behind the solar limb.

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Title: Segmentation of Coronal Features to Understand the Solar
    EUV and UV Irradiance Variability III. Inclusion and Analysis of
    Bright Points
Authors: van der Zwaard, Rens; Bergmann, Matthias; Zender, Joe;
   Kariyappa, Rangaiah; Giono, Gabriel; Damé, Luc
2021SoPh..296..138V    Altcode:
  The study of solar irradiance variability is of great importance in
  heliophysics, Earth's climate, and space weather applications. These
  studies require careful identifying, tracking and monitoring of features
  in the solar photosphere, chromosphere, and corona. Do coronal bright
  points contribute to the solar irradiance or its variability as input
  to the Earth atmosphere? We studied the variability of solar irradiance
  for a period of 10 years (May 2010 - June 2020) using the Large Yield
  Radiometer (LYRA), the Sun Watcher using APS and image Processing
  (SWAP) on board PROBA2, and the Atmospheric Imaging Assembly (AIA),
  and applied a linear model between the segmented features identified
  in the EUV images and the solar irradiance measured by LYRA. Based
  on EUV images from AIA, a spatial possibilistic clustering algorithm
  (SPoCA) is applied to identify coronal holes (CHs), and a morphological
  feature detection algorithm is applied to identify active regions
  (ARs), coronal bright points (BPs), and the quiet Sun (QS). The
  resulting segmentation maps were then applied on SWAP images,
  images of all AIA wavelengths, and parameters such as the intensity,
  fractional area, and contribution of ARs/CHs/BPs/QS features were
  computed and compared with LYRA irradiance measurements as a proxy for
  ultraviolet irradiation incident to the Earth atmosphere. We modeled
  the relation between the solar disk features (ARs, CHs, BPs, and QS)
  applied to EUV images against the solar irradiance as measured by
  LYRA and the F10.7 radio flux. A straightforward linear model was
  used and corresponding coefficients computed using a Bayesian method,
  indicating a strong influence of active regions to the EUV irradiance
  as measured at Earth's atmosphere. It is concluded that the long- and
  short-term fluctuations of the active regions drive the EUV signal as
  measured at Earth's atmosphere. A significant contribution from the
  bright points to the LYRA irradiance could not be found.

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Title: The UVSQ-SAT/INSPIRESat-5 CubeSat Mission: First In-Orbit
    Measurements of the Earth's Outgoing Radiation
Authors: Meftah, Mustapha; Boutéraon, Thomas; Dufour, Christophe;
   Hauchecorne, Alain; Keckhut, Philippe; Finance, Adrien; Bekki, Slimane;
   Abbaki, Sadok; Bertran, Emmanuel; Damé, Luc; Engler, Jean-Luc;
   Galopeau, Patrick; Gilbert, Pierre; Lapauw, Laurent; Sarkissian, Alain;
   Vieau, André-Jean; Lacroix, Patrick; Caignard, Nicolas; Arrateig,
   Xavier; Hembise Fanton d'Andon, Odile Hembise Fanton; Mangin, Antoine;
   Carta, Jean-Paul; Boust, Fabrice; Mahé, Michel; Mercier, Christophe
2021RemS...13.1449M    Altcode:
  No abstract at ADS

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Title: Solar Soft X-ray Irradiance Variability, I: Segmentation
    of Hinode/XRT Full-Disk Images and Comparison with GOES (1 - 8 Å)
    X-Ray Flux
Authors: Adithya, H. N.; Kariyappa, Rangaiah; Shinsuke, Imada; Kanya,
   Kusano; Zender, Joe; Damé, Luc; Gabriel, Giono; DeLuca, Edward;
   Weber, Mark
2021SoPh..296...71A    Altcode:
  It is of great interest and importance to study the variabilities of
  solar EUV, UV and X-ray irradiance in heliophysics, in Earth's climate,
  and space weather applications. A careful study is required to identify,
  track, monitor and segment the different coronal features such as active
  regions (ARs), coronal holes (CHs), the background regions (BGs) and
  the X-ray bright points (XBPs) from spatially resolved full-disk images
  of the Sun. Variability of solar soft X-ray irradiance is studied for a
  period of 13 years (February 2007-March 2020, covers Solar Cycle 24),
  using the X-Ray Telescope on board the Hinode (Hinode/XRT) and GOES
  (1 - 8 Å). The full-disk X-ray images observed in Al_mesh filter
  from XRT are used, for the first time, to understand the solar X-ray
  irradiance variability measured, Sun as a star, by GOES instrument. An
  algorithm in Python has been developed and applied to identify and
  segment coronal X-ray features (ARs, CHs, BGs, and XBPs) from the
  full-disk soft X-ray observations of Hinode/XRT. The segmentation
  process has been carried out automatically based on the intensity
  level, morphology and sizes of the X-ray features. The total intensity,
  area, and contribution of ARs/CHs/BGs/XBPs features were estimated and
  compared with the full-disk integrated intensity (FDI) and GOES (1 -
  8 Å) X-ray irradiance measurements. The XBPs have been identified and
  counted automatically over the full disk to investigate their relation
  to solar magnetic cycle. The total intensity of ARs/CHs/BGs/XBPs/FD
  regions are compared with the GOES (1 - 8 Å) X-ray irradiance
  variations. We present the results obtained from Hinode/XRT full-disk
  images (in Al_mesh filter) and compare the resulting integrated
  full-disk intensity (FDI) with GOES X-ray irradiance. The X-ray
  intensity measured over ARs/CHs/BGs/XBPs/FD is well correlated with
  GOES X-ray flux. The contributions of the segmented X-ray features
  to FDI and X-ray irradiance variations are determined. It is found
  that the background and active regions have a greater impact on the
  X-ray irradiance fluctuations. The mean contribution estimated for the
  whole observed period of the background regions (BGs) will be around 65
  ±10.97 % , whereas the ARs, XBPs and CHs are 30 ±11.82 % , 4 ±1.18 %
  and 1 ±0.52 % , respectively, to total solar X-ray flux. We observed
  that the area and contribution of ARs and CHs varies with the phase of
  the solar cycle, whereas the BGs and XBPs show an anti-correlation. We
  find that the area of the coronal features is highly variable suggesting
  that their area has to be taken into account in irradiance models,
  in addition to their intensity variations. The time series results of
  XBPs suggest for an existence of anti-correlation between the number
  of XBPs and the sunspot numbers. It is also important to consider both
  the number variation and the contribution of XBPs in the reconstruction
  of total solar X-ray irradiance variability.

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Title: SoSWEET-SOUP: an enhanced constellation mission concept for
    Space Weather, extreme events, radiation budget and ozone
Authors: Damé, Luc; Bolsee, David; Sarkissian, Alain; Philippe,
   Duvel Jean; Keckhut, Philippe; Hauchecorne, Alain; Meftah, Mustapha;
   Bekki, Slimane; Pereira, Nuno; Thiéblemont, Rémi; Marchand, Marion;
   Cessateur, Gäel
2021cosp...43E1505D    Altcode:
  SoSWEET-SOUP is an innovative small satellites constellation which aims
  to measure on complementary platforms the solar influence on climate,
  namely on one part solar activity and spectral variability and, on
  the other, the different components of the Earth radiation budget,
  energy input and energy re-emitted at the top of the Earth atmosphere,
  with a particular focus on the UV part of the spectrum and on the
  ozone layer, which are most sensitive to solar variability. The
  UV is the only wavelength band with energy absorbed in the high
  atmosphere (stratosphere), in the ozone (Herzberg continuum, 200-242
  nm) and oxygen bands, and its high variability is most probably
  at the origin of a climate influence. A simultaneous observation
  of the incoming UV and of the ozone (O3) production, would bring an
  invaluable information on this process of solar-climate forcing. Space
  instruments have already measured the different components of the
  Earth radiation budget but this is, to our knowledge, the first time
  that all instruments could be operated simultaneously on coordinated
  platforms. This characteristic guarantees by itself obtaining new
  significant original scientific results. Another major scientific and
  operational objective is Space Weather extreme events detection that
  is better expressed in Lyman Alpha with 3 orders more sensitivity than
  in H Alpha and a resolution and contrast of eruptions largely superior
  to the commonly used He II line at 30.4 nm. Previsions are possible
  hours in advance by following flux ropes deformation and rising in the
  atmosphere. SoSWEET-SOUP is an evolution of the SUITS/SWUSV and SUMO
  earlier proposed missions, acknowledging the scientific advantages
  of associating a constellation of 12 small satellites of some 20 to
  30 kg (12 to 24 "U" or so nanosatellites) on equatorial orbits (+/-
  20° in latitude) to a small polar satellite of less than 150 kg on
  a OneWeb Arrow like platform for an almost continuous solar following
  (a polar orbit is also essential to understanding the relation between
  solar UV variability and stratospheric ozone on arctic and antarctic
  regions). SoSWEET polar satellite model payload definition's options
  are still under assessment but will include, on the polar satellite,
  SUAVE (Solar Ultraviolet Advanced Variability Experiment), an optimized
  heavy-duty thermally stable SiC telescope for FUV (Lyman-Alpha) and
  MUV (200-242 nm Herzberg continuum) imaging (sources of variability,
  extreme events detection), and SOLSIM (SOLar Spectral Irradiance
  Monitor), a newly designed double-monochromator instrument covering
  the 170-340 nm ultraviolet spectral range and in within a limited
  mass-power budget. Other instruments include a small coronagraph,
  new UVC detectors (optimized for Herzberg continuum) and ozone
  radiometers, an Earth radiation budget assembly, Electron-Proton
  detectors and a vector magnetometer. The constellation of small
  satellites includes, on its side, precise ozone profiles measurements
  ("miniGOMOS" experiment, derived from GOMOS ENVISAT, with dual Sun
  and stars occultations), including middle atmosphere temperature
  measurements (observing, during the diurnal part of the orbit, the
  vertical profile of the sunlight scattering at limb), and enhanced
  energy radiation budget monitors ("miniScaRaB" instrumental evolution
  of ScaRaB on Megha-Tropiques). Science objectives, mission profiles
  and model payloads will be presented and opportunities of missions
  and potential collaborations discussed.

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Title: SOLAR-v: A new solar spectral irradiance dataset based on
    SOLAR/SOLSPEC observations during solar cycle 24
Authors: Meftah, M.; Snow, M.; Damé, L.; Bolseé, D.; Pereira, N.;
   Cessateur, G.; Bekki, S.; Keckhut, P.; Sarkissian, A.; Hauchecorne, A.
2021A&A...645A...2M    Altcode:
  Context. Solar spectral irradiance (SSI) is the wavelength-dependent
  energy input to the top of the Earth's atmosphere. Solar ultraviolet
  (UV) irradiance represents the primary forcing mechanism for the
  photochemistry, heating, and dynamics of the Earth's atmosphere. Hence,
  both temporal and spectral variations in solar UV irradiance represent
  crucial inputs to the modeling and understanding of the behavior
  of the Earth's atmosphere. Therefore, measuring the long-term solar
  UV irradiance variations over the 11-year solar activity cycle (and
  over longer timescales) is fundamental. Thus, each new solar spectral
  irradiance dataset based on long-term observations represents a major
  interest and can be used for further investigations of the long-term
  trend of solar activity and the construction of a homogeneous solar
  spectral irradiance record. <BR /> Aims: The main objective of this
  article is to present a new solar spectral irradiance database (SOLAR-v)
  with the associated uncertainties. This dataset is based on solar UV
  irradiance observations (165-300 nm) of the SOLAR/SOLSPEC space-based
  instrument, which provides measurements of the full-disk SSI during
  solar cycle 24. <BR /> Methods: SOLAR/SOLSPEC made solar acquisitions
  between April 5, 2008 and February 10, 2017. During this period, the
  instrument was affected by the harsh space environment that introduces
  instrumental trends (degradation) in the SSI measurements. A new method
  based on an adaptation of the Multiple Same-Irradiance-Level (MuSIL)
  technique was used to separate solar variability and any uncorrected
  instrumental trends in the SOLAR/SOLSPEC UV irradiance measurements. <BR
  /> Results: A new method for correcting degradation has been applied
  to the SOLAR/SOLSPEC UV irradiance records to provide new solar cycle
  variability results during solar cycle 24. Irradiances are reported at
  a mean solar distance of 1 astronomical unit (AU). In the 165-242 nm
  spectral region, the SOLAR/SOLSPEC data agrees with the observations
  (SORCE/SOLSTICE) and models (SATIRE-S, NRLSSI 2) to within the 1-sigma
  error envelope. Between 242 and 300 nm, SOLAR/SOLSPEC agrees only with
  the models.

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Title: VizieR Online Data Catalog: Solar spectral irradiance during
    Solar Cycle 24 (Meftah+, 2021)
Authors: Meftah, M.; Snow, M.; Dame, L.; Bolsee, D.; Pereira, N.;
   Cessateur, G.; Bekki, S.; Keckhut, P.; Sarkissian, A.; Hauchecorne, A.
2020yCat..36450002M    Altcode:
  The SOLAR/SOLSPEC Solar Spectral Irradiance (SSI) data product is
  constructed using measurements from the SOLAR/SOLSPEC instrument
  (low time resolution) and the SATIRE-S model (data reconstruction
  to fill the gaps of SOLAR/SOLSPEC observations), which are combined
  into merged daily solar spectra over the spectral intervals shown
  in the table below. Irradiances are reported at a mean solar
  distance of 1AU. <P />SELECTION CRITERIA: date range: 20080405 to
  20170210 cadence: 24 hours (daily) spectral range: 165.0 to 3000.0
  nm number of data: 2396394 identifier<SUB>product</SUB>doi (CDS):
  XXXX.XXXX.XX identifier<SUB>product</SUB>doi_authority (CDS):
  http://dx.doi.org/ <P />DATA DEFINITIONS: number = 6 (name, type,
  format) nominal<SUB>date</SUB>yyyy-mm-dd nominal_time wavelength bin
  lower bound, f12.2 (nm) wavelength bin upper bound, f12.2 (nm) spectral
  solar irradiance, e12.6 (W/m<SUP>2</SUP>/nm^) irradiance_uncertainty,
  f12.8 (unitless, 1 sigma) <P />(1 data file).

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Title: Segmentation of coronal features to understand the solar EIV
    and UV irradiance variability
Authors: Zender, Joe; van der Zwaart, Rens; Kariyappa, Rangaiah;
   Damé, Luc; Giono, Gabriel
2020EGUGA..2219496Z    Altcode:
  The study of solar irradiance variability is of great importance in
  heliophysics, the Earth's climate, and space weather applications. These
  studies require careful identifying, tracking and monitoring of
  features in the solar magnetosphere, chromosphere, and corona. We
  studied the variability of solar irradiance for a period of 10 years
  (May 2010-January 2020) using the Large Yield Radiometer (LYRA), the
  Sun Watcher using APS and image Processing (SWAP) on board PROBA2, the
  Atmospheric Imaging Assembly (AIA), and the Helioseismic and Magnetic
  Imager (HMI) of on board the Solar Dynamics Observatory (SDO), and
  applied a linear model between the identified features and the measured
  solar irradiance by LYRA.We used the spatial possibilistic clustering
  algorithm (SPoCA) to identify coronal holes, and a morphological feature
  detection algorithm to identify active regions (AR), coronal bright
  points (BPS), and the quite sun (QS) and segment coronal features from
  the EUV observations of AIA. The AIA segmentation maps were then applied
  on SWAP images, images of all AIA wavelengths, HMI line-of-sight (LOS)
  magnetograms, and parameters such as the intensity, fractional area,
  and contribution of ARs/CHs/BPs/QS features were computed and compared
  with LYRA irradiance measurements as a proxy for ultraviolet irradiation
  incident to the Earth atmosphere.We modelled the relation between the
  solar disk features (ARs, CHs, BPs, and QS) applied to magnetrogram
  and EUV images against the solar irradiance as measured by LYRA and the
  F10.7 radio flux. To avoid correlation between different the segmented
  features, a principal component analysis (PCM) was done. Using the
  independent component, a straightforward linear model was used and
  corresponding coefficients computed using the Bayesian framework. The
  model selected is stable and coefficients converge well.The application
  of the model to data from 2010 to 2020 indicates that both at solar
  cycle timeframes as well as shorter timeframes, the active region
  influence the EUV irradiance as measured at Earth. Our model replicates
  the LYRA measured irradiance well.

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Title: VizieR Online Data Catalog: SOLAR-ISS Spectrum covering
    165-3000nm (Meftah+, 2020)
Authors: Meftah, M.; Dame, L.; Bolsee, D.; Pereira, N.; Snow, M.;
   Weber, M.; Bramstedt, K.; Hilbig, T.; Cessateur, G.; Boudjella,
   M. -Y.; Marchand, M.; Lefevre, F.; Thieblemont, R.; Sarkissian, A.;
   Hauchecorne, A.; Keckhut, P.; Bekki, S.
2020yCatp058029501M    Altcode:
  A new solar reference spectrum (SOLAR-ISS - V1.1) representative of
  the 2008 solar minimum was obtained from the measurements made by the
  SOLAR/SOLSPEC instrument and its calibrations. <P />(1 data file).

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Title: A New Version of the SOLAR-ISS Spectrum Covering the 165 -
    3000 nm Spectral Region
Authors: Meftah, M.; Damé, L.; Bolsée, D.; Pereira, N.; Snow,
   M.; Weber, M.; Bramstedt, K.; Hilbig, T.; Cessateur, G.; Boudjella,
   M. -Y.; Marchand, M.; Lefèvre, F.; Thiéblemont, R.; Sarkissian,
   A.; Hauchecorne, A.; Keckhut, P.; Bekki, S.
2020SoPh..295...14M    Altcode:
  The accurate measurement of the solar spectrum at the top of the
  atmosphere and its variability are fundamental inputs for solar physics
  (Sun modeling), terrestrial atmospheric photochemistry, and Earth's
  climate (climate's modeling). These inputs were the prime objective
  set in 1996 for the SOLAR International Space Station (ISS). The SOLAR
  package represents a set of three solar instruments measuring the
  total and spectral absolute irradiance from 16 nm to 3088 nm. SOLAR was
  launched with the European Columbus space laboratory in February 2008
  aboard the NASA Space Shuttle Atlantis. SOLAR on the ISS tracked the
  Sun until it was decommissioned in February 2017. The SOLar SPECtrum
  (SOLSPEC) instrument of the SOLAR payload allowed the measurement
  of solar spectra in the 165 - 3000 nm wavelength range for almost
  a decade. Until the end of its mission, SOLAR/SOLSPEC was pushed to
  its limits to test how it was affected by space environmental effects
  (external thermal factors) and to better calibrate the space-based
  spectrometer. To that end, a new solar reference spectrum (SOLAR-ISS -
  V1.1) representative of the 2008 solar minimum was obtained from
  the measurements made by the SOLAR/SOLSPEC instrument and its
  calibrations. The main purpose of this article is to improve the
  SOLAR-ISS reference spectrum (between 165 and 180 nm in the far
  ultraviolet, between 216.9 and 226.8 nm in the middle ultraviolet,
  and between 2400 and 3000 nm in the near-infrared). SOLAR-ISS has a
  resolution better than 0.1 nm between 165 and 1000 nm, and 1 nm in the
  1000 - 3000 nm wavelength range. Finally, a first comparison is made
  between the new SOLAR-ISS spectrum (V2.0) and the Total and Spectral
  solar Irradiance Sensor (TSIS-1) spectrum obtained from its first
  observations from the ISS. Indeed, the launch of TSIS in December
  2017 provides a new light on the absolute determination of the solar
  spectrum and especially in the infrared region of the spectrum.

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Title: Solar oblateness variations in phase with the 22 year-magnetic
    cycle
Authors: Damé, L.; Irbah, A.
2019AGUFMSH11D3392D    Altcode:
  The solar oblateness results from distortion processes due to several
  phenomena inside the Sun but also induced by the centrifugal potential
  of the surface rotation. This fundamental parameter is therefore of
  great scientific interest, but its measurements for more than a century
  are still very controversial, whether for its average value and/or its
  variations observed or not over time. Images acquired for almost the
  whole Cycle 24 during the roll calibration mode by the Helioseismic and
  Magnetic Imager (HMI) onboard the Solar Dynamic Observatory (SDO) are
  used for calculating solar oblateness. The average oblateness obtained
  is 8.8+/-0.8 milli-arcseconds in good agreement with measurements of
  the last two decades. Variations are observed in anti-phase with the
  solar activity during cycle 24 whereas they were in phase with activity
  of Cycle 23. More generally, the trend of both in phase variation
  during odd cycles and anti-phase variation during even cycles is also
  confirmed when revisiting past measurements. We give an overview of
  the main issues raised by solar oblateness, present the data used and
  processing method, and discuss the major results of this study.

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Title: Variations of Solar Oblateness with the 22 yr Magnetic Cycle
    Explain Apparently Inconsistent Measurements
Authors: Irbah, Abdanour; Mecheri, Redouane; Damé, Luc; Djafer,
   Djelloul
2019ApJ...875L..26I    Altcode:
  Solar oblateness results from distortion processes due to several
  phenomena inside of the Sun, but it can also be induced by the
  centrifugal potential of surface rotation. This fundamental parameter
  is of great scientific interest, yet for more than a century its
  measurements have remained a controversial topic, whether because of its
  average value or its variations observed (or not) over time. Special
  images acquired for almost the whole of Cycle 24 by the Helioseismic
  and Magnetic Imager on board the Solar Dynamic Observatory are used
  for calculating solar oblateness. The average oblateness obtained is
  8.8 ± 0.8 mas, in good agreement with measurements over the last two
  decades. Variations are observed in anti-phase with the solar activity
  during Cycle 24, whereas they were in phase with activity during Cycle
  23. More generally, the trend of both in-phase variation during odd
  cycles and anti-phase variation during even cycles is confirmed when
  revisiting past measurements. Therefore, it is possible that the Sun
  initiates a physical process resulting in a pulsation with the 22 yr
  magnetic cycle; it has extreme values during the polarity reversals,
  with a maximum swelling during odd cycles and the opposite for even
  ones. This oscillation could resolve the controversy surrounding
  past measurements.

---------------------------------------------------------
Title: AntarctiCor: Solar Coronagraph in Antarctica for the ESCAPE
    Project
Authors: Fineschi, S.; Capobianco, G.; Massone, G.; Susino, R.;
   Zangrilli, L.; Bemporad, A.; Liberatore, A.; Landini, F.; Romoli,
   M.; Damé, L.; Christille, J. M.; Sandri, P.; Marmonti, M.; Galy, C.
2019NCimC..42...26F    Altcode:
  The Antarctica solar coronagraph - AntarctiCor- for the "Extreme
  Solar Coronagraphy Antarctic Program Experiment" -ESCAPE- comprises
  an internally-occulted coronagraph based on the externally-occulted
  ASPIICS coronagraph for the ESA formation-flying PROBA-3 mission. This
  paper describes the AntarctiCor design for ground-based observations
  from the DomeC Antarctica plateau of the polarized broad-band (591 nm
  ± 5 nm) K-corona and of the narrow-band (FWHM = 0.5 nm), polarized
  emission of the coronal green-line at 530.3 nm. The science goal of
  these observations is to map the topology and dynamics of the coronal
  magnetic field, addressing coronal heating and space weather questions.

---------------------------------------------------------
Title: Solar radius determined from PICARD/SODISM observations
    and extremely weak wavelength dependence in the visible and the
    near-infrared
Authors: Meftah, M.; Corbard, T.; Hauchecorne, A.; Morand, F.; Ikhlef,
   R.; Chauvineau, B.; Renaud, C.; Sarkissian, A.; Damé, L.
2018A&A...616A..64M    Altcode:
  Context. In 2015, the International Astronomical Union (IAU) passed
  Resolution B3, which defined a set of nominal conversion constants for
  stellar and planetary astronomy. Resolution B3 defined a new value of
  the nominal solar radius (R<SUB>⊙</SUB><SUP>N</SUP> = 695 700 km
  km) that is different from the canonical value used until now (695
  990 km). The nominal solar radius is consistent with helioseismic
  estimates. Recent results obtained from ground-based instruments,
  balloon flights, or space-based instruments highlight solar radius
  values that are significantly different. These results are related to
  the direct measurements of the photospheric solar radius, which are
  mainly based on the inflection point position methods. The discrepancy
  between the seismic radius and the photospheric solar radius can be
  explained by the difference between the height at disk center and the
  inflection point of the intensity profile on the solar limb. At 535.7
  nm (photosphere), there may be a difference of ∼330 km between the
  two definitions of the solar radius. <BR /> Aims: The main objective
  of this work is to present new results of the solar radius in the
  near-ultraviolet, the visible, and the near-infrared from PICARD
  space-based and ground-based observations. Simulations show the
  strong influence of atmosphere effects (refraction and turbulence) on
  ground-based solar radius determinations and highlight the interest of
  space-based solar radius determinations, particularly during planet
  transits (Venus or Mercury), in order to obtain more realistic and
  accurate measurements. <BR /> Methods: Solar radius observations
  during the 2012 Venus transit have been made with the SOlar Diameter
  Imager and Surface Mapper (SODISM) telescope on board the PICARD
  spacecraft. We used the transit of Venus as an absolute calibration
  to determine the solar radius accurately at several wavelengths. Our
  results are based on the determination of the inflection point position
  of the solar limb-darkening function (the most common solar radius
  definition). A realistic uncertainty budget is provided for each solar
  radius obtained with the PICARD space-based telescope during the 2012
  Venus transit. The uncertainty budget considers several sources of
  error (detection of the centers of Venus and Sun in PICARD images,
  positions of Sun and Venus from ephemeris (planetary theory), PICARD
  on-board timing, PICARD spacecraft position, and optical distortion
  correction from PICARD images). <BR /> Results: We obtain new values
  of the solar radius from the PICARD mission at several wavelengths and
  in different solar atmosphere regions. The PICARD spacecraft with its
  SODISM telescope was used to measure the radius of the Sun during the
  Venus transit in 2012. At 535.7 nm, the solar radius is equal to 696 134
  ± 261 km (combined standard uncertainty based (ξ) on the uncertainty
  budget). At 607.1 nm, the solar radius is equal to 696 156 ± 145 km
  (ξ), and the standard deviation of the solar radius mean value is
  ±22 km. At 782.2 nm, the solar radius is equal to 696 192 ± 247 km
  (ξ). The PICARD space-based results as well as PICARD ground-based
  results show that the solar radius wavelength dependence in the visible
  and the near-infrared is extremely weak. The differences in inflection
  point position of the solar radius at 607.1 nm, 782.2 nm, and 1025.0
  nm from a reference at 535.7 nm are less than 60 km for the different
  PICARD measurements.

---------------------------------------------------------
Title: The New SCIAMACHY Reference Solar Spectral Irradiance and
    Its Validation
Authors: Hilbig, T.; Weber, M.; Bramstedt, K.; Noël, S.; Burrows,
   J. P.; Krijger, J. M.; Snel, R.; Meftah, M.; Damé, L.; Bekki, S.;
   Bolsée, D.; Pereira, N.; Sluse, D.
2018SoPh..293..121H    Altcode:
  This paper describes a new reference solar spectrum retrieved from
  measurements of the satellite instrument SCIAMACHY in the wavelength
  region from 0.24 μ m to 2.4 μ m and its comparison with several
  other established solar reference spectra. The SCIAMACHY reference
  spectrum was recorded early in the mission before substantial optical
  degradation due to the harsh space environment sets in. The radiometric
  calibration of SCIAMACHY, applied in this study, includes a physical
  model of the scanner unit. Furthermore, SCIAMACHY's internal white
  light source (WLS) is used to correct for on-ground to in-flight
  changes. The resultant calibrated solar spectrum from SCIAMACHY is
  in good agreement with several available solar spectral irradiance
  (SSI) references in the visible spectral range. Strong throughput
  losses due to detector icing in the near infrared (NIR) are now
  adequately accounted for. Nevertheless, a deficit with respect to the
  ATLAS-3 composite and SORCE/SIM SSI is observed in the NIR. However,
  the SCIAMACHY solar reference spectrum agrees well with the recently
  re-evaluated SOLAR/SOLSPEC-ISS and recent ground measurements taken
  at Mauna Loa in the NIR.

---------------------------------------------------------
Title: SoSWEET-SOUP (SOlar, Space Weather Extreme EvenTs and
    Stratospheric Ozone Ultimate Profiles) dual constellation mission
Authors: Damé, Luc; Meftah, Mustapha
2018cosp...42E.753D    Altcode:
  SoSWEET-SOUP is an innovative small satellites constellation which aims
  to measure on complementary platforms the solar influence on climate,
  namely on one part solar activity and spectral variability and, on
  the other, the different components of the Earth radiation budget,
  energy input and energy re-emitted at the top of the Earth atmosphere,
  with a particular focus on the UV part of the spectrum and on the ozone
  layer, which are most sensitive to solar variability. The far UV (FUV)
  is the only wavelength band with energy absorbed in the high atmosphere
  (stratosphere), in the ozone (Herzberg continuum, 200-220 nm) and oxygen
  bands, and its high variability is most probably at the origin of a
  climate influence. A simultaneous observation of the incoming FUV and
  of the ozone (O3) production, would bring an invaluable information on
  this process of solar-climate forcing. Space instruments have already
  measured the different components of the Earth radiative budget but
  this is, to our knowledge, the first time that all instruments will be
  operated simultaneously on coordinated platforms. This characteristic
  guarantees by itself obtaining new significant original scientific
  results. SoSWEET-SOUP is an evolution of the SUITS/SWUSV and SUMO
  proposed missions, acknowledging the scientific advantages of
  associating a constellation of 10 to 12 small satellites of some
  20 to 30 kg (12 "U" or so nanosatellites) on equatorial orbits (+/-
  20° in latitude) to a small polar satellite of 100 to 120 kg on a
  OneWeb like platform for an almost continuous solar following (a polar
  orbit is also essential to the understanding of the relation between
  solar UV variability and stratospheric ozone on arctic and antarctic
  regions).SoSWEET-SOUP definition's options are still under assessment
  but will include, on the polar satellite, SUAVE (Solar Ultraviolet
  Advanced Variability Experiment), an optimized heavy-duty thermally
  stable SiC telescope for FUV (Lyman-Alpha) and MUV (200-220 nm Herzberg
  continuum) imaging (sources of variability, extreme events detection),
  and SOLSIM (SOLar Spectral Irradiance Monitor), a newly designed
  double-monochromator instrument covering the 170-340 nm ultraviolet
  spectral range and in within a limited mass-power budget. Other
  instruments include a small coronagraph, UV and ozone radiometers,
  Earth radiative budget assembly, Electron-Proton detectors and a vector
  magnetometer. The constellation of small satellites includes, on its
  side, precise ozone profiles measurements (miniGOMOS experiment with
  dual Sun and stars occultations) and detailed energy radiative budget
  monitors. Science objectives, mission profiles and model payloads will
  be presented and opportunities of missions and potential collaborations
  discussed.

---------------------------------------------------------
Title: Eight years of solar observations with PICARD
Authors: Meftah, M.; Corbard, T.; Morand, F.; Renaud, C.; Ikhlef,
   R.; Fodil, M.; Vieau, A. -J.; Damé, L.
2018SPIE10704E..1FM    Altcode:
  PICARD is a mission devoted to solar variability observation, which
  aims at perpetuating valuable historical time-series of the solar
  radius. PICARD contains a double program with in-space and on-ground
  measurements using Ritchey-Chrétien telescopes. The PICARD spacecraft
  was launched on June 15, 2010, commissioned in-flight in October of
  the same year, and was retired in April 2014. PICARD ground-based
  observatory is functional since May 2011 in the Plateau de Calern
  (France), and is still operational today. We shall give an overview
  of the PICARD instrumentation and the performances of the existing
  ground-based telescope. We will also present our current results about
  solar radius variations after eight years of solar observations.

---------------------------------------------------------
Title: SERB, a first innovative proof-of-concept nano-satellite of
    a constellation to measure the Earth Radiation Budget
Authors: Meftah, Mustapha; Sarkissian, Alain; Damé, Luc; Keckhut,
   Philippe; Irbah, Abdanour; Bekki, Slimane; Thiéblemont, Rémi
2018cosp...42E2242M    Altcode:
  The only way to measure the imbalance with sufficient accuracy is to
  measure both the incoming solar radiations (total solar irradiance)
  and the outgoing terrestrial radiations (top of atmosphere outgoing
  longwave radiations and shortwave radiations) onboard the same
  satellite, and ideally, with the same instrument. The incoming solar
  radiations and the outgoing terrestrial radiations are of nearly equal
  magnitude of the order of 340.5 W/m2. The objective is to measure these
  quantities over time by using differential Sun-Earth measurements (to
  counter calibration errors) with an accuracy better than 0.05 W/m2. It
  is necessary to observe during a decade and to measure the global
  diurnal cycle with a dozen satellites. Solar irradiance and Earth
  Radiation Budget (SERB) is a potential first in orbit demonstration
  satellite. The SERB nano-satellite aims to measure on the same platform
  the different components of the Earth radiation budget and the total
  solar irradiance. Instrumental payloads (solar radiometer and Earth
  radiometers) can acquire the technical maturity for the future large
  missions (constellation that insure global measurement cover) by
  flying in a CubeSat. This presentation is intended to demonstrate the
  ability to build a low-cost satellite with a high accuracy measurement
  in order to have constant flow of data from space.

---------------------------------------------------------
Title: Cycle 24 variability of the ultraviolet solar spectral
    irradiance with the SOLAR/SOLSPEC 9 years of data from the
    International Space Station
Authors: Damé, Luc; Bolsee, David; Hauchecorne, Alain; Meftah,
   Mustapha; Irbah, Abdanour; Bekki, Slimane; Pereira, Nuno; Sluse,
   Dominique; Cessateur, Gäel
2018cosp...42E.754D    Altcode:
  Accurate measurements of solar spectral irradiance (SSI) and its
  temporal variation are of primary interest to better understand
  solar mechanisms and the links between solar variability and Earth's
  atmosphere and climate. We present recent Ultra Violet (UV) SSI
  observations performed by the SOLAR/SOLSPEC spectrometer on board
  the International Space Station. SOLAR/SOLSPEC observations cover the
  essential of the solar cycle 24, from April 5, 2008 to February 15,
  2017.We provide an evolution of the solar spectral irradiance during
  Cycle 24 using the SOLAR/SOLSPEC data thanks to revised engineering
  corrections, improved calibrations, and advanced procedures to account
  for thermal and aging corrections of the instrument. The SOLAR/SOLSPEC
  observations are compared with other measurements (SORCE/SOLSTICE,
  SORCE/SIM, SCIAMACHY) and models (SATIRE-S, NRLSSI).

---------------------------------------------------------
Title: Think the way to measure the Earth Radiation Budget and the
    Total Solar Irradiance with a small satellites constellation
Authors: Meftah, M.; Keckhut, P.; Damé, L.; Bekki, S.; Sarkissian,
   A.; Hauchecorne, A.
2018SPIE10641E..0SM    Altcode:
  Within the past decade, satellites constellations have become possible
  and practical. One of the interest to use a satellites constellation
  is to measure the true Earth Radiation Imbalance, which is a crucial
  quantity for testing climate models and for predicting the future course
  of global warming. This measurement presents a high interest because the
  2001-2010 decade has not shown the accelerating pace of global warming
  that most models predict, despite the fact that the greenhouse-gas
  radiative forcing continues to rise. All estimates (ocean heat content
  and top of atmosphere) show that over the past decade the Earth
  radiation imbalance ranges between 0.5 to 1W<SUP>-2</SUP>. Up to now,
  the Earth radiation imbalance has not been measured directly. The only
  way to measure the imbalance with sufficient accuracy is to measure both
  the incoming solar radiations (total solar irradiance) and the outgoing
  terrestrial radiations (top of atmosphere outgoing longwave radiations
  and shortwave radiations) onboard the same satellite, and ideally, with
  the same instrument. The incoming solar radiations and the outgoing
  terrestrial radiations are of nearly equal magnitude of the order of
  340.5W<SUP>-2</SUP>. The objective is to measure these quantities
  over time by using differential Sun-Earth measurements (to counter
  calibration errors) with an accuracy better than 0.05Wm<SUP>-2</SUP>
  at 1σ. It is also necessary to have redundant instruments to track
  aging in space in order to measure during a decade and to measure the
  global diurnal cycle with a dozen satellites. Solar irradiance and Earth
  Radiation Budget (SERB) is a potential first in orbit demonstration
  satellite. The SERB nano-satellite aims to measure on the same platform
  the different components of the Earth radiation budget and the total
  solar irradiance. Instrumental payloads (solar radiometer and Earth
  radiometers) can acquire the technical maturity for the future large
  missions (constellation that insure global measurement cover) by flying
  in a CubeSat. This paper is intended to demonstrate the ability to
  build a low-cost satellite with a high accuracy measurement in order
  to have constant flow of data from space.

---------------------------------------------------------
Title: The Measurement of the Solar Spectral Irradiance during the
    Solar Cycle 24 using SOLAR/SOLSPEC on ISS
Authors: Bolsée, David; Pereira, Nuno; Sluse, Dominique; Cessateur,
   Gaël; Meftah, Mustapha; Damé, Luc; Hauchecorne, Alain; Bekki,
   Slimane; Marchand, Marion
2018EGUGA..2013041B    Altcode:
  Between April 2008 and February 2017, the Solar Spectral Irradiance
  (SSI) was measured by the SOLAR/SOLSPEC from 166 nm to 3088 nm. The
  instrument was a part of the Solar Monitoring Observatory (SOLAR)
  payload, externally mounted on the Columbus module of the International
  Space Station. As the SSI is a key input for the validation of solar
  physics models, together with playing a role in the climate system
  and photochemistry of the Earth atmosphere, SOLAR/SOLSPEC spectral
  measurements becomes important. In this study, the in-flight operations
  and performances of the instrument -including the engineering
  corrections- will be presented for the nine years of the SOLAR
  mission. Using an accurate absolute calibration, the SSI as measured
  by SOLAR/SOLSPEC in the course of the solar cycle 24 will be presented
  and compared to other instruments and ground-based measurements. The
  accuracy of these measurements will be also discussed here.

---------------------------------------------------------
Title: Recent variability of the solar spectral irradiance by using
    SOLAR/SOLSPEC data
Authors: Meftah, Mustapha; Damé, Luc; Hauchecorne, Alain; Irbah,
   Abdanour; Bekki, Slimane; Bolsée, David; Pereira, Nuno; Sluse,
   Dominique; Cessateur, Gael
2018EGUGA..20.3498M    Altcode:
  Accurate measurements of the solar spectral irradiance (SSI) and
  its temporal variation are of primary interest to better understand
  solar mechanisms and the links between solar variability and Earth's
  atmosphere and climate. We will present recent Ultra Violet (UV) SSI
  observations performed by the SOLAR/SOLSPEC spectrometer on board the
  International Space Station. SOLAR/SOLSPEC observations covered the
  essential of the solar cycle 24 from April 5, 2008 to February 15,
  2017. We wish to provide evolution of solar spectral irradiance during
  Cycle 24 using the SOLAR/SOLSPEC data thanks to revised engineering
  corrections, improved calibrations, and advanced procedures to account
  for thermal and aging corrections of the instrument. The SOLAR/SOLSPEC
  observations will be directly compared with other measurements
  (SORCE/SOLSTICE, SORCE/SIM) and models (SATIRE-S, NRLSSI).

---------------------------------------------------------
Title: Investigation of the low flux servo-controlled limit of a
    co-phased interferometer
Authors: Damé, Luc; Derrien, Marc; Kozlowski, Mathias; Merdjane,
   Mohamed
2018SPIE10570E..0UD    Altcode:
  This paper, "Investigation of the low flux servo-controlled limit of
  a co-phased interferometer," was presented as part of International
  Conference on Space Optics—ICSO 1997, held in Toulouse, France.

---------------------------------------------------------
Title: SOLAR/SOLSPEC: a new solar reference spectrum, SOLAR-ISS
    165-3000 nm and 9 years observations of solar spectral irradiance
    from space from the ISS
Authors: Damé, Luc; Meftah, Mustapha; Hauchecorne, Alain; Irbah,
   Abdenour; Bekki, Slimane; Bolsée, David; Pereira, Nuno; Sluse,
   Dominique; Cessateur, Gael
2018EGUGA..2016445D    Altcode:
  For 9 years since April 5, 2008 and until February 15, 2017, the SOLSPEC
  (SOLar SPECtrometer) spectro-radiometer of the SOLAR facility on the
  International Space Station (ISS) performed accurate measurements
  of Solar Spectral Irradiance (SSI) from the far ultraviolet to the
  infrared (165 nm to 3000 nm). These measurements, unique by their large
  spectral coverage and long time range, are of primary importance for
  a better understanding of solar physics and of the impact of solar
  variability on climate (via Earth's atmospheric photochemistry),
  noticeably through the "top-down" mechanism amplifying ultraviolet
  solar forcing effects on the climate (UV affects stratospheric dynamics
  and temperatures, altering interplanetary waves and weather patterns
  both poleward and downward to the lower stratosphere and troposphere
  regions). SOLAR/SOLSPEC, with almost 9 years of observations covering
  the essential of the unusual solar cycle 24, followed UV temporal
  variability and established a new reference solar spectra from UV
  to IR (165-3000 nm). A complete reanalysis of data was possible
  thanks to revised engineering corrections, improved calibrations
  and advanced procedures to account for thermal influence, aging
  (degradation) and pointing corrections. These intensive ground and
  space calibrations allowed a proper evaluation of uncertainties on these
  measurements. Results, UV variability and absolute reference spectrum
  (SOLAR-ISS), are displayed and compared with other measurements (WHI,
  ATLAS-3, SCIAMACHY, SORCE/SOLSTICE, SORCE/SIM) and models (SATIRE-S,
  NRLSSI2).

---------------------------------------------------------
Title: SOLAR-ISS: A new reference spectrum based on SOLAR/SOLSPEC
    observations
Authors: Meftah, M.; Damé, L.; Bolsée, D.; Hauchecorne, A.; Pereira,
   N.; Sluse, D.; Cessateur, G.; Irbah, A.; Bureau, J.; Weber, M.;
   Bramstedt, K.; Hilbig, T.; Thiéblemont, R.; Marchand, M.; Lefèvre,
   F.; Sarkissian, A.; Bekki, S.
2018A&A...611A...1M    Altcode:
  Context. Since April 5, 2008 and up to February 15, 2017, the SOLar
  SPECtrometer (SOLSPEC) instrument of the SOLAR payload on board the
  International Space Station (ISS) has performed accurate measurements
  of solar spectral irradiance (SSI) from the middle ultraviolet to
  the infrared (165 to 3088 nm). These measurements are of primary
  importance for a better understanding of solar physics and the impact
  of solar variability on climate. In particular, a new reference solar
  spectrum (SOLAR-ISS) is established in April 2008 during the solar
  minima of cycles 23-24 thanks to revised engineering corrections,
  improved calibrations, and advanced procedures to account for thermal
  and aging corrections of the SOLAR/SOLSPEC instrument. <BR /> Aims:
  The main objective of this article is to present a new high-resolution
  solar spectrum with a mean absolute uncertainty of 1.26% at 1σ from 165
  to 3000 nm. This solar spectrum is based on solar observations of the
  SOLAR/SOLSPEC space-based instrument. <BR /> Methods: The SOLAR/SOLSPEC
  instrument consists of three separate double monochromators that use
  concave holographic gratings to cover the middle ultraviolet (UV),
  visible (VIS), and infrared (IR) domains. Our best ultraviolet, visible,
  and infrared spectra are merged into a single absolute solar spectrum
  covering the 165-3000 nm domain. The resulting solar spectrum has a
  spectral resolution varying between 0.6 and 9.5 nm in the 165-3000 nm
  wavelength range. We build a new solar reference spectrum (SOLAR-ISS)
  by constraining existing high-resolution spectra to SOLAR/SOLSPEC
  observed spectrum. For that purpose, we account for the difference of
  resolution between the two spectra using the SOLAR/SOLSPEC instrumental
  slit functions. <BR /> Results: Using SOLAR/SOLSPEC data, a new solar
  spectrum covering the 165-3000 nm wavelength range is built and is
  representative of the 2008 solar minimum. It has a resolution better
  than 0.1 nm below 1000 nm and 1 nm in the 1000-3000 nm wavelength
  range. The new solar spectrum (SOLAR-ISS) highlights significant
  differences with previous solar reference spectra and with solar
  spectra based on models. The integral of the SOLAR-ISS solar spectrum
  yields a total solar irradiance of 1372.3 ± 16.9 Wm<SUP>-2</SUP>
  at 1σ, that is yet 11 Wm<SUP>-2</SUP> over the value recommended
  by the International Astronomical Union in 2015. <P />The spectrum
  shown in Fig. B.1 is available at the CDS via anonymous ftp to <A
  href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (<A
  href="http://cdsarc.u-strasbg.fr">http://130.79.128.5</A>) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/611/A1">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/611/A1</A>

---------------------------------------------------------
Title: Solar-Iss a New Solar Reference Spectrum Covering the Far UV
    to the Infrared (165 to 3088 Nm) Based on Reanalyzed Solar/solspec
    Cycle 24 Observations
Authors: Damé, L.; Meftah, M.; Irbah, A.; Hauchecorne, A.; Bekki,
   S.; Bolsée, D.; Pereira, N.; Sluse, D.; Cessateur, G.
2017AGUFMSH42A..07D    Altcode:
  Since April 5, 2008 and until February 15, 2017, the SOLSPEC
  (SOLar SPECtrometer) spectro-radiometer of the SOLAR facility on the
  International Space Station performed accurate measurements of Solar
  Spectral Irradiance (SSI) from the far ultraviolet to the infrared
  (165 nm to 3088 nm). These measurements, unique by their large spectral
  coverage and long time range, are of primary importance for a better
  understanding of solar physics and of the impact of solar variability
  on climate (via Earth's atmospheric photochemistry), noticeably
  through the "top-down" mechanism amplifying ultraviolet (UV) solar
  forcing effects on the climate (UV affects stratospheric dynamics
  and temperatures, altering interplanetary waves and weather patterns
  both poleward and downward to the lower stratosphere and troposphere
  regions). SOLAR/SOLSPEC, with almost 9 years of observations covering
  the essential of the unusual solar cycle 24 from minimum in 2008
  to maximum, allowed to establish new reference solar spectra from
  UV to IR (165 to 3088 nm) at minimum (beginning of mission) and
  maximum of activity. The complete reanalysis was possible thanks to
  revised engineering corrections, improved calibrations and advanced
  procedures to account for thermal, aging and pointing corrections. The
  high quality and sensitivity of SOLSPEC data allow to follow temporal
  variability in UV but also in visible along the cycle. Uncertainties
  on these measurements are evaluated and results, absolute reference
  spectra and variability, are compared with other measurements (WHI,
  ATLAS-3, SCIAMACHY, SORCE/SOLSTICE, SORCE/SIM) and models (SATIRE-S,
  NRLSSI, NESSY)

---------------------------------------------------------
Title: SSI Variations in the visible as observed with SOLAR/SOLSPEC
    during cycle 24 - Comparison with SORCE/SIM.
Authors: Irbah, A.; Damé, L.; Meftah, M.; Bekki, S.; Bolsée, D.
2017AGUFMSH43B2808I    Altcode:
  The solar spectral irradiance (SSI) and its temporal variations
  are of prime importance to apprehend the physics of the Sun and to
  understand its effects on Earth climate through changes of atmospheric
  properties. Ground based measurements of SSI are indeed affected by
  the Earth atmosphere and space observations are therefore required
  to perform adequate observations. Only a few long series of SSI space
  measurements were obtained these last decades. The SOLSPEC instrument
  of the SOLAR payload on the International Space Station (ISS) has
  recorded one of them from April 2008 to February 2017 covering almost
  the whole solar cycle 24. The instrument is a spectro-radiometer
  recording data of the Sun from 166 to 3088 nm. Operated from the ISS
  in a harsh environment it needed appropriate processing methods to
  extract significant scientific results from noise and instrumental
  effects. We present the methods used to process the data to evidence
  visible SSI variations during cycle 24. We discuss the results obtained
  showing SSI variations in phase with solar activity. We compare them
  with SORCE/SIM measurements.

---------------------------------------------------------
Title: ASPIICS: a giant, white light and emission line coronagraph
    for the ESA proba-3 formation flight mission
Authors: Lamy, P. L.; Vivès, S.; Curdt, W.; Damé, L.; Davila, J.;
   Defise, J. -M.; Fineschi, S.; Heinzel, P.; Howard, Russel; Kuzin,
   S.; Schmutz, W.; Tsinganos, K.; Zhukov, A.
2017SPIE10565E..0TL    Altcode:
  Classical externally-occulted coronagraphs are presently limited in
  their performances by the distance between the external occulter and
  the front objective. The diffraction fringe from the occulter and
  the vignetted pupil which degrades the spatial resolution prevent
  useful observations of the white light corona inside typically 2-2.5
  solar radii (Rsun). Formation flying offers and elegant solution to
  these limitations and allows conceiving giant, externally-occulted
  coronagraphs using a two-component space system with the external
  occulter on one spacecraft and the optical instrument on the
  other spacecraft at a distance of hundred meters [1, 2]. Such
  an instrument ASPIICS (Association de Satellites Pour l'Imagerie
  et l'Interférométrie de la Couronne Solaire) has been selected
  by the European Space Agency (ESA) to fly on its PROBA-3 mission
  of formation flying demonstration which is presently in phase B
  (Fig. 1). The classical design of an externally-occulted coronagraph is
  adapted to the formation flying configuration allowing the detection
  of the very inner corona as close as 0.04 solar radii from the solar
  limb. By tuning the position of the occulter spacecraft, it may even be
  possible to reach the chromosphere and the upper part of the spicules
  [3]. ASPIICS will perform (i) high spatial resolution imaging of the
  continuum K+F corona in photometric and polarimetric modes, (ii) high
  spatial resolution imaging of the E-corona in two coronal emission lines
  (CEL): Fe XIV and He I D3, and (iii) two-dimensional spectrophotometry
  of the Fe XIV emission line. ASPIICS will address the question of the
  coronal heating and the role of waves by characterizing propagating
  fluctuations (waves and turbulence) in the solar wind acceleration
  region and by looking for oscillations in the intensity and Doppler
  shift of spectral lines. The combined imaging and spectral diagnostics
  capabilities available with ASPIICS will allow mapping the velocity
  field of the corona both in the sky plane (directly on the images)
  and along the line-of-sight by measuring the Doppler shifts of
  emission lines in an effort to determine how the different components
  of the solar wind, slow and fast are accelerated. With a possible
  launch in 2014, ASPIICS will observe the corona during the maximum of
  solar activity, insuring the detection of many Coronal Mass Ejections
  (CMEs). By rapidly alternating high-resolution imaging and spectroscopy,
  CMEs will be thoroughly characterized.

---------------------------------------------------------
Title: High resolution solar physics by aperture synthesis: the
    SOLARNET program
Authors: Derrien, Marc; Damé, Luc; Perrot, Sylvain; Kozlowski, Mathias
2017SPIE10569E..2GD    Altcode:
  We present the 3 telescopes breadboards used to demonstrate the
  cophasing and imaging capabilities of the Solar Imaging Interferometer
  (SOLARNET).

---------------------------------------------------------
Title: A solar diameter metrology measurement: the Picard
    microsatellite program
Authors: Damé, Luc; Brun, Jean-Francis; Cugnet, David; Derrien, Marc;
   Leroy, Claude; Meftah, Mustapha; Meissonnier, Mireille; Porteneuve,
   Jacques
2017SPIE10569E..14D    Altcode:
  The PICARD microsatellite mission will provide 3 to 4 years
  simultaneous measurements of the solar diameter, differential rotation
  and solar constant to investigate the nature of their relations and
  variabilities. The major instrument, SODISM, is a whole Sun imaging
  telescope of Ø110 mm which will deliver an absolute measure (better
  than 4 mas) of the solar diameter and solar shape. Now in Phase B,
  PICARD is expected to be launched by 2005. We recall the scientific
  goals linked to the diameter measurement with interest for Earth
  Climate, Space Weather and Helioseismology, present the instrument
  optical concept and design, and give a brief overview of the program
  aspects.

---------------------------------------------------------
Title: Mathematical modelling of the complete metrology of the
    PROBA-3/ASPIICS formation flying solar coronagraph
Authors: Stathopoulos, F.; Vives, S.; Damé, L.; Tsinganos, K.
2017SPIE10565E..2SS    Altcode:
  Formation flying, with ESA's mission PROBA-3, is providing the chance of
  creating a giant solar coronagraph in Space. The scientific payload,
  the solar coronagraph ASPIICS, has been selected in January 2009
  [1]. The advantages of formation flying are: 1) larger dimensions
  for the coronagraph, which leads to better spatial resolution and
  lower straylight level and 2) possibility of continuous observations
  of the inner corona. The PROBA-3/ASPIICS mission is composed of two
  spacecrafts (S/Cs) at 150 meters distance, the Occulter-S/C (O-S/C)
  which holds the external occulter, and the Coronagraph-S/C (C-S/C)
  which holds the main instrument, i.e. the telescope. In addition of
  the scientific capabilities of the instrument, it will continuously
  monitor the exact position and pointing of both S/Cs in 3D space, via
  two additional metrology units: the Shadow Position Sensor (SPS) and
  the Occulter Position Sensor (OPS). In this paper we are presenting the
  metrology of this formation flying mission combining the outputs of the
  above mentioned sensors, SPS and OPS. This study has been conducted in
  the framework of an ESA "STARTIGER" initiative, a novel approach aimed
  at demonstrating the feasibility of a new and promising technology
  concept (in our case formation flying applied to solar coronagraphy,
  cf. [2, 3]) on a short time scale (six months study).

---------------------------------------------------------
Title: VizieR Online Data Catalog: SOLAR/SOLSPEC Spectral Irradiance -
    0.5-3000nm (Meftah+, 2018)
Authors: Meftah, M.; Dame, L.; Bolsee, D.; Hauchecorne, A.; Pereira,
   N.; Sluse, D.; Cessateur, G.; Irbah, A.; Bureau, J.; Weber, M.;
   Bramstedt, K.; Hilbig, T.; Thieblemont, R.; Marchand, M.; Lefevre,
   F.; Sarkissian, A.; Bekki, S.
2017yCat..36110001M    Altcode:
  The SOLAR/SOLSPEC space-based instrument has measured the solar spectral
  irradiance from 165 to 3000nm at 0.6 to 9.5nm spectral resolution during
  the almost nine years of the SO- LAR/ISS mission. The instrument was
  calibrated using the PTB standard blackbody developed for temperatures
  up to 3200K. The absolute accuracy, based on a detailed analysis of
  error sources, indicates a mean absolute uncertainty of 1.26% of the
  total solar irradiance in the 165-3000nm range. Using SOLAR/SOLSPEC
  data, a new solar spectrum (SOLAR-ISS) covering the 165-3000nm
  wavelength range is built with added high spectral resolution. This
  SOLAR-ISS spectrum is developed by combining high spectral resolution
  from reference solar spectra with the resulting SOLAR/SOLSPEC spectrum
  through the knowledge of the slit functions of the SOLAR/SOLSPEC
  instrument. <P />(1 data file).

---------------------------------------------------------
Title: Segmentation of photospheric magnetic elements corresponding to
    coronal features to understand the EUV and UV irradiance variability
Authors: Zender, J. J.; Kariyappa, R.; Giono, G.; Bergmann, M.;
   Delouille, V.; Damé, L.; Hochedez, J. -F.; Kumara, S. T.
2017A&A...605A..41Z    Altcode:
  Context. The magnetic field plays a dominant role in the solar
  irradiance variability. Determining the contribution of various magnetic
  features to this variability is important in the context of heliospheric
  studies and Sun-Earth connection. <BR /> Aims: We studied the solar
  irradiance variability and its association with the underlying magnetic
  field for a period of five years (January 2011-January 2016). We used
  observations from the Large Yield Radiometer (LYRA), the Sun Watcher
  with Active Pixel System detector and Image Processing (SWAP) on board
  PROBA2, the Atmospheric Imaging Assembly (AIA), and the Helioseismic
  and Magnetic Imager (HMI) on board the Solar Dynamics Observatory
  (SDO). <BR /> Methods: The Spatial Possibilistic Clustering Algorithm
  (SPoCA) is applied to the extreme ultraviolet (EUV) observations
  obtained from the AIA to segregate coronal features by creating
  segmentation maps of active regions (ARs), coronal holes (CHs) and
  the quiet sun (QS). Further, these maps are applied to the full-disk
  SWAP intensity images and the full-disk (FD) HMI line-of-sight (LOS)
  magnetograms to isolate the SWAP coronal features and photospheric
  magnetic counterparts, respectively. We then computed full-disk
  and feature-wise averages of EUV intensity and line of sight (LOS)
  magnetic flux density over ARs/CHs/QS/FD. The variability in these
  quantities is compared with that of LYRA irradiance values. <BR />
  Results: Variations in the quantities resulting from the segmentation,
  namely the integrated intensity and the total magnetic flux density
  of ARs/CHs/QS/FD regions, are compared with the LYRA irradiance
  variations. We find that the EUV intensity over ARs/CHs/QS/FD is well
  correlated with the underlying magnetic field. In addition, variations
  in the full-disk integrated intensity and magnetic flux density values
  are correlated with the LYRA irradiance variations. <BR /> Conclusions:
  Using the segmented coronal features observed in the EUV wavelengths as
  proxies to isolate the underlying magnetic structures is demonstrated
  in this study. Sophisticated feature identification and segmentation
  tools are important in providing more insights into the role of various
  magnetic features in both the short- and long-term changes in the solar
  irradiance. <P />The movie associated to Fig. 2 is available at <A
  href="http://www.aanda.org/10.1051/0004-6361/201629924/olm">http://www.aanda.org</A>

---------------------------------------------------------
Title: A New Solar Spectrum from 656 to 3088 nm
Authors: Meftah, M.; Damé, L.; Bolsée, D.; Pereira, N.; Sluse, D.;
   Cessateur, G.; Irbah, A.; Sarkissian, A.; Djafer, D.; Hauchecorne,
   A.; Bekki, S.
2017SoPh..292..101M    Altcode:
  The solar spectrum is a key parameter for different scientific
  disciplines such as solar physics, climate research, and atmospheric
  physics. The SOLar SPECtrometer (SOLSPEC) instrument of the Solar
  Monitoring Observatory (SOLAR) payload onboard the International Space
  Station (ISS) has been built to measure the solar spectral irradiance
  (SSI) from 165 to 3088 nm with high accuracy. To cover the full
  wavelength range, three double-monochromators with concave gratings are
  used. We present here a thorough analysis of the data from the third
  channel/double-monochromator, which covers the spectral range between
  656 and 3088 nm. A new reference solar spectrum is therefore obtained
  in this mainly infrared wavelength range (656 to 3088 nm); it uses
  an absolute preflight calibration performed with the blackbody of the
  Physikalisch-Technische Bundesanstalt (PTB). An improved correction of
  temperature effects is also applied to the measurements using in-flight
  housekeeping temperature data of the instrument. The new solar spectrum
  (SOLAR-IR) is in good agreement with the ATmospheric Laboratory for
  Applications and Science (ATLAS 3) reference solar spectrum from 656
  nm to about 1600 nm. However, above 1600 nm, it agrees better with
  solar reconstruction models than with spacecraft measurements. The new
  SOLAR/SOLSPEC measurement of solar spectral irradiance at about 1600
  nm, corresponding to the minimum opacity of the solar photosphere,
  is 248.08 ± 4.98 mW m<SUP>−2</SUP> nm<SUP>−1</SUP> (1 σ ),
  which is higher than recent ground-based evaluations.

---------------------------------------------------------
Title: On-orbit degradation of recent space-based solar instruments
    and understanding of the degradation processes
Authors: Meftah, M.; Dominique, M.; BenMoussa, A.; Dammasch, I. E.;
   Bolsée, D.; Pereira, N.; Damé, L.; Bekki, S.; Hauchecorne, A.
2017SPIE10196E..06M    Altcode:
  The space environment is considered hazardous to spacecraft, resulting
  in materials degradation. Understanding the degradation of space-based
  instruments is crucial in order to achieve the scientific objectives,
  which are derived from these instruments. This paper discusses
  the on-orbit performance degradation of recent spacebased solar
  instruments. We will focus on the instruments of three space-based
  missions such as the Project for On-Board Autonomy 2 (PROBA2)
  spacecraft, the Solar Monitoring Observatory (SOLAR) payload onboard the
  Columbus science Laboratory of the International Space Station (ISS)
  and the PICARD spacecraft. Finally, this paper intends to understand
  the degradation processes of these space-based solar instruments.

---------------------------------------------------------
Title: VizieR Online Data Catalog: SOLAR/SOLSPEC UV SSI from 2008-2015
    (Meftah+, 2016)
Authors: Meftah, M.; Bolsee, D.; Dame, L.; Hauchecorne, A.; Pereira,
   N.; Irbah, A.; Bekki, S.; Cessateur, G.; Foujols, T.; Thieblemont, R.
2017yCatp058029101M    Altcode:
  The SOLar SPECtrum (SOLSPEC) instrument of the Solar Monitoring
  Observatory (SOLAR) was exposed to sunlight for the first time on
  April 5, 2008. The duration to record a solar spectrum (165-3088nm)
  is less than 17 minutes. Between April 2008 and May 2016, more
  than 700 solar spectra were acquired. <P />The present article is
  dedicated to the UV portion (165-400nm) of the solar spectrum and
  its temporal variations during Solar Cycle 24. Measurements from two
  separated double-spectrometers of SOLAR/SOLSPEC ('UV' and 'VIS') are
  combined. From these data, we obtained the UV solar spectrum above
  Earth's atmosphere at a distance of one astronomical unit (initial
  values for studying the UV solar variability). <P />(1 data file).

---------------------------------------------------------
Title: SOLAR/SOLSPEC mission on ISS: In-flight performance for SSI
    measurements in the UV
Authors: Bolsée, D.; Pereira, N.; Gillotay, D.; Pandey, P.; Cessateur,
   G.; Foujols, T.; Bekki, S.; Hauchecorne, A.; Meftah, M.; Damé, L.;
   Hersé, M.; Michel, A.; Jacobs, C.; Sela, A.
2017A&A...600A..21B    Altcode:
  Context. The SOLar SPECtrum (SOLSPEC) experiment is part of the
  Solar Monitoring Observatory (SOLAR) payload, and has been externally
  mounted on the Columbus module of the International Space Station (ISS)
  since 2008. SOLAR/SOLSPEC combines three absolutely calibrated double
  monochromators with concave gratings for measuring the solar spectral
  irradiance (SSI) from 166 nm to 3088 nm. This physical quantity is a
  key input for studies of climatology, planetary atmospheres, and solar
  physics. <BR /> Aims: A general description of the instrument is given,
  including in-flight operations and performance of the ultraviolet
  (UV) channel from 175 nm to 340 nm. <BR /> Methods: We developed a
  range of processing and correction methods, which are described in
  detail. For example, methods for correcting thermal behavior effects,
  instrument linearity, and especially the accuracy of the wavelength
  and absolute radiometric scales have been validated by modeling the
  standard uncertainties. <BR /> Results: The deliverable is a quiet Sun
  UV reference solar spectrum as measured by SOLAR/SOLSPEC during the
  minimum of solar activity prior to cycle 24. Comparisons with other
  instruments measuring SSI are also presented. <P />The quiet Sun UV
  spectrum (FITS file) is only available at the CDS via anonymous ftp to
  <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
  (<A href="http://130.79.128.5">http://130.79.128.5</A>) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/600/A21">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/600/A21</A>

---------------------------------------------------------
Title: A new solar reference spectrum from 165 to 3088 nm
Authors: Damé, Luc; Meftah, Mustapha; Bolsée, David; Pereira, Nuno;
   Bekki, Slimane; Hauchecorne, Alain; Irbah, Abdenour; Cessateur, Gaël;
   Sluse, Dominique
2017EGUGA..1913906D    Altcode:
  Since April 5, 2008 and until February 15, 2017 the SOLAR/SOLSPEC
  spectro-radiometer on the International Space Station performed
  accurate measurements of Solar Spectral Irradiance (SSI) from the far
  ultraviolet to the infrared (165 nm to 3088 nm). These measurements
  are of primary importance for a better understanding of solar physics
  and of the impact of solar variability on climate (via Earth's
  atmospheric photochemistry). In particular, a new reference solar
  spectrum is established covering most of the unusual solar cycle
  24 from minimum in 2008 to maximum. Temporal variability in the UV
  (165 to 400 nm) is presented in several wavelengths bands. These
  results are possible thanks to revised engineering corrections,
  improved calibrations and new procedures to account for thermal and
  aging advanced corrections. Uncertainties on these measurements are
  evaluated and compare favorably with other instruments.

---------------------------------------------------------
Title: 8 years of Solar Spectral Irradiance Observations from the
    ISS with the SOLAR/SOLSPEC Instrument
Authors: Damé, L.; Bolsée, D.; Meftah, M.; Irbah, A.; Hauchecorne,
   A.; Bekki, S.; Pereira, N.; Cessateur, G.; Marchand, M.; Thiéblemont,
   R.; Foujols, T.
2016AGUFMSA51B2426D    Altcode:
  Accurate measurements of Solar Spectral Irradiance (SSI) are of
  primary importance for a better understanding of solar physics
  and of the impact of solar variability on climate (via Earth's
  atmospheric photochemistry). The acquisition of a top of atmosphere
  reference solar spectrum and of its temporal and spectral variability
  during the unusual solar cycle 24 is of prime interest for these
  studies. These measurements are performed since April 2008 with the
  SOLSPEC spectro-radiometer from the far ultraviolet to the infrared
  (166 nm to 3088 nm). This instrument, developed under a fruitful
  LATMOS/BIRA-IASB collaboration, is part of the Solar Monitoring
  Observatory (SOLAR) payload, externally mounted on the Columbus module
  of the International Space Station (ISS). The SOLAR mission, with its
  actual 8 years duration, will cover almost the entire solar cycle 24. We
  present here the in-flight operations and performances of the SOLSPEC
  instrument, including the engineering corrections, calibrations and
  improved know-how procedure for aging corrections. Accordingly, a SSI
  reference spectrum from the UV to the NIR will be presented, together
  with its UV variability, as measured by SOLAR/SOLSPEC. Uncertainties
  on these measurements and comparisons with other instruments will be
  briefly discussed.

---------------------------------------------------------
Title: A new solar reference spectrum obtained with the SOLAR/SOLSPEC
    space-based spectro-radiometer
Authors: Meftah, M.; Bolsée, D.; Hauchecorne, A.; Damé, L.; Bekki,
   S.; Pereira, N.
2016AGUFMSH31B2554M    Altcode:
  The solar spectrum is a key input for different disciplines such as
  Solar Physics and Climate Physics. Based on SOLAR/SOLSPEC data, we
  will present a new solar irradiance spectrum from 165 to 3088 nm. The
  methodology for obtaining these results will be described. Finally,
  this new solar reference spectrum will be compared with other solar
  irradiance reference spectra (ATLAS 3 and WHI 2008).

---------------------------------------------------------
Title: Solar Irradiance from 165 to 400 nm in 2008 and UV Variations
    in Three Spectral Bands During Solar Cycle 24
Authors: Meftah, M.; Bolsée, D.; Damé, L.; Hauchecorne, A.; Pereira,
   N.; Irbah, A.; Bekki, S.; Cessateur, G.; Foujols, T.; Thiéblemont, R.
2016SoPh..291.3527M    Altcode: 2016SoPh..tmp..162M
  Accurate measurements of the solar spectral irradiance (SSI) and
  its temporal variations are of primary interest to better understand
  solar mechanisms, and the links between solar variability and Earth's
  atmosphere and climate. The SOLar SPECtrum (SOLSPEC) instrument of the
  Solar Monitoring Observatory (SOLAR) payload onboard the International
  Space Station (ISS) has been built to carry out SSI measurements from
  165 to 3088 nm. We focus here on the ultraviolet (UV) part of the
  measured solar spectrum (wavelengths less than 400 nm) because the
  UV part is potentially important for understanding the solar forcing
  of Earth's atmosphere and climate. We present here SOLAR/SOLSPEC UV
  data obtained since 2008, and their variations in three spectral bands
  during Solar Cycle 24. They are compared with previously reported UV
  measurements and model reconstructions, and differences are discussed.

---------------------------------------------------------
Title: VizieR Online Data Catalog: Sun UV spectrum
    (06/06/2008-26/04/2009) (Bolsee+, 2017)
Authors: Bolsee, D.; Pereira, N.; Gillotay, D.; Pandey, P.; Cessateur,
   G.; Foujols, T.; Bekki, S.; Hauchecorne, A.; Meftah, M.; Dame, L.;
   Herse, M.; Michel, A.; Jacobs, C.; Sela, A.
2016yCat..36000021B    Altcode:
  This file provides the data of the Figure 12 of the paper. It is
  the average spectral irradiance of the Sun as measured by the space
  instrument SOLAR/SOLSPEC on ISS during the minimum of solar activity
  prior to cycle 24. Spectral range: 175nm-340nm by step of 0.5nm. Time
  interval for averaging: 6th June 2008 - 26th April 2009. <P />(1
  data file).

---------------------------------------------------------
Title: Variations in the Geometry of the Sun Observed with HMI/SDO
    during Cycle 24
Authors: Irbah, Abdenour; Damé, Luc
2016usc..confE.128I    Altcode:
  Geometry of the Sun and its temporal variations observed with
  ground-based instruments are still subject to questioning. The geometry,
  which inform us on the interior of the Sun, is achieved by high
  resolution measurements of the radius, oblateness and gravitational
  moments c2 and c4. Several space missions were developed these last
  decades to validate or refute its observed variations with ground
  experiments and the link with solar activity. High angular resolution
  of solar radius measurements and its long term trend is however a
  challenge in Space. The first attempts with MDI (Soho) then SODISM
  (PICARD) and HMI (SDO) revealed the difficulties of such measures
  due to hostile environment which introduces thermal variations of
  the instruments along the satellite orbit. These variations have
  non negligible impacts on optical properties of onboard telescopes
  and therefore on images and parameters extracted, such as the solar
  radius. We need to take into account the thermal behavior (housekeeping
  data) recorded together with the science data to correct them. Solar
  oblateness and gravitational moments ask for both special spacecraft
  operations and appropriate processing methods to obtain the needed
  accuracy for their measurements. We present here some results on the
  solar radius and oblateness obtained with HMI data. Images analysed
  cover six years since May 1, 2010 (beginning of Cycle 24), until
  now. Results show that the geometry of the Sun presents some temporal
  variations related to solar activity. In particular we evidence a
  Quasi-Biennale Oscillation (QBO) correlated with the solar cycle,
  as was observed with ground observations.

---------------------------------------------------------
Title: 8 years of Solar Spectral Irradiance Variability Observed
    from the ISS with the SOLAR/SOLSPEC Instrument
Authors: Damé, Luc; Bolsée, David; Meftah, Mustapha; Irbah, Abdenour;
   Hauchecorne, Alain; Bekki, Slimane; Pereira, Nuno; Cessateur, Marchand;
   Gäel; , Marion; et al.
2016usc..confE.129D    Altcode:
  Accurate measurements of Solar Spectral Irradiance (SSI) are of
  primary importance for a better understanding of solar physics
  and of the impact of solar variability on climate (via Earth's
  atmospheric photochemistry). The acquisition of a top of atmosphere
  reference solar spectrum and of its temporal and spectral variability
  during the unusual solar cycle 24 is of prime interest for these
  studies. These measurements are performed since April 2008 with the
  SOLSPEC spectro-radiometer from the far ultraviolet to the infrared
  (166 nm to 3088 nm). This instrument, developed under a fruitful
  LATMOS/BIRA-IASB collaboration, is part of the Solar Monitoring
  Observatory (SOLAR) payload, externally mounted on the Columbus module
  of the International Space Station (ISS). The SOLAR mission, with
  its actual 8 years duration, will cover almost the entire solar cycle
  24. We present here the in-flight operations and performances of the
  SOLSPEC instrument, including the engineering corrections, calibrations
  and improved know-how procedure for aging corrections. Accordingly,
  a SSI reference spectrum from the UV to the NIR will be presented,
  together with its variability in the UV, as measured by SOLAR/SOLSPEC
  for 8 years. Uncertainties on these measurements and comparisons with
  other instruments will be briefly discussed.

---------------------------------------------------------
Title: Future space missions and ground observatory for measurements
    of coronal magnetic fields
Authors: Fineschi, Silvano; Gibson, Sarah; Bemporad, Alessandro;
   Zhukov, Andrei; Damé, Luc; Susino, Roberto; Larruquert, Juan
2016cosp...41E.602F    Altcode:
  This presentation gives an overview of the near-future perspectives for
  probing coronal magnetism from space missions (i.e., SCORE and ASPIICS)
  and ground-based observatory (ESCAPE). Spectro-polarimetric imaging of
  coronal emission-lines in the visible-light wavelength-band provides an
  important diagnostics tool of the coronal magnetism. The interpretation
  in terms of Hanle and Zeeman effect of the line-polarization
  in forbidden emission-lines yields information on the direction
  and strength of the coronal magnetic field. As study case, this
  presentation will describe the Torino Coronal Magnetograph (CorMag)
  for the spectro-polarimetric observation of the FeXIV, 530.3 nm,
  forbidden emission-line. CorMag - consisting of a Liquid Crystal (LC)
  Lyot filter and a LC linear polarimeter. The CorMag filter is part
  of the ESCAPE experiment to be based at the French-Italian Concordia
  base in Antarctica. The linear polarization by resonance scattering
  of coronal permitted line-emission in the ultraviolet (UV)can be
  modified by magnetic fields through the Hanle effect. Space-based
  UV spectro-polarimeters would provide an additional tool for the
  disgnostics of coronal magnetism. As a case study of space-borne UV
  spectro-polarimeters, this presentation will describe the future upgrade
  of the Sounding-rocket Coronagraphic Experiment (SCORE) to include new
  generation, high-efficiency UV polarizer with the capability of imaging
  polarimetry of the HI Lyman-α, 121.6 nm. SCORE is a multi-wavelength
  imager for the emission-lines, HeII 30.4 nm and HI 121.6 nm, and
  visible-light broad-band emission of the polarized K-corona. SCORE
  has flown successfully in 2009. The second lauch is scheduled in
  2016. Proba-3 is the other future solar mission that would provide
  the opportunity of diagnosing the coronal magnetic field. Proba-3 is
  the first precision formation-flying mission to launched in 2019). A
  pair of satellites will fly together maintaining a fixed configuration
  as a 'large rigid structure' in space. The paired satellites will
  together form a 150-m long solar coronagraph (ASPIICS) to study the
  Sun's faint corona closer to the solar limb than has ever before been
  achieved. High-resolution imaging in polarized visible-light of shock
  waves generated by Coronal Mass Ejections would provide a diagnostics
  of the magnetic field in the pre-shock ambient corona.

---------------------------------------------------------
Title: SOLAR/SOLSPEC ultraviolet solar spectral irradiance variability
    since 2008
Authors: Damé, Luc; Bolsee, David; Hauchecorne, Alain; Meftah,
   Mustapha; Bekki, Slimane; Pereira, Nuno
2016cosp...41E.398D    Altcode:
  The SOLAR/SOLSPEC experiment measures the Solar Spectral Irradiance
  (SSI) from the Space Station since April 2008. Measurements are carried
  between 166 nm and 3088 nm by three double-monochromators. SSI,
  particularly in the ultraviolet, is a key input to determine the
  dynamics and coupling of Earth's atmosphere in response to solar
  and terrestrial inputs. In-flight operations and performances of the
  instrument, including corrections, will be presented for the 8 years
  of the mission. After an accurate calibration following recent special
  on-orbit new operations, we present the variability measured in the UV
  by SOLAR/SOLSPEC. The accuracy of these measurements will be discussed.

---------------------------------------------------------
Title: Main results of the PICARD mission
Authors: Meftah, M.; Corbard, T.; Hauchecorne, A.; Irbah, A.; Boumier,
   P.; Chevalier, A.; Schmutz, W.; Ikhlef, R.; Morand, F.; Renaud, C.;
   Hochedez, J. -F.; Cessateur, G.; Turck-Chièze, S.; Salabert, D.;
   Rouzé, M.; van Ruymbeke, M.; Zhu, P.; Kholikov, S.; Koller, S.;
   Conscience, C.; Dewitte, S.; Damé, L.; Djafer, D.
2016SPIE.9904E..0ZM    Altcode:
  PICARD is a mission devoted to solar variability observations through
  imagery and radiometric measurements. The main goal is to provide data
  for scientific investigation first in the area of solar physics, and
  second in the assessment of the influence of the solar variability on
  the Earth climate variability. PICARD contains a double program with
  in-space and on-ground measurements. The PICARD spacecraft was launched
  on June 15, 2010, commissioned in-flight in October of the same year
  and was retired in April 2014. The PICARD ground-based observatory is
  operational since May 2011. We shall give a short overview of the PICARD
  instrumentation. New estimates of the absolute values of the total solar
  irradiance, of the solar spectral irradiance at typical wavelengths,
  and of the solar oblateness will be given. We will also report about
  helioseismic studies. Finally, we will present our current results
  about solar radius variations after six years of solar observation.

---------------------------------------------------------
Title: How mission requirements affect observations: case of the
    PICARD mission
Authors: Irbah, A.; Meftah, M.; Hauchecorne, A.; Damé, L.; Djafer, D.
2016SPIE.9904E..4GI    Altcode:
  The scientific objectives of a space mission result into instrumental
  developments and specific satellite operations to observe astronomical
  objects of interest. The payload in its space environment is however
  subject to important thermal variations that affect observations. This
  is well observed when images of the Sun are recorded with the constraint
  of keeping the solar rotational axis in a constant direction relatively
  to the camera reference frame. Consequences are clearly observed
  on image positions that follow the thermal variations induced by
  the satellite orbit. This is, in particular, the case for the space
  mission PICARD. This phenomenon is similar to defocus and motions of
  images recorded with ground-based telescopes. We first present some
  simulations showing these effects. We then compare our results with
  real data obtained from the space mission PICARD.

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Title: Solar seeing monitor MISOLFA: A new method for estimating
    atmospheric turbulence parameters
Authors: Irbah, A.; Borgnino, J.; Djafer, D.; Damé, L.; Keckhut, P.
2016A&A...591A.150I    Altcode:
  <BR /> Aims: Daily observation conditions are needed when observing the
  Sun at high angular resolution. MISOLFA is a daytime seeing monitor
  developed for this purpose that allows the estimation of the spatial
  and temporal parameters of atmospheric turbulence. This information
  is necessary, for instance, for astrometric measurements of the
  solar radius performed at Calern Observatory (France) with SODISM
  II, the ground-based version of the SODISM instrument of the PICARD
  mission. <BR /> Methods: We present a new way to estimate the spatial
  parameters of atmospheric turbulence for daily observations. This
  method is less sensitive to vibrations and guiding defaults of the
  telescope since it uses short-exposure images. It is based on the
  comparison of the optical transfer function obtained from solar data
  and the theoretical values deduced from the Kolmogorov and Von Kàrmàn
  models. This method, previously tested on simulated solar images, is
  applied to real data recorded at Calern Observatory in July 2013 with
  the MISOLFA monitor. <BR /> Results: First, we use data recorded in the
  pupil plane mode of MISOLFA and evaluate the turbulence characteristic
  times of angle-of-arrival fluctuations: between 5 and 16 ms. Second,
  we use the focal plane mode of MISOLFA to simultaneously record solar
  images to obtain isoplanatic angles: ranging from 1 to 5 arcsec (in
  agreement with previously published values). These images and our
  new method allow Fried's parameter to be measured; it ranges from 0.5
  cm to 4.7 cm with a mean value of 1.5 cm when Kolmogorov's model is
  considered, and from less than 0.5 to 2.6 cm with a mean value of 1.3
  cm for the Von Kàrmàn model. Measurements of the spatial coherence
  outer scale parameter are also obtained when using the Von Kàrmàn
  model; it ranges from 0.25 to 13 m with a mean value of 3.4 m for the
  four days of observation that we analyzed. We found that its value
  can undergo large variations in only a few hours and that more data
  analysis is needed to better define its statistics.

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Title: HiRISE/NEOCE: an ESA M5 formation flying proposed mission
    combining high resolution and coronagraphy for ultimate observations
    of the chromosphere, corona and interface
Authors: Damé, Luc; Von Fay-Siebenburgen Erdélyi, Robert
2016cosp...41E.397D    Altcode:
  The global understanding of the solar environment through the magnetic
  field emergence and dissipation, and its influence on Earth, is at
  the centre of the four major thematics addressed by HiRISE/NEOCE (High
  Resolution Imaging and Spectroscopy Explorer/New Externally Occulted
  Coronagraph Experiment). They are interlinked and also complementary:
  the internal structure of the Sun determines the surface activity
  and dynamics that trigger magnetic field structuring which evolution,
  variation and dissipation will, in turn, explain the coronal heating
  onset and the major energy releases that feed the influence of the Sun
  on Earth. The 4 major themes of HiRISE/NEOCE are: - fine structure of
  the chromosphere-corona interface by 2D spectroscopy in FUV at very
  high resolution; - coronal heating roots in inner corona by ultimate
  externally-occulted coronagraphy; - resolved and global helioseismology
  thanks to continuity and stability of observing at L1 Lagrange point;
  - solar variability and space climate with a global comprehensive view
  of UV variability as well. Recent missions have shown the definite
  role of waves and of the magnetic field deep in the inner corona, at
  the chromosphere-corona interface, where dramatic changes occur. The
  dynamics of the chromosphere and corona is controlled by the emerging
  magnetic field, guided by the coronal magnetic field. Accordingly,
  the direct measurement of the chromospheric and coronal magnetic
  fields is of prime importance. This is implemented in HiRISE/NEOCE,
  to be proposed for ESA M5 ideally placed at the L1 Lagrangian point,
  providing FUV imaging and spectro-imaging, EUV and XUV imaging and
  spectroscopy, and ultimate coronagraphy by a remote external occulter
  (two satellites in formation flying 375 m apart minimizing scattered
  light) allowing to characterize temperature, densities and velocities
  up to the solar upper chromosphere, transition zone and inner
  corona with, in particular, 2D very high resolution multi-spectral
  imaging-spectroscopy and direct coronal magnetic field measurement:
  a unique set of tools to understand the structuration and onset of
  coronal heating. We give a detailed account of the major scientific
  objectives, and present the ESA M5 proposed mission profile and model
  payload (in particular of the SuperASPIICS package of visible, NIR
  and UV, Lyman-Alpha and OVI, coronagraphs).

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Title: SUITS/SWUSV: a small-size mission to address solar spectral
    variability, space weather and solar-climate relations
Authors: Damé, Luc; Keckhut, Philippe; Hauchecorne, Alain; Meftah,
   Mustapha; Bekki, Slimane
2016cosp...41E.396D    Altcode:
  We present the SUITS/SWUSV microsatellite mission investigation:
  "Solar Ultraviolet Influence on Troposphere/Stratosphere, a Space
  Weather &amp; Ultraviolet Solar Variability" mission. SUITS/SWUSV was
  developed to determine the origins of the Sun's activity, understand the
  flaring process (high energy flare characterization) and onset of CMEs
  (forecasting). Another major objective is to determine the dynamics and
  coupling of Earth's atmosphere and its response to solar variability
  (in particular UV) and terrestrial inputs. It therefore includes the
  prediction and detection of major eruptions and coronal mass ejections
  (Lyman-Alpha and Herzberg continuum imaging) the solar forcing on
  the climate through radiation and their interactions with the local
  stratosphere (UV spectral irradiance measures from 170 to 400 nm). The
  mission is proposed on a sun-synchronous polar orbit 18h-6h (for
  almost constant observing) and proposes a 7 instruments model payload
  of 65 kg - 65 W with: SUAVE (Solar Ultraviolet Advanced Variability
  Experiment), an optimized telescope for FUV (Lyman-Alpha) and MUV
  (200-220 nm Herzberg continuum) imaging (sources of variability);
  SOLSIM (Solar Spectral Irradiance Monitor), a spectrometer with 0.65
  nm spectral resolution from 170 to 340 nm; SUPR (Solar Ultraviolet
  Passband Radiometers), with UV filter radiometers at Lyman-Alpha,
  Herzberg, MgII index, CN bandhead and UV bands coverage up to 400 nm;
  HEBS (High Energy Burst Spectrometers), a large energy coverage (a few
  tens of keV to a few hundreds of MeV) instrument to characterize large
  flares; EPT-HET (Electron-Proton Telescope - High Energy Telescope),
  measuring electrons, protons, and heavy ions over a large energy
  range; ERBO (Earth Radiative Budget and Ozone) NADIR oriented; and a
  vector magnetometer. Complete accommodation of the payload has been
  performed on a PROBA type platform very nicely. Heritage is important
  both for instruments (SODISM and PREMOS on PICARD, LYRA on PROBA-2,
  SOLSPEC on ISS,...) and platform (PROBA-2, PROBA-V,...), leading to
  high TRL levels (&gt;7). SUITS/SWUSV was initially designed in view of
  the ESA/CAS AO for a Small Mission; it is now envisaged for a joint
  CNES/NASA opportunity with Europeans and Americans partners for a
  possible flight in 2021.

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Title: The future of solar spectral irradiance in the ultraviolet
    with the SOLSIM double-monochromator
Authors: Damé, Luc; Bolsee, David; Rouanet, Nicolas; Gilbert, Pierre
2016cosp...41E.399D    Altcode:
  Solar Spectral Irradiance (SSI) in the UV, and its variability, are of
  prime importance to quantify the solar forcing on the climate through
  radiation and their interactions with the local stratosphere, noticeably
  through the "top-down" mechanism amplifying UV solar forcing on the
  climate (UV affects stratospheric dynamics and temperatures, altering
  interplanetary waves and weather patterns both poleward and downward to
  the lower stratosphere and tropopause regions). SOLSIM (Solar Spectral
  Irradiance Monitor) is a newly designed double-monochromator instrument
  covering the 170 - 340 nm ultraviolet spectral range. It is an enhanced
  and optimized version of the previously flown SOLSPEC instrument
  externally mounted on the Columbus module of the International Space
  Station. While SOLSPEC had 3 double-monochromators to cover the UV to
  the IR, the SOLSIM spectrometer is covering only the UV but with an
  almost constant 0.65 nm spectral resolution from 170 to 340 nm. To
  avoid thermal issues with the instrument, a sun-synchronous polar
  orbit 18h-6h (for almost constant observing) is preferred to the Space
  Station (SOLSIM is part of the model payload of the SUITS/SWUSV proposed
  mission). Characteristics, performances and calibrations foreseen for
  this new generation SSI instrument will be presented.

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Title: The Measurement of the Solar Spectral Irradiance Variability
    during the Solar Cycle 24 using SOLAR/SOLSPEC on ISS
Authors: Bolsée, David; Pereira, Nuno; Pandey, Praveen; Cessateur,
   Gaël; Gillotay, Didier; Foujols, Thomas; Hauchecorne, Alain; Bekki,
   Slimane; Marchand, Marion; Damé, Luc; Meftah, Mustapha; Bureau,
   Jerôme
2016EGUGA..18.8103B    Altcode:
  Since April 2008, SOLAR/SOLSPEC measures the Solar Spectral Irradiance
  (SSI) from 166 nm to 3088 nm. The instrument is a part of the Solar
  Monitoring Observatory (SOLAR) payload, externally mounted on the
  Columbus module of the International Space Station. As the SSI is a key
  input for the validation of solar physics models, together with playing
  a role in the climate system and photochemistry of the Earth atmosphere,
  SOLAR/SOLSPEC spectral measurements becomes important. In this study,
  the in-flight operations and performances of the instrument -including
  the engineering corrections- will be presented for seven years of the
  SOLAR mission. Following an accurate absolute calibration, the SSI
  variability in the UV as measured by SOLAR/SOLSPEC in the course of the
  solar cycle 24 will be presented and compared to other instruments. The
  accuracy of these measurements will be also discussed here.

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Title: Solar Spectral Irradiance at 782 nm as Measured by the SES
    Sensor Onboard Picard
Authors: Meftah, M.; Hauchecorne, A.; Irbah, A.; Cessateur, G.; Bekki,
   S.; Damé, L.; Bolsée, D.; Pereira, N.
2016SoPh..291.1043M    Altcode: 2016SoPh..tmp...53M
  Picard is a satellite dedicated to the simultaneous measurement
  of the total and solar spectral irradiance, the solar diameter,
  the solar shape, and to the Sun's interior through the methods of
  helioseismology. The satellite was launched on June 15, 2010, and
  pursued its data acquisitions until March 2014. A Sun Ecartometry Sensor
  (SES) was developed to provide the stringent pointing requirements
  of the satellite. The SES sensor produced an image of the Sun at
  782 ±2.5 nm. From the SES data, we obtained a new time series of
  the solar spectral irradiance at 782 nm from 2010 to 2014. During
  this period of Solar Cycle 24, the amplitude of the changes has
  been of the order of ± 0.08 %, corresponding to a range of about 2
  ×10<SUP>−3</SUP>Wm−<SUP>2</SUP>nm−<SUP>1</SUP>. SES observations
  provided a qualitatively consistent evolution of the solar spectral
  irradiance variability at 782 nm. SES data show similar amplitude
  variations with the semi-empirical model Spectral And Total Irradiance
  REconstruction for the Satellite era (SATIRE-S), whereas the Spectral
  Irradiance Monitor instrument (SIM) onboard the SOlar Radiation and
  Climate Experiment satellite (SORCE) highlights higher amplitudes.

---------------------------------------------------------
Title: Solar radius measurements with the space instrument HMI (SDO)
Authors: Irbah, Abdanour; Hauchecorne, Alain; Meftah, Mustapha; Damé,
   Luc; Keckhut, Philippe
2016EGUGA..18.6886I    Altcode:
  The solar radius variations and its effects on the Earth climate are
  still a long scientific debate. The observed variations from ground
  experiments were not totally admitted and several space missions
  have had these measures as a goal. The high angular resolution of
  radius measurements and its long-term trend is however a challenge in
  space. The first attempts with MDI (Soho) then SODISM (PICARD) and HMI
  (SDO) revealed the difficulties of such measures due to the hostile
  environment which introduces thermal variations on the instruments all
  along the satellite orbit. These variations have non-negligible impacts
  on the optical properties of the onboard telescopes and therefore on
  the images and the parameters which are extracted such as the solar
  radius. We need then to make a posteriori corrections using the thermal
  housekeeping's recorded together with the data science. We present here
  how we make such correction on the solar radius obtained from the HMI
  images. We will then compare and discuss the results with the solar
  radius recorded at 607 nm with the ground-based instrument of PICARD.

---------------------------------------------------------
Title: SUITS/SWUSV: a Solar-Terrestrial Space Weather &amp; Climate
    Mission
Authors: Damé, Luc; Hauchecorne, Alain
2016EGUGA..1816581D    Altcode:
  The SUITS/SWUSV (Solar Ultraviolet Influence on
  Troposphere/Stratosphere, a Space Weather &amp; Ultraviolet Solar
  Variability mission) microsatellite mission is developed on one hand
  to determine the origins of the Sun's activity, understand the flaring
  process (high energy flare characterization) and onset (forecasting) of
  Coronal Mass Ejections (CMEs) and, on the other hand, to determine the
  dynamics and coupling of Earth's atmosphere and its response to solar
  variability (in particular UV) and terrestrial inputs. It therefore
  includes the prediction and detection of major eruptions and CMEs
  (Lyman-Alpha and Herzberg continuum imaging 200-220 nm), the solar
  forcing on the climate through radiation, and their interactions
  with the local stratosphere (UV spectral irradiance 170-400 nm and
  ozone measurements). SUITS/SWUSV includes a 8 instruments model
  payload with, in particular for Space Weather and Climate, SUAVE
  (Solar Ultraviolet Advanced Variability Experiment), an optimized
  telescope for FUV (Lyman-Alpha) and MUV (Herzberg continuum) imaging
  (sources of variability), SOLSIM (Solar Spectral Irradiance Monitor),
  a spectrometer with 0.65 nm spectral resolution from 170 to 340 nm, SUPR
  (Solar Ultraviolet Passband Radiometers), with UV filter radiometers
  at Lyman-Alpha, Herzberg, MgII, CN bandhead and UV bands coverage up to
  400 nm, and ERBO (Earth Radiative Budget and Ozone), NADIR oriented to
  measure ozone (6 bands) and 0.1-100 μm ERB. Example of accommodation
  of the payload has been performed on a new PROBA type platform very
  nicely by Qinetic. Heritage is important both for instruments and
  platform leading to high TRL levels. SUITS/SWUSV is designed in view
  of ESA Small Mission Calls and other possible CNES/NASA opportunities
  in the near future (Heliophysics, Earth Observation, etc.).

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Title: Ground-based measurements of the solar diameter during the
    rising phase of solar cycle 24
Authors: Meftah, M.; Corbard, T.; Irbah, A.; Ikhlef, R.; Morand, F.;
   Renaud, C.; Hauchecorne, A.; Assus, P.; Borgnino, J.; Chauvineau, B.;
   Crepel, M.; Dalaudier, F.; Damé, L.; Djafer, D.; Fodil, M.; Lesueur,
   P.; Poiet, G.; Rouzé, M.; Sarkissian, A.; Ziad, A.; Laclare, F.
2014A&A...569A..60M    Altcode:
  Context. For the past thirty years, modern ground-based time-series of
  the solar radius have shown different apparent variations according to
  different instruments. The origins of these variations may result from
  the observer, the instrument, the atmosphere, or the Sun. Solar radius
  measurements have been made for a very long time and in different
  ways. Yet we see inconsistencies in the measurements. Numerous
  studies of solar radius variation appear in the literature, but
  with conflicting results. These measurement differences are certainly
  related to instrumental effects or atmospheric effects. Use of different
  methods (determination of the solar radius), instruments, and effects
  of Earth's atmosphere could explain the lack of consistency on the
  past measurements. A survey of the solar radius has been initiated
  in 1975 by Francis Laclare, at the Calern site of the Observatoire
  de la Côte d'Azur (OCA). Several efforts are currently made from
  space missions to obtain accurate solar astrometric measurements,
  for example, to probe the long-term variations of solar radius, their
  link with solar irradiance variations, and their influence on the
  Earth climate. <BR /> Aims: The Picard program includes a ground-based
  observatory consisting of different instruments based at the Calern site
  (OCA, France). This set of instruments has been named "Picard Sol" and
  consists of a Ritchey-Chrétien telescope providing full-disk images
  of the Sun in five narrow-wavelength bandpasses (centered on 393.37,
  535.7, 607.1, 782.2, and 1025.0 nm), a Sun-photometer that measures the
  properties of atmospheric aerosol, a pyranometer for estimating a global
  sky-quality index, a wide-field camera that detects the location of
  clouds, and a generalized daytime seeing monitor allowing us to measure
  the spatio-temporal parameters of the local turbulence. Picard Sol is
  meant to perpetuate valuable historical series of the solar radius and
  to initiate new time-series, in particular during solar cycle 24. <BR />
  Methods: We defined the solar radius by the inflection-point position
  of the solar-limb profiles taken at different angular positions of the
  image. Our results were corrected for the effects of refraction and
  turbulence by numerical methods. <BR /> Results: From a dataset of more
  than 20 000 observations carried out between 2011 and 2013, we find a
  solar radius of 959.78 ± 0.19 arcsec (696 113 ± 138 km) at 535.7 nm
  after making all necessary corrections. For the other wavelengths in
  the solar continuum, we derive very similar results. The solar radius
  observed with the Solar Diameter Imager and Surface Mapper II during
  the period 2011-2013 shows variations shorter than 50 milli-arcsec
  that are out of phase with solar activity.

---------------------------------------------------------
Title: Thermal effects on solar images recorded in space
Authors: Irbah, A.; Meftah, M.; Hauchecorne, A.; Damé, L.; Bocquier,
   M.; Cissé, M.
2014SPIE.9143E..42I    Altcode:
  The Earth's atmosphere introduces a spatial frequency filtering in
  the object images recorded with ground-based instruments. A solution
  is to observe with telescopes onboard satellites to avoid atmospheric
  effects and to obtain diffraction limited images. However, similar
  atmosphere problems encountered with ground-based instruments may
  subsist in space when we observe the Sun since thermal gradients at
  the front of the instrument affect the observations. We present in
  this paper some simulations showing how solar images recorded in a
  telescope focal plane are directly impacted by thermal gradients in
  its pupil plane. We then compare the results with real solar images
  recorded with the PICARD mission in space.

---------------------------------------------------------
Title: SUAVE: a UV telescope for space weather and solar variability
    studies
Authors: Damé, L.; Meftah, M.; Irbah, A.; Hauchecorne, A.; Keckhut,
   P.; Quémerais, E.
2014SPIE.9144E..31D    Altcode:
  SUAVE (Solar Ultraviolet Advanced Variability Experiment) is a far
  ultraviolet (FUV) imaging solar telescope of novel design for ultimate
  thermal stability and long lasting performances. SUAVE is a 90 mm
  Ritchey- Chrétien telescope with SiC (Silicon Carbide) mirrors
  and no entrance window for long and uncompromised observations
  in the UV (no coatings of mirrors, flux limited to less than
  a solar constant on filters to avoid degradation), associated
  with an ultimate thermal control (heat evacuation, focus control,
  stabilization). Design of the telescope and early thermal modeling
  leading to a representative breadboard (a R and T program supported
  by CNES) will be presented. SUAVE is the main instrument of the SUITS
  (Solar Ultraviolet Influence on Troposphere/Stratosphere) microsatellite
  mission, a small-size mission proposed to CNES and ESA.

---------------------------------------------------------
Title: A nano-satellite to study the Sun and the Earth
Authors: Meftah, M.; Irbah, A.; Hauchecorne, A.; Damé, L.; Sarkissian,
   A.; Keckhut, P.; Lagage, P. -O.; Dewitte, S.; Chevalier, A.
2014SPIE.9085E..0YM    Altcode:
  Since the launch of the first artificial satellite in 1957, more than
  6,000 satellites have been sent into space. Despite technological
  advances, the space domain remains little accessible. However, with
  the miniaturization of electronic components, it has recently become
  possible to develop small satellites with which scientific goals can
  be addressed. Micro-satellites have demonstrated that these goals are
  achievable. However, completion times remain long. Today, we hope
  through the use of nano-satellites to reduce size, costs, time of
  development and accordingly to increase accessibility to space for
  scientific objectives. Nano-satellites have become important tools
  for space development and utilization, which may lead to new ways of
  space exploration. This paper is intended to present a future space
  mission enabled by the development of nano-satellites and the underlying
  technologies they employ. Our future mission expands observations of the
  Sun (total solar irradiance and solar spectral irradiance measurements)
  and of the Earth (outgoing long-wave radiation, short-wave radiation
  measurements and stratospheric ozone measurements). Constellations of
  nano-satellites providing simultaneous collection of data over a wide
  area of geo-space may be built later and present a great interest for
  Sun-Earth relationships.

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Title: Picard SODISM, a Space Telescope to Study the Sun from the
    Middle Ultraviolet to the Near Infrared
Authors: Meftah, M.; Hochedez, J. -F.; Irbah, A.; Hauchecorne, A.;
   Boumier, P.; Corbard, T.; Turck-Chièze, S.; Abbaki, S.; Assus,
   P.; Bertran, E.; Bourget, P.; Buisson, F.; Chaigneau, M.; Damé,
   L.; Djafer, D.; Dufour, C.; Etcheto, P.; Ferrero, P.; Hersé, M.;
   Marcovici, J. -P.; Meissonnier, M.; Morand, F.; Poiet, G.; Prado,
   J. -Y.; Renaud, C.; Rouanet, N.; Rouzé, M.; Salabert, D.; Vieau,
   A. -J.
2014SoPh..289.1043M    Altcode: 2013arXiv1303.0731M
  The Solar Diameter Imager and Surface Mapper (SODISM) onboard the
  Picard space mission provides wide-field images of the photosphere
  and chromosphere of the Sun in five narrow bandpasses centered at
  215.0, 393.37, 535.7, 607.1, and 782.2 nm. The Picard spacecraft
  was successfully launched on 15 June 2010 into a Sun-synchronous
  dawn-dusk orbit. The Picard space mission represents a European asset
  in collecting solar observations useful to improve Earth climatic
  models. The scientific payload consists of the SODISM imager and
  of two radiometers, SOlar VAriability Picard (SOVAP) and PREcision
  MOnitor Sensor (PREMOS), which measure the Total Solar Irradiance
  (TSI) and part of the Solar Spectral Irradiance (SSI).

---------------------------------------------------------
Title: NEOCE: a new external occulting coronagraph experiment for
    ultimate observations of the chromosphere, corona and interface
Authors: Damé, Luc; Fineschi, Silvano; Kuzin, Sergey; Von
   Fay-Siebenburgen, Erdélyi Robert
2014cosp...40E.617D    Altcode:
  Several ground facilities and space missions are currently dedicated
  to the study of the Sun at high resolution and of the solar corona
  in particular. However, and despite significant progress with the
  advent of space missions and UV, EUV and XUV direct observations
  of the hot chromosphere and million-degrees coronal plasma, much is
  yet to be achieved in the understanding of these high temperatures,
  fine dynamic dissipative structures and of the coronal heating in
  general. Recent missions have shown the definite role of a wide
  range of waves and of the magnetic field deep in the inner corona,
  at the chromosphere-corona interface, where dramatic and physically
  fundamental changes occur. The dynamics of the chromosphere and corona
  is controlled and governed by the emerging magnetic field. Accordingly,
  the direct measurement of the chromospheric and coronal magnetic fields
  is of prime importance. The solar corona consists of many localised
  loop-like structures or threads with the plasmas brightening and
  fading independently. The plasma evolution in each thread is believed
  to be related to the formation of filaments, each one being dynamic,
  in a non-equilibrium state. The mechanism sustaining this dynamics,
  oscillations or waves (Alfvén or other magneto-plasma waves),
  requires both very high-cadence, multi-spectral observations, and high
  resolution and coronal magnetometry. This is foreseen in the future
  Space Mission NEOCE (New External Occulting Coronagraph Experiment),
  the ultimate new generation high-resolution coronagraphic heliospheric
  mission, to be proposed for ESA M4. NEOCE, an evolution of the HiRISE
  mission, is ideally placed at the L5 Lagrangian point (for a better
  follow-up of CMEs), and provides FUV imaging and spectro-imaging,
  EUV and XUV imaging and spectroscopy, and ultimate coronagraphy by
  a remote external occulter (two satellites in formation flying 375 m
  apart minimizing scattered light) allowing to characterize temperature,
  densities and velocities up to the solar upper chromosphere, transition
  zone and inner corona with, in particular, 2D very high resolution
  multi-spectral imaging-spectroscopy and direct coronal magnetic field
  measurement: a unique set of tools to understand the structuration and
  onset of coronal heating. We give a detailed account of the proposed
  mission profile, and its major scientific objectives and model payload
  (in particular of the SuperASPIICS package of visible, NIR and UV,
  Lyman-Alpha and OVI, coronagraphs).

---------------------------------------------------------
Title: SWUSV: a microsatellite mission for space weather early
    forecasting of major flares and CMEs and the complete monitoring of
    the ultraviolet solar variability influence on climate
Authors: Damé, Luc
2014cosp...40E.614D    Altcode:
  The SWUSV (Space Weather &amp; Ultraviolet Solar Variability) proposed
  microsatellite mission encompasses three major scientific objectives:
  (1) Space Weather including the prediction and detection of major
  eruptions and coronal mass ejections (using Lyman-Alpha and Herzberg
  continuum imaging and H-Alpha ground support); (2) solar forcing on
  the climate through radiation and their interactions with the local
  stratosphere (UV spectral irradiance from 180 to 400 nm by bands of
  10 to 20 nm, including ozone, plus Lyman-Alpha and the CN bandhead);
  (3) simultaneous local radiative budget of the Earth, UV to IR,
  with an accuracy better than 1% in differential. The mission is on a
  sun-synchronous polar orbit and proposes 5 instruments to the model
  payload: SUAVE (Solar Ultraviolet Advanced Variability Experiment), an
  optimized telescope for FUV (Lyman-Alpha) and MUV (200-220 nm Herzberg
  continuum) imaging (sources of variability); UPR (Ultraviolet Passband
  Radiometers), with 64 UV filter radiometers; a vector magnetometer;
  thermal plasma measurements and Langmuir probes; and a total and
  spectral solar irradiance and Earth radiative budget ensemble (SERB,
  Solar irradiance &amp; Earth Radiative Budget). SWUSV is proposed as
  a small mission to CNES and to ESA for a possible flight as early
  as 2020-2021. With opening to Chinese collaboration (ESA-CAS Small
  Mission) a further instrument could be added (HEBS, High Energy Burst
  Spectrometers) to reinforced Space Weather flares prediction objectives.

---------------------------------------------------------
Title: SUMO: solar ultraviolet monitor and ozone nanosatellite for
    spectral irradiance, ozone and Earth radiative budget simultaneous
    evaluation
Authors: Damé, Luc
2014cosp...40E.615D    Altcode:
  SUMO is an innovative proof-of-concept nano-satellite which aims to
  measure on the same platform the different components of the Earth
  radiation budget, the solar energy input and the energy reemitted at the
  top of the Earth atmosphere, with a particular focus on the UV part of
  the spectrum and on the ozone layer, which are the most sensitive to
  the solar variability. The far UV (FUV) is the only wavelength band
  with energy absorbed in the high atmosphere (stratosphere), in the
  ozone (Herzberg continuum, 200-220 nm) and oxygen bands, and its high
  variability is most probably at the origin of a climate influence (UV
  affects stratospheric dynamics and temperatures, altering interplanetary
  waves and weather patterns both poleward and downward to the lower
  stratosphere and tropopause regions). Recent measurements at the time of
  the last solar minimum suggest that variations in the UV may be larger
  than previously assumed what implies a very different response in both
  stratospheric ozone and temperature. A simultaneous observation of
  the incoming FUV and of the ozone (O _{3}) production, would bring an
  invaluable information on this process of solar-climat forcing. Space
  instruments have already measured the different components of the Earth
  radiative budget but this is, to our knowledge, the first time that
  all instruments are operated on the same platform. This characteristic
  guarantees by itself obtaining original scientific results. SUMO is a
  10x10x30 cm (3) nanosatellite (“3U"), the payload occupying “1U",
  i.e. a cube of 10x10x10 cm (3) for 1 kg and 1 W of power. Orbit is
  polar since a further challenge in understanding the relation between
  solar UV variability and stratospheric ozone on arctic and antarctic
  regions. SUMO definition has been completed (platform and payload
  assembly integration and tests are possible in 24 months) and it is
  now intended to be proposed to CNES for a flight in 2017. Mission
  is expected to last up to 1 year. Follow-up is 2 fold: on one part
  a more complete set of measurements is possible by integrating SUMO
  miniaturized instruments on a larger satellite (e.g. on the SWUSV
  microsatellite mission for instance, the SERB package); on the other
  part it is particularly advantageous to increase the coverage in local
  time and latitude using a constellation of SUMO nanosatellites around
  the Earth.

---------------------------------------------------------
Title: The Space Weather &amp; Ultraviolet Solar Variability
    Microsatellite Mission (SWUSV)
Authors: Damé, Luc; Damé
2014IAUS..300..525D    Altcode:
  We present a summary of the scientific objectives, payload and mission
  profile of the Space Weather &amp; Ultraviolet Solar Variability
  Microsatellite Mission (SWUSV) proposed to CNES and ESA (small mission).

---------------------------------------------------------
Title: Segmentation of coronal features to understand the solar EUV
    and UV irradiance variability
Authors: Kumara, S. T.; Kariyappa, R.; Zender, J. J.; Giono, G.;
   Delouille, V.; Chitta, L. P.; Damé, L.; Hochedez, J. -F.; Verbeeck,
   C.; Mampaey, B.; Doddamani, V. H.
2014A&A...561A...9K    Altcode:
  Context. The study of solar irradiance variability is of great
  importance in heliophysics, the Earth's climate, and space weather
  applications. These studies require careful identifying, tracking
  and monitoring of active regions (ARs), coronal holes (CHs), and the
  quiet Sun (QS). <BR /> Aims: We studied the variability of solar
  irradiance for a period of two years (January 2011-December 2012)
  using the Large Yield Radiometer (LYRA), the Sun Watcher using APS and
  image Processing (SWAP) on board PROBA2, and the Atmospheric Imaging
  Assembly (AIA) on board the Solar Dynamics Observatory (SDO). <BR />
  Methods: We used the spatial possibilistic clustering algorithm (SPoCA)
  to identify and segment coronal features from the EUV observations of
  AIA. The AIA segmentation maps were then applied on SWAP images, and
  parameters such as the intensity, fractional area, and contribution
  of ARs/CHs/QS features were computed and compared with the full-disk
  integrated intensity and LYRA irradiance measurements. <BR /> Results:
  We report the results obtained from SDO/AIA and PROBA2/SWAP images
  taken from January 2011 to December 2012 and compare the resulting
  integrated full-disk intensity with PROBA2/LYRA irradiance. We
  determine the contributions of the segmented features to EUV and UV
  irradiance variations. The variations of the parameters resulting
  from the segmentation, namely the area, integrated intensity, and
  relative contribution to the solar irradiance, are compared with LYRA
  irradiance. We find that the active regions have a great impact on the
  irradiance fluctuations. In the EUV passbands considered in this study,
  the QS is the greatest contributor to the solar irradiance, with up
  to 63% of total intensity values. Active regions, on the other hand,
  contribute to about 10%, and off-limb structures to about 24%. We
  also find that the area of the features is highly variable suggesting
  that their area has to be taken into account in irradiance models,
  in addition to their intensity variations. <BR /> Conclusions:
  We successfully show that the feature extraction allows us to use
  EUV telescopes to measure irradiance fluctuations and to quantify
  the contribution of each part to the EUV spectral solar irradiance
  observed with a calibrated radiometer. This study also shows that
  SPoCA is viable, and that the segmentation of images can be a useful
  tool. We also provide the measurement correlation between SWAP and
  AIA during this analysis.

---------------------------------------------------------
Title: Extreme solar coronagraphy in Antarctica (ESCAPE) to support
    ASPIICS/PROBA-3 ESA program
Authors: Damé, Luc
2014cosp...40E.616D    Altcode:
  The coronal heating problem is still one of the most debated questions
  in solar physics. ESCAPE (the Extreme Solar Coronagraphy Antarctic
  Program Experiment) is designed to measure wave properties in corona
  and their possible contribution to the coronal heating and solar wind
  acceleration. It measures the polarization of coronal line emission,
  allowing to map the topology and dynamics of the magnetic field
  in corona. Furthermore, ESCAPE will be able of up to 3 months of
  continuous monitoring of the coronal activity, such as CMEs that are
  relevant for space weather studies. The Dome C high plateau is unique
  for coronagraphic observations: sky brightness is reduced, water vapour
  is low, seeing is excellent and continuity of observations on several
  weeks is possible. ESCAPE will perform 2-dimensional spectroscopy of
  the forbidden line of FeXIV at 530.285 nm, of FeXIII at 1074.7 nm
  and of the Sodium D3 line at 587 nm (precise line profile analysis
  will allow the diagnostic of the nature of waves by simultaneous
  measurements of velocities and intensities in the corona). ESCAPE is
  approved by CNRS/INSU with a test this summer at Pic du Midi and a first
  campaign planned at Dome C/Concordia in 2015/2016. Most subsystems
  are available thanks to the ESA STARTIGER R&amp;D program “Toward
  a New Generation of Formation Flying Coronagraph" performed in 2010
  in support of the ASPIICS ESA/PROBA-3 formation flying coronagraph
  mission. A Three Mirrors Anastigmat telescope and a 4 stages Liquid
  Crystal Tunable-filter Polarimeter have been developed and allow us
  to propose an automated Coronal Green Line full-field Polarimeter for
  unique observations (waves nature and intensity to address coronal
  heating) and with the best possible performances on Earth. No other
  ground site would allow such coronagraphic performances (the sky
  brightness is a factor 2 to 4 better than in Hawaii) and with high
  spatial resolution (better than an arcsec). ESCAPE will also help in
  validating the experimental approach of critical sub-systems of future
  space coronagraphy missions (e.g. the 587 nm filters of ASPIICS), bring
  ground simultaneous/complementary observations, and will open the way
  to future and more ambitious projects in Antarctica (e.g. AFSIIC)
  and in Space (e.g. HiRISE, NEOCE). ESCAPE is part of the SCAR/AAA
  research working group international effort.

---------------------------------------------------------
Title: Solar Activity Monitoring of Flares and CMEs Precursors
    through Lyman-Alpha Imaging and Tracking of Filaments and Prominences
Authors: Damé, Luc; Khaled, Safinaz A.
2014IAUS..300..523D    Altcode:
  We investigate the advantages of imaging solar filaments and prominences
  in Lyman-Alpha, coupled to H-Alpha on ground, to develop more reliable
  precursors indicators for large flares, several hours before their
  occurrence.

---------------------------------------------------------
Title: Special Issue on "Heliospheric Physics during and after a
    deep solar minimum"
Authors: Damé, Luc; Hady, A.
2013JAdR....4..205D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Space Weather and Ultraviolet Solar Variability (SWUSV)
    Microsatellite Mission
Authors: Damé, Luc
2013JAdR....4..235D    Altcode:
  We present the ambitions of the SWUSV (Space Weather and Ultraviolet
  Solar Variability) Microsatellite Mission that encompasses three major
  scientific objectives: (1) Space Weather including the prediction and
  detection of major eruptions and coronal mass ejections (Lyman-Alpha
  and Herzberg continuum imaging); (2) solar forcing on the climate
  through radiation and their interactions with the local stratosphere
  (UV spectral irradiance from 180 to 400 nm by bands of 20 nm,
  plus Lyman-Alpha and the CN bandhead); (3) simultaneous radiative
  budget of the Earth, UV to IR, with an accuracy better than 1% in
  differential. The paper briefly outlines the mission and describes
  the five proposed instruments of the model payload: SUAVE (Solar
  Ultraviolet Advanced Variability Experiment), an optimized telescope
  for FUV (Lyman-Alpha) and MUV (200-220 nm Herzberg continuum) imaging
  (sources of variability); UPR (Ultraviolet Passband Radiometers),
  with 64 UV filter radiometers; a vector magnetometer; thermal plasma
  measurements and Langmuir probes; and a total and spectral solar
  irradiance and Earth radiative budget ensemble (SERB, Solar irradiance
  &amp; Earth Radiative Budget). SWUSV is proposed as a small mission
  to CNES and to ESA for a possible flight as early as 2017-2018.

---------------------------------------------------------
Title: Cooler and Hotter X-ray Bright Points from Hinode/XRT
    Observations
Authors: Kariyappa, R.; DeLuca, E. E.; Saar, S. H.; Golub, L.; Damé,
   L.; Varghese, B. A.
2012ASPC..454..149K    Altcode:
  We use a 7-hour (17:00 UT - 24:00 UT) time sequence of soft X-ray images
  observed almost simultaneously in two filters (Ti_poly and Al_mesh) on
  April 14, 2007 with X-Ray Telescope (XRT) on-board the Hinode mission
  to determine the temperature of X-ray bright points (XBPs). A sample
  of 14 XBPs and 2 background coronal regions have been identified and
  selected on both the images for detailed analysis. The temperature of
  XBPs is determined by filter ratio method. We find that the XBPs show
  temperature fluctuations and that the average temperature ranges from
  1.1 MK to 3.4 MK which may correspond to different X-ray fluxes. These
  results suggest the existence of cooler and hotter XBPs and that the
  heating rate of XBPs is highly variable on short time scales.

---------------------------------------------------------
Title: SWUSV: a Space Weather Microsatellite Program to Investigate
    CMEs Precursors and the Influence of Solar UV Variability on Climate
Authors: Damé, Luc; Dudok De Wit, Thierry; Abdel Hady, Ahmed; Mahrous,
   Ayman; Quemerais, Eric; Keckhut, Philippe; Hauchecorne, Alain; Meftah,
   Mustapha; Zaki, Amal; Khaled, Safinaz; Ghitas, Ahmed; Marzouk, Besheir
2012cosp...39..394D    Altcode: 2012cosp.meet..394D
  No abstract at ADS

---------------------------------------------------------
Title: Solar Activity Monitoring of Flares and CMEs Precursors:
    the Importance of Lyman-Alpha
Authors: Damé, Luc; Kretzschmar, Matthieu; Dammasch, Ingolf; Kumara,
   S. T.; Kariyappa, R.; Dominique, Marie; Ueno, Satoru; Khaled, Safinaz
2012cosp...39..395D    Altcode: 2012cosp.meet..395D
  No abstract at ADS

---------------------------------------------------------
Title: Segmentation of Coronal Features to Understand the UV and
    EUV Irradiance Variations
Authors: Kumara, S. T.; Hochedez, Jean-François; Damé, Luc;
   Doddamani, Vijayakumar H.; Kariyappa, R.
2012cosp...39.1641K    Altcode: 2012cosp.meet.1641K
  No abstract at ADS

---------------------------------------------------------
Title: ESCAPE : a first step to high resolution solar coronagraphy
    in Antarctica
Authors: Damé, L.; Abe, L.; Faurobert, M.; Fineschi, S.; Kuzin, S.;
   Lamy, P.; Meftah, M.; Vives, S.
2012EAS....55..359D    Altcode:
  The Dome C high plateau is unique for coronagraphic observations: sky
  brightness is reduced, water vapour is low, seeing is excellent and
  continuity of observations on several weeks is possible. ESCAPE (the
  Extreme Solar Coronagraphy Antarctic Program Experiment) will perform
  2-dimensional spectroscopy of the forbidden line of FeXIV at 530.285 nm:
  precise line profile analysis will allow the diagnostic of the nature
  of waves by simultaneous measurements of velocities and intensities in
  the corona. ESCAPE is proposed to Institut Paul-Emile Victor (IPEV)
  for a campaign in 2012-2013 at Dome C/Concordia since all subsystems
  are available in particular thanks to an ESA STARTIGER 2010 R&amp;D
  "Toward a New Generation of Formation Flying Coronagraph". Using
  state-of-the-art technologies developed for Space missions (a
  Three Mirrors Anastigmat telescope, the TMA, a 4 stages Liquid
  Crystal Tunable-filter Polarimeter, the LCTP) allows us to propose
  an automated Coronal Green Line full-field Polarimeter for unique
  observations (waves nature and intensity to address coronal heating)
  with the best possible performances on Earth and for preparing and
  testing the technologies for the next steps in Space. No other site
  would allow such coronagraphic performances (the sky brightness is a
  factor 2 to 4 better than in Hawaï) and with high spatial resolution
  (better than an arcsec is possible).

---------------------------------------------------------
Title: New Technology Solar Coronagraphs
Authors: Koutchmy, S.; Bazin, C.; Damé, L.; Rochain, S.; Tavabi, E.
2012EAS....55..375K    Altcode:
  We present the Mirror Advanced technology Coronagraph (MAC) as a
  new generation solar telescope to be put at suitable high altitude
  coronal sites in order to resolve modern problems of solar physics,
  like the origin of the heating of the chromosphere and of the corona,
  the analysis of the mesospheric layers of the solar atmosphere and the
  effects of shearing the photospheric magnetic fields on the dynamics
  of the upper coronal layers.

---------------------------------------------------------
Title: Preliminary Results on Irradiance Measurements from Lyra
    and Swap
Authors: Kumara, S. T.; Kariyappa, R.; Dominique, M.; Berghmans, D.;
   Damé, L.; Hochedez, J. F.; Doddamani, V. H.; Chitta, Lakshmi Pradeep
2012AdAst2012E...5K    Altcode: 2012AdAst2012E..10K
  No abstract at ADS

---------------------------------------------------------
Title: Temperature variability in X-ray bright points observed
    with Hinode/XRT
Authors: Kariyappa, R.; Deluca, E. E.; Saar, S. H.; Golub, L.; Damé,
   L.; Pevtsov, A. A.; Varghese, B. A.
2011A&A...526A..78K    Altcode:
  <BR /> Aims: We investigate the variability in temperature as
  a function of time among a sample of coronal X-ray bright points
  (XBPs). <BR /> Methods: We analysed a 7-h (17:00-24:00 UT) long time
  sequence of soft X-ray images observed almost simultaneously in two
  filters (Ti_poly and Al_mesh) on April 14, 2007 with X-ray telescope
  (XRT) onboard the Hinode mission. We identified and selected 14 XBPs
  for a detailed analysis. The light curves of XBPs were derived using
  the SolarSoft library in IDL. The temperature of XBPs was determined
  using the calibrated temperature response curves of the two filters
  by means of the intensity ratio method. <BR /> Results: We find that
  the XBPs show a high variability in their temperature and that the
  average temperature ranges from 1.1 MK to 3.4 MK. The variations
  in temperature are often correlated with changes in average X-ray
  emission. It is evident from the results of time series that the XBP
  heating rate can be highly variable on short timescales, suggesting
  that it has a reconnection origin.

---------------------------------------------------------
Title: Demonstrator of the formation flying solar coronagraph
    ASPIICS/PROBA-3
Authors: Vives, Sébastien; Damé, Luc; Lamy, Philippe; Antonopoulos,
   A.; Bon, W.; Capobianco, G.; Crescenzio, G.; da Deppo, V.; Ellouzi,
   M.; Garcia, J.; Guillon, C.; Mazzoli, A.; Soilly, T.; Stathopoulos,
   F.; Tsiganos, C.
2010SPIE.7731E..47V    Altcode: 2010SPIE.7731E.136V
  Formation Flying opens the possibility to conceive and deploy giant
  solar coronagraphs in space permanently reproducing the optimum
  conditions of a total eclipse of the Sun ("artificial" eclipse) thus
  giving access to the inner corona with unprecedented spatial resolution
  and contrast (low stray light). The first opportunity to implement such
  a coronagraph "ASPIICS" will be offered by the European Space Agency
  (ESA) PROBA-3 technology mission devoted to the in-orbit demonstration
  of formation flying technologies. Two spacecrafts separated by about 150
  m form a giant externally-occulted coronagraph: the optical part hosted
  by one spacecraft remains entirely protected from direct sunlight
  by remaining in the shadow of an external occulter hosted by the
  other spacecraft. We developed and tested a scale-model 'breadboard'
  (i.e., 30m) of the PROBA-3/ASPIICS Formation Flying coronagraph. The
  investigations focused on two metrology systems capable of measuring
  both the absolute pointing of the coronagraph (by sensing the projected
  shadow and penumbra produced by the external occulting disk) and
  the alignment of the formation (by re-imaging light sources located
  on the rear-side of the occulting disk with the optical part of the
  coronagraph). In this contribution, we will describe the demonstrator
  and report on our results on the crucial question of the alignment and
  pointing in space of long instruments (&gt; 100 m) with an accuracy of
  a few arcsec. This study has been conducted in the framework of an ESA
  "STARTIGER" Initiative, a novel approach aimed at demonstrating the
  feasibility of a new and promising technology on a very short time scale
  (six months).

---------------------------------------------------------
Title: ASPIICS: a giant coronagraph for the ESA/PROBA-3 Formation
    Flying Mission
Authors: Lamy, Philippe; Damé, Luc; Vivès, Sébastien; Zhukov, Andrei
2010SPIE.7731E..18L    Altcode: 2010SPIE.7731E..31L
  Classical externally-occulted coronagraphs are presently limited in
  their performances by the distance between the external occulter and
  the front objective. The diffraction fringe from the occulter and the
  vignetted pupil which degrades the spatial resolution prevent useful
  observations of the white light corona inside typically 2-2.5 solar
  radii. Formation flying offers an elegant solution to these limitations
  and allows conceiving giant, externally-occulted coronagraphs using a
  two-component space system with the external occulter on one spacecraft
  and the optical instrument on the other spacecraft at a distance of
  hundred meters. Such an instrument, ASPIICS (Association de Satellites
  Pour l'Imagerie et l'Interférométrie de la Couronne Solaire), has
  just been selected by the European Space Agency (ESA) to fly (launch
  expected in 2014) on its third PROBA (Project for On-Board Autonomy)
  mission of formation flying demonstration which is presently in phase
  B. It will perform both high spatial resolution imaging of the solar
  corona as well as 2- dimensional spectroscopy of several emission
  lines (in particular the forbidden line of FeXIV at 530.285 nm) from
  the coronal base out to 3 solar radii. For this, it will use filters,
  polarisers and a solid Fabry-Perot interferometer ("étalon"). The
  classical design of an externally-occulted coronagraph is adapted to the
  formation flying configuration allowing the detection of the very inner
  corona as close as 0.04-0.05 solar radii (40-50 arcsec) from the solar
  limb. By tuning the position of the occulter spacecraft, it may even be
  possible to reach the chromosphere and the upper part of the spicules.

---------------------------------------------------------
Title: Simulation of the metrology of the PROBA-3/ASPIICS formation
    flying solar coronagraph
Authors: Stathopoulos, F.; Antonopoulos, A.; Vives, S.; Damé, L.
2010SPIE.7731E..44S    Altcode: 2010SPIE.7731E.133S
  Formation Flying is now considered to be the most promising and
  effective approach to deploy the forthcoming generation of very
  large instruments in space. PROBA-3 is a technology mission devoted
  to the in-orbit demonstration of formation flying techniques and
  technologies. PROBA-3 will implement a giant coronagraph (called
  ASPIICS) that will both demonstrate and exploit the capabilities
  and performances of formation flying. ASPIICS is distributed on two
  spacecrafts separated by 150m, one hosting the external occulting
  disk and the other the optical part of the coronagraph. ASPIICS
  will incorporate metrology units which will allow determining
  both the absolute pointing and the relative alignment of the
  formation. Photosensors located around the entrance pupil of the
  coronagraph will determine the absolute positioning of the instrument
  by sensing the penumbra behind the occulting disk. Light sources
  located on the rear-side of the occulting disk will allow verifying
  the alignment of the formation. We carried out a complete numerical
  simulation of the metrology system and showed how corrections are
  derived from the measurements to be applied to each spacecraft in
  case of misalignments. This simulation was validated by a scaled
  model of the coronagraph developed at Laboratoire d'Astrophysique de
  Marseille. This study has been conducted in the framework of an ESA
  "STARTIGER" Initiative, a novel approach aimed at demonstrating the
  feasibility of a new and promising technology on a very short time scale
  (six months).

---------------------------------------------------------
Title: Towards a New Formation Flying Solar Coronagraph
Authors: Lamy, P.; Vives, S.; Curdt, W.; Dame, L.; Davila, J.; Defise,
   J. M.; Fineschi, S.; Heinzel, P.; Kuzin, S.; Schmutz, W.; Tsinganos,
   K.; Turck-Chieze, S.; Zhukov, A.
2010ASPC..424...15L    Altcode:
  We briefly describe an investigation aiming at the development of a
  giant solar coronagraph instrument onboard of two satellites, separated
  by about 150 m in formation flight for the detailed observation of the
  solar coronal plasma. The European Space Agency (ESA) has selected this
  instrument as the only payload onboard the Proba 3 satellites which
  will be launched in 2013. The Greek team is developing the command
  control board of the coronagraph.

---------------------------------------------------------
Title: Calibration and alignment of the demonstrator of the
    PROBA-3/ASPIICS formation flying coronagraph
Authors: Crescenzio, Giuseppe; Capobianco, Gerardo; da Deppo, Vania;
   Damé, Luc; Vivès, Sébastien; Garcia, Josè; Guillon, Christophe
2010SPIE.7731E..48C    Altcode: 2010SPIE.7731E.137C
  This article describes the calibration and alignment procedures of a
  demonstrator for the ASPIICS coronagraph proposed for the ESA technology
  mission PROBA-3 aimed at demonstrating the feasibility of a Formation
  Flying coronagraph. ASPIICS is distributed on two spacecrafts separated
  by 150 m, one hosting the external occulting disk and the other the
  optical part of the coronagraph. The purpose of the demonstrator
  is to reproduce on ground the metrology systems that will equip the
  coronagraph in order to realize the alignment of the two spacecrafts
  and the absolute pointing to the center of the Sun. The demonstrator is
  composed of a device that reproduces the solar umbra/penumbra created
  by the solar occulter[1] and of a Three Mirror Anastigmatic (TMA)
  telescope mounted on a hexapod, a new-generation platform that allows 6
  degrees of freedom. A large plane folding mirror is used on ground to
  obtain a distance between the occulter and the TMA up to 30 m. Photo
  sensors located around the entrance pupil of the TMA determine the
  absolute positioning of the instrument by sensing the penumbra behind
  the occulting disk. Light sources (LEDs) located on the rear-side of the
  occulting disk allow verifying the alignment of the formation. The paper
  describes the whole demonstrator, its integration, its calibration, and
  the performance of the metrology systems of the coronagraph. This study
  has been conducted in the framework of an ESA "STARTIGER" Initiative,
  a novel approach aimed at demonstrating the feasibility of a new and
  promising technology on a very short time scale (six months).

---------------------------------------------------------
Title: HiRISE Mission to Address the Dynamical Chromosphere-Corona
    Interface
Authors: Damé, Luc; Lamy, Philippe; von Fay-Siebenburgen Erdélyi,
   Robert
2010cosp...38.2844D    Altcode: 2010cosp.meet.2844D
  Several ground facilities and space missions are currently dedicated
  to the study of the Sun at high resolution and of the solar corona
  in particular. However, and despite significant progress with the
  advent of space missions and UV, EUV and XUV direct observations of
  the hot chro-mosphere and million degrees coronal plasma, much is yet
  to be achieved in the understanding of these high temperatures, fine
  dissipative structures and of the coronal heating in general. Recent
  missions have shown the definite role of waves and of the magnetic
  field deep in the inner corona, at the chromosphere-corona interface,
  where dramatic changes occur. The dynamics of the chromosphere and
  corona is controlled by the emerging magnetic field, guided by the
  coronal magnetic field. Accordingly, the direct measurement of the
  chromospheric and coronal magnetic fields is of prime importance. The
  solar corona consists of many thin loops or threads with the plasmas
  brightening and fading independently. The dynamics in each thread is
  believed to be related to the formation of filaments, each one being
  dynamic, in a non-equilibrium state. The mechanism sustaining that
  dynamics, oscillations or waves (Alfvén or MHD?), require both very
  high-cadence, multi-spectral observations, and high resolution. This
  is foreseen in the future Space Mission HiRISE, the ultimate new
  generation ultrahigh resolution, interferomet-ric and coronagraphic,
  Solar Physics Mission, proposed for ESA Cosmic Vision (pre-selected
  in 2007, and under preparation for 2012 second call). HiRISE (High
  Resolution Imaging and Spectroscopy Explorer), at the L1 Lagrangian
  point, provides meter class FUV imaging and spectro-imaging, EUV and
  XUV imaging and spectroscopy, and ultimate coronagraphy by a remote
  external occulter (satellites in formation flying 280 m apart) allowing
  to characterize temperature, densities and velocities in the solar upper
  chromosphere, transition zone and inner corona with, in particular, 2D
  very high resolution multi-spectral imaging-spectroscopy, direct coronal
  magnetic field measurement: a unique set of tools to understand the
  structuration and onset of coronal heating. We give a detail account
  of the proposed mission profile, major scien-tific objectives and
  model payload of HiRISE, a natural complement to the Solar Probe type
  missions lacking duty cycle, high resolution, spatial, spectral and
  temporal multi-temperature diagnostics and full coronal magnetometry.

---------------------------------------------------------
Title: ASPIICS / PROBA-3 formation flying externally-occulted giant
    coronagraph mission
Authors: Lamy, Philippe; Damé, Luc
2010cosp...38.1882L    Altcode: 2010cosp.meet.1882L
  During the time operation of the Helios mission, from 1974 to
  metricconverterProductID1986, a1986, a large number of magnetic clouds
  was identified by the magnetic field and solar wind sensors onboard
  the probes. Among these magnetic clouds, some of them were identified
  by at least two probes, provided that IMP-8 and ISEE-3 were monitoring
  the dayside magnetosphere. The magnetic cloud observed on from DOY 029
  to DOY 030/1977 by Helios 1, Helios 2, and IMP-8 represents a potential
  multi-spacecraft observed magnetic cloud. Despite the interaction with
  the high-speed stream that compressed the magnetic cloud, the minimum
  variance analysis technique showed the same direction of rotation of
  the magnetic field inside the magnetic cloud. This helped to associate
  the observation of the magnetic cloud at multi-spacecraft.

---------------------------------------------------------
Title: Long-period intensity oscillations of the quiet solar
    atmosphere from TRACE 1600 Åcontinuum observations.
Authors: Kariyappa, R.; Damé, L.
2010MmSAI..81..786K    Altcode:
  We have analysed a 6-hour long time sequence of ultraviolet (uv) images
  obtained on May 24, 2003 in 1600 Å continuum under high spatial
  and temporal resolutions from the Transition Region and Coronal
  Explorer (TRACE). We have selected 15 isolated bright points, 15
  network elements and 15 quiet background regions from these images for
  detailed analysis. We derived the cumulative intensity values and the
  light curves of these features for the total duration of observations,
  and performed also a power spectrum analysis using the complete time
  series data. We found that the uv bright points, the uv network and
  the uv background regions exhibit long-period intensity oscillations
  namely, 5.5 hours, 4.6 hours and 3.4 hours respectively, in addition
  to the more familiar small scale intensity fluctuations. We suggest
  that these longer periods of oscillation might be related to solar
  atmospheric g-modes.

---------------------------------------------------------
Title: ARENA Solar Astrophysics Working Group Reporting on Dome C
    Exceptional Potential for Solar Observations
Authors: Damé, L.; Andretta, V.; Arena Solar Astrophysics Working
   Group Members
2010EAS....40..451D    Altcode:
  The ARENA Solar Astrophysics Working Group (WG6) is reviewing the
  exceptional site conditions prevailing at Dome C/Concordia making it
  a unique place on Earth for solar observations: excellent seeing, low
  sky brightness, low water vapour and high duty cycle. These qualities
  open science programmes which can combine very high resolution,
  coronagraphy, infrared access, and long time series (continuity). Major
  objectives accessible are the chromosphere-corona interface at very
  high resolution, direct magnetic field measurements in the chromosphere
  (prominences) and in the corona, 2D imaging spectroscopy and waves. A
  first mid-size facility is proposed and described, AFSIIC (Antarctica
  Facility for Solar Interferometric Imaging and Coronagraphy),
  using 3×Ø50 cm off-axis telescopes (1.4 m equivalent telescope)
  to access these objectives with the proper flux, angular resolution
  and coronagraphic potential. Support infrastructure and logistics have
  been studied and are discussed, noticeably a 30 m tower to place the
  observatory over the very thin surface turbulent layer of Dome C.

---------------------------------------------------------
Title: The solar diameter is most probably constant over the solar
    cycle
Authors: Damé, Luc
2010cosp...38.1701D    Altcode: 2010cosp.meet.1701D
  We analyzed 7 years of filtregrams data (150000 photograms and
  magnetograms) of the SOHO/MDI experiment. We used the maximum possible
  sampling compatible with full frame recording, carefully avoiding any
  suspicious filtregram. Going further than the previous analysis of
  Emilio et al. (Ap. J. 543, 2000) and Kuhn et al. (Ap. J. 613, 2004)
  we better corrected for changes in optical aberrations and, along
  Turmon et al. (Ap. J., 568, 396, 2002), we reduced radius measurement
  errors by identifying active regions from magnetograms and by avoiding
  radius measurements herein. We found that, within the limit of our noise
  level uncertainties (8 to 9 mas), the solar diameter is compatible with
  constancy over the half cycle investigated. Our results confirm the
  reanalysis of the 7 years of MDI data of Antia (Ap. J. 590, 2003), with
  a completely different method since using the ultra-precise frequency
  variation of the f-modes (fundamental modes linked to the diameter),
  who found (carefully removing the yearly Earth induced variations
  and avoiding the SOHO data gap of 1999) that the diameter is constant
  over the half solar cycle (radius variation are less than 0.6 km, 0.8
  mas -nothing over noise level). We can conclude, along Antia, that:
  "If a careful analysis is performed, then it turns out that there is
  no evidence for any variation in the solar radius." There were no
  theoretical reasons for large solar radius variations and there is
  no observational evidence for them with consistent space observations
  made with 3 different approaches.

---------------------------------------------------------
Title: ASPIICS / PROBA-3: a formation flying externally-occulted
    giant coronagraph mission
Authors: Lamy, Philippe; Damé, Luc; Curdt, W.; Davila, J.; Defise,
   J. M.; Fineschi, S.; Heinzel, P.; Howard, R.; Kuzin, S.; Schmutz,
   W.; Tsinganos, K.; Turck-Chièze, S.; Zhukov, A.
2010cosp...38.2858L    Altcode: 2010cosp.meet.2858L
  Classical externally-occulted coronagraphs are presently limited in
  their performances by the distance between the external occulter and
  the front objective. The diffraction fringe from the occulter and
  the vignetted pupil which degrades the spatial resolution prevent
  useful observa-tions of the white light corona inside typically 2-2.5
  Rsun. Formation flying offers an elegant solution to these limitations
  and allows conceiving giant, externally-occulted coronagraphs
  us-ing a two-component space system with the external occulter on
  one spacecraft and the optical instrument on the other spacecraft
  at distances of hundred meters. Such an instrument has just been
  selected by ESA to fly (by the end of 2013) on its PROBA-3 mission,
  presently in phase B, to demonstrate formation flying. It will perform
  both high spatial resolution imaging of the solar corona as well as
  2-dimensional spectroscopy of several emission lines (in partic-ular
  the forbidden line of FeXIV at 530.285 nm) from the coronal base out
  to 3 Rsun using a Fabry-Perot interferometer. The classical design of
  an externally-occulted coronagraph is adapted to the formation flying
  configuration allowing the detection of the very inner corona as close
  as 0.05 Rsun from the solar limb. By tuning the position of the occulter
  spacecraft, it may even be possible to try reaching the chromosphere
  and the upper part of the spicules. ASPIICS/PROBA-3 mission, payload
  and scientific objectives are detailed.

---------------------------------------------------------
Title: Multi-spacecraft observation of a magnetic cloud
Authors: de Lucas, Aline; Dal Lago, Alisson; Schwenn, Rainer; Clúa de
   Gonzalez, Alicia L.; Marsch, Eckart; Lamy, Philippe; Damé, Luc; Curdt,
   W.; Davila, J.; Defise, J. M.; Fineschi, S.; Heinzel, P.; Howard, R.;
   Kuzin, S.; Schmutz, W.; Tsinganos, K.; Turck-Chièze, S.; Zhukov, A.
2010cosp...38.1921D    Altcode: 2010cosp.meet.1921D
  Classical externally-occulted coronagraphs are presently limited in
  their performances by the distance between the external occulter and
  the front objective. The diffraction fringe from the occulter and
  the vignetted pupil which degrades the spatial resolution prevent
  useful observa-tions of the white light corona inside typically 2-2.5
  Rsun. Formation flying offers an elegant solution to these limitations
  and allows conceiving giant, externally-occulted coronagraphs
  us-ing a two-component space system with the external occulter on
  one spacecraft and the optical instrument on the other spacecraft
  at distances of hundred meters. Such an instrument has just been
  selected by ESA to fly (by the end of 2013) on its PROBA-3 mission,
  presently in phase B, to demonstrate formation flying. It will perform
  both high spatial resolution imaging of the solar corona as well as
  2-dimensional spectroscopy of several emission lines (in partic-ular
  the forbidden line of FeXIV at 530.285 nm) from the coronal base out
  to 3 Rsun using a Fabry-Perot interferometer. The classical design of
  an externally-occulted coronagraph is adapted to the formation flying
  configuration allowing the detection of the very inner corona as close
  as 0.05 Rsun from the solar limb. By tuning the position of the occulter
  spacecraft, it may even be possible to try reaching the chromosphere
  and the upper part of the spicules. ASPIICS/PROBA-3 mission, payload
  and scientific objectives are presented.

---------------------------------------------------------
Title: 30 m Stable towers for optimum astronomical observations at
    dome c/concordia
Authors: Dournaux, J. -L.; Amans, J. -P.; Damé, L.; Le Moigne, J.
2010EAS....40..477D    Altcode:
  This paper gives an overview of conceptual studies that have been
  realized since 2007 on 30 m towers for Dome C taking into account
  local available infrastructures and conditions. Some 30 m tower's
  concepts are presented and finite element simulations are carried to
  determine their dynamic behaviour including wind-induced vibrations,
  and to optimize their design.

---------------------------------------------------------
Title: New perspectives in solar coronagraphy offered by formation
flying: from PROBA-3 to Cosmic Vision
Authors: Lamy, P.; Vivès, S.; Damé, L.; Koutchmy, S.
2008SPIE.7010E..1HL    Altcode:
  Formation flying opens new perspectives in solar physics, and allow to
  conceive giant, externally-occulted coronagraphs using a two-component
  space system with the external occulter on one spacecraft and the
  optical instrument on the other spacecraft at a distance of hundred
  meters. Conditions close to those of a solar total eclipse can then be
  achieved offering the capability of imaging the solar corona down to the
  limb at very high spatial resolution. ASPIICS (Association de Satellites
  Pour l'Imagerie et l'Interférométrie de la Couronne Solaire) is a
  mission proposed to ESA in the framework of its PROBA-3 demonstration
  program of formation flying which is presently in phase A. ASPIICS is
  a single coronagraph which will perform both high spatial resolution
  imaging of the solar corona as well as 2-dimensional spectroscopy of
  several emission lines from the coronal base out to 3 R\beye using
  a Fabry-Pérot étalon interferometer. The classical design of an
  externally-occulted coronagraph is adapted to the formation flying
  configuration allowing the detection of the very inner corona as
  close as 0.01 R\beye from the solar limb. Super-ASPIICS is an even
  more ambitious instrument part of the scientific payload of HiRise,
  the High Resolution Imaging and Spectroscopy Explorer proposed to
  ESA in the framework of its Cosmic Vision program. With an increased
  inter-satellite distance of 280 m, an aperture of 300 mm, a spectral
  domain extending from the ultraviolet to the near-infrared, and
  spectroscopic capabilities, Super-ASPIICS will offer unprecedented
  diagnostic capabilities, including the measurement of coronal magnetic
  fields.

---------------------------------------------------------
Title: Observational searches for g-mode oscillations in the quiet
    solar atmosphere from TRACE 1600A Continuum Observations
Authors: Kariyappa, R.; Dame, L.
2008arXiv0804.3502K    Altcode:
  Our aim is to search for atmospheric g-mode oscillations in UV
  network, UV bright points and Uv background regions. We have analysed
  a 6-hours of time sequence of ultraviolet (uv) images obtained on
  May 24, 2003 in 1600A continuum under high spatial and temporal
  resolution from Transition Region and Coronal Explorer (TRACE). We
  have selected an isolated 15 uv bright points, 15 uv network elements
  and 15 uv background regions in a quiet region from the images for
  the detailed analysis. We derived the cumulative intensity values of
  these features. The light curves of all the features have been derived
  for the total duration of observations and done the power spectrum
  analysis using the time series data. We found that the uv bright points,
  the uv network and uv background regions will exhibit a longer period
  of intensity oscillations namely, 5.5 hours, 4.6 hours and 3.4 hours
  respectively, in addition to the more familiar small scale intensity
  fluctuations. We suggest that the longer periods of oscillation may
  be related to solar atmospheric g-modes.

---------------------------------------------------------
Title: Solar Astrophysics, Interferometry, and Coronagraphy at
    DomeC/Concordia
Authors: Damé, L.; Amans, J. -P.; Dournaux, J. -L.; Koutchmy, S.;
   Lamy, P.; Preumont, A.
2008EAS....33..105D    Altcode:
  Excellent seeing, coronal conditions, and very low IR thermal
  background are qualities of the Dome C/Concordia station site that
  will allow unique solar astrophysics science. We review the science
  case for inner corona observations (onset of the coronal heating
  mechanism still poorly understood) and the promises of high angular
  resolution to disentangle the possible mechanisms at work between
  waves, convection, and reconnection in this particularly magnetically
  structured solar atmosphere between the high chromosphere and inner
  corona. For coronagraphy, IR and high resolution possibilities, Dome
  C is a case by itself between classical ground-based sites and space
  opportunities. Telescopes from 50 cm (coronagraphy oriented) to 4 m
  (full high resolution advantage including IR access) are proposed to
  benefit from these remarkable observing capabilities. Using 3×O50
  cm off-axis telescopes, we first propose a medium size facility
  (1.4 m equivalent telescope) for very high resolution access, ADSIIC
  (Antarctica Demonstrator of Solar Interferometric Imaging &amp;
  Coronagraphy), before the ultimate 9-telescope Solar Facility
  equivalent to a 4 m diameter telescope: A-FOURMI (Antarctica 4 m
  Interferometer). Finally, 30 m tower designs and their logistics using
  standard containers and elementary elements of 6 m maximum length,
  are presented and discussed. These towers are indeed of general
  interest also for the other optical and IR telescopes intended for
  Dome C/Concordia, allowing to get over most of the turbulent ground
  layer and to reach the best possible permanent seeing conditions
  (better than half an arcsec).

---------------------------------------------------------
Title: Telescope and instrument robotization at Dome C
Authors: Strassmeier, K. G.; Agabi, K.; Agnoletto, L.; Allan, A.;
   Andersen, M. I.; Ansorge, W.; Bortoletto, F.; Briguglio, R.; Buey,
   J. -T.; Castellini, S.; Coudé du Foresto, V.; Damé, L.; Deeg,
   H. J.; Eiroa, C.; Durand, G.; Fappani, D.; Frezzotti, M.; Granzer, T.;
   Gröschke, A.; Kärcher, H. J.; Lenzen, R.; Mancini, A.; Montanari,
   C.; Mora, A.; Pierre, A.; Pirnay, O.; Roncella, F.; Schmider, F. -X.;
   Steele, I.; Storey, J. W. V.; Tothill, N. F. H.; Travouillon, T.;
   Vittuari, L.
2007AN....328..451S    Altcode: 2004astro.ph..8233Z
  This article reviews the situation for robotization of telescopes
  and instruments at the Antarctic station Concordia on Dome C. A
  brain-storming meeting was held in Tenerife in March 2007 from which
  this review emerged. We describe and summarize the challenges for
  night-time operations of various astronomical experiments at conditions
  “between Earth and Space” and conclude that robotization is likely
  a prerequisite for continuous astronomical data taking during the
  2000-hour night at Dome C.

---------------------------------------------------------
Title: Solar Shape Changes and Oscillations from Space (P15)
Authors: Damé, L.
2006ihy..workE.107D    Altcode:
  The diameter was observed to be constant over the last solar cycles and,
  as such, is not a "proper" solar-terrestrial "climate" indicator. Ground
  measurements with small telescopes are spurious diffraction and seeing
  affected, the Maunder Minimum ones of Picard during the XVII century
  not being an exception. Large instruments (like the 45 cm Gregory's of
  A. Wittmann in Locarno and Tenerife) that average seeing cells see no
  variations (&lt; 40 mas) and, as well, space instruments (MDI/SOHO)
  that are naturally not affected by turbulence. We present the four
  approaches, Wittmann on ground with large telescopes, Kuhn et al. (2004)
  who used the six pixels limb data of MDI, Antia (2003) with a completely
  different method since using the ultra-precise frequency variation of
  the f-modes, and our approach (Damé and Cugnet, 2006) using seven years
  of MDI filtergrams data (150 000 photograms and magnetograms). These
  four careful analyses converge towards the same insignificant variations
  (below 15 mas for space experiments or even less: 0.6 km, 0.8 mas for
  the helioseismology approach!). Following Antia, we conclude that:
  "If a careful analysis is performed, then it turns out that there is
  no evidence for any variation in the solar radius." There were no
  theoretical reasons for large solar radius variations and there is
  no observational evidence for them with consistent ground and space
  observations. This being said, the radius measurements are of interest
  for the solar shape changes that might occur along the cycle (sub-
  surface convective flows?). Radius oscillations (but higher in the
  atmosphere, further in the UV: 220 nm) might also bring up low order
  p-modes and, eventually, g-modes if ever accessible. At the level of
  formation of the 220 nm continuum there is the maximum magnification
  of the p-modes and intensity oscillations. 220 nm is also the Lyman
  Alpha absorption region and ozone formation layer. A New Solar Shape
  and Oscillation Telescope (NSSOT) is proposed and designed along the
  non-degraded UV imaging concept developed earlier for SODISM/PICARD
  (Damé, et al., 1999, 2000, 2001), optimized for these measures of solar
  shape and oscillations at 220 nm. It has a carbon-carbon structure, SiC
  mirrors, no window and no spurious optics affecting thermal behavior and
  scattered light. A model of simplicity and precision. Lyman Alpha and UV
  images, in selected wavelengths, will complete these measurements. We
  present the design and bread-boarding activities (SiC thermally
  controlled mirrors) of NSSOT, and its scientific revisited objectives.

---------------------------------------------------------
Title: Chromosphere and Transition Zone Dynamics and Heating: Need
    for Future Space Missions
Authors: Damé, L.
2006ihy..workE..34D    Altcode:
  SOHO and TRACE observations have clearly shown that even the very
  quietest part of the solar chromosphere is very structured and
  dynamic with brightenings and waves. Diagnostics from this region
  are very difficult because spectral lines are neither formed in
  LTE nor under optically thin conditions that prevail higher in the
  Transition Zone. The gas goes from being dominated by the gas pressure
  in the photosphere to being dominated by the magnetic pressure in the
  upper chromosphere, involving steep gradients to obtain significant
  dissipation or heating. The ionization balance of important elements
  is furthermore out of equilibrium. A proper understanding thus demands
  very high spatial resolution with accurate measurements of velocity and
  line width, uninterrupted in Space, across a broad range of temperature
  ("heights"), to distinguish between wave heating and reconnection
  events in the chromosphere and Transition Zone. Complex modeling, that
  ideally should include non-LTE radiative transfer in 3D including the
  dynamic driving in the convection zone, non- equilibrium ionization,
  magnetic fields, the transition region and the corona, will be necessary
  to understand these observations. We will discuss various aspects of
  this very complex problem and insist on ground measures and, above all,
  Future Space Missions which should better address Doppler information,
  temperature coverage and discrimination and, most important, very high
  spatial resolution to progress on the way to a fully comprehensive
  view of chromospheric and coronal heating.

---------------------------------------------------------
Title: Observational Searches for Chromospheric g-Mode
    Oscillationsfrom CaII H-Line Observations
Authors: Kariyappa, R.; Dame, L.; Hiremath, K. M.
2006JApA...27..327K    Altcode:
  We have used a high spatial and temporal resolution of long time
  sequence of spectra in CaII H-line obtained at the Vacuum Tower
  Telescope (VTT) of the Sacramento Peak Observatory on a quiet region
  at the center of the solar disk over a large number of bright points
  and network elements to search for atmospheric (chromospheric) g-mode
  oscillations. An important parameter of the H-line profile, intensity at
  H<SUB>2V</SUB>(IH<SUB>2V</SUB>), has been derived from a large number
  of line profiles. We derived the light curves of all the bright points
  and network elements. The light curves represent the main pulse with
  large intensity amplitude and followed by several follower pulses with
  lower intensity amplitudes. The light curves of these bright points
  would give an impression that one can as well draw curves towards and
  away from the highest peak (main pulse) showing an exponential growth
  and decay of the amplitudes. An exponential decaying function has been
  fitted for all the light curves of the bright points to determine the
  damping time of the modes that are more or less the same, and one
  value of the coefficient of exponent can represent reasonably well
  the decay for all the cases. The FFT analysis of temporal variation of
  both the bright points and the network elements indicates around 10-min
  periodicity. We speculate that this longer period of oscillation may
  be related to chromospheric g-mode oscillations.

---------------------------------------------------------
Title: Search For Atmospheric G-mode Oscillations from TRACE
    Observations
Authors: Kariyappa, R.; Dame, L.; Varghese, B. A.
2006IAUJD...3E...1K    Altcode:
  An identification and clarification of different modes of oscillations
  may eventually illuminate the solar neutrino problem. The internal
  g-modes of the Sun are the most powerful tool for investigation of
  solar core and the neutrino problem. The detection of atmospheric
  g-mode oscillations are also equally important in order to know
  the role of different kinds of oscillations in the heating of the
  chromosphere and corona. We have analysed a 6-hours of time sequence of
  ultraviolet images obtained on May 24, 2003 in 1600 Å continuum under
  high spatial and temporal resolution with TRACE Space Mission. We have
  chosen 15 uv bright points, 15 uv network elements and 15 uv background
  regions from the time sequence images for the detailed analysis. We
  derived the cumulative intensity values of all these features using
  SolarSoftware (SSW) in IDL. The light curves of all the features have
  been generated for the total duration of observations. We have done
  the power spectrum analysis using their time series data. We find that
  the uv bright points, the uv network and uv background regions will
  exhibit longer period of intensity oscillations namely, 5.5 hours,
  4.6 hours and 3.4 hours respectively, in addition to small scale
  intensity fluctuations. We suggest that these periods may be related
  to a very high order atmospheric g-modes showing a large periods at
  the transition region.

---------------------------------------------------------
Title: Contribution of Chromospheric Features to UV Irradiance
    Variability
Authors: Kariyappa, R.; Dame, L.
2006IAUJD...8E...1K    Altcode:
  We have determined the time series data of the different parameters
  like the intensity, area, the full-disk intensity (spatial K index),
  and the Full Width at Half Maximum (FWHM) for the segregated features
  of the chromosphere from the CaII K spectroheliograms of 1992 and 1980,
  observed at the NSO at Sac Peak, using their histograms taken for the
  full-disk. We established, for the first time, from the results of 1992
  and 1980 images that the FWHM can be used as a good index for measuring
  and describing the chromospheric activity in the K-line. Our study
  shows that besides the plages, a significant portion of the variation
  observed in UV irradiance is related to the changing emission of the
  network and intranetwork + background regions. This indicates that in
  addition to plages and network, the intranetwork + background regions
  may also play a significant role in their contribution to the variation
  in UV irradiance. We estimated the contribution of various chromospheric
  features to the total CaII K flux from the intensity time series data
  and found that about 50% of the CaII K solar cycle variability results
  from plages, about 32% from network, and about 18% from intranetwork +
  background features.

---------------------------------------------------------
Title: A Very High Resolution Vision for Solar Physics: Interferometry
    &amp; Spectral-Imaging in the Far Ultraviolet
Authors: Damé, L.
2006ESASP.617E..35D    Altcode: 2006soho...17E..35D
  No abstract at ADS

---------------------------------------------------------
Title: Multi-aperture Instantaneous Interferometric Imaging of
    Extended and Moving Objects by Phase Optimized Spatial Filtering
Authors: Dame, L.
2006ESASP.621E..74D    Altcode: 2006spop.confE..74D
  No abstract at ADS

---------------------------------------------------------
Title: Preliminary results from the March 29, 2006 total eclipse
    observations in Egypt
Authors: Koutchmy, S.; Daniel, J. -Y.; Mouette., J.; Vilinga, J.;
   Noëns, J. -C.; Damé, L.; Faurobert, M.; Dara, H.; Hady, A.; Semeida,
   M.; Sabry, M.; Domenech, A.; Munier, J. -M.; Jimenez, R.; Legault,
   Th.; Viladrich, Ch.; Kuzin, S.; Pertsov, A.; O. A. Team
2006sf2a.conf..547K    Altcode:
  A coordinated effort has been carried in the framework of
  the French-Egyptian scientific cooperation to permit joined
  simultaneous eclipse observations of the solar corona during the
  total solar eclipse of March 29, 2006. Spaceborne EIT and Lasco (SoHO)
  observations were also planned at the same time and were successfully
  collected. Scientists from other countries collaborated on different
  experiments. The synthetic image showing the magnetic coronal structure
  of this quasi-minimum corona seen in W-L is given. Some preliminary
  results are presented; a White Light (W.L.) movie has been also taken
  during the totality.

---------------------------------------------------------
Title: SOLARNET &amp; LAIME: Imaging &amp; Spectroscopy in the
    Far Ultraviolet
Authors: Damé, Luc; Koutchmy, Serge
2006IAUS..233..435D    Altcode:
  SOLARNET is a medium size high resolution solar physics mission proposed
  to CNES and ESA for a new start in 2007 and a possible launch in 2012
  (CNES) or later (ESA Cosmic Vision framework: 2015-2016). Partnerships
  with India and China are under discussion, and several European
  contributions are considered. At the center of the SOLARNET mission is
  a 3-telescope interferometer of 1 meter baseline capable to provide 40
  times the best ever spatial resolution achieved in Space with previous,
  current or even planned solar missions: 20 mas - 20 km on the Sun in the
  FUV. The interferometer is associated to an on-axis Subtractive Double
  Monochromator coupled to an Imaging Fourier Transform Spectrometer
  capable of high spectral (0.01 nm) and high temporal resolutions
  (50 ms) on a field of view of 40 arcsec and covering the FUV and UV
  spectral domains (from 117.5 to 400 nm). This will allow to access
  process scales of magnetic reconnection, dissipation, emerging flux
  and much more, from the chromosphere to the low corona with emphasis
  on the transition zone where the magnetic confinement is expected
  to be maximum. A whole new chapter of the physics of solar magnetic
  field structuring, evolution and mapping from the photosphere to the
  high atmosphere will be opened. The interferometer is completed by
  instruments providing larger field of view and higher temperature
  (EUV-XUV coronal imaging &amp; spectroscopy) to define the context
  and extension of the solar phenomena. The 3-telescope interferometer
  design results of an extensive laboratory demonstration program
  of interferometric imaging of extended objects. We will review the
  scientific program of SOLARNET, describe the interferometer concept
  and design, present the results of the breadboard and give a short
  overview of the mission aspects. In a different category, LAIME,
  the Lyman Alpha Imaging-Monitor Experiment, is a remarkably simple
  (no mechanisms) and compact full Sun imager to be flown with TESIS on
  the CORONAS-PHOTON mission in 2008. It could be the only chromospheric
  imager to be flown in the next years, supporting Solar-B, STEREO,
  SDO and the Belgian LYRA Lyman Alpha flux monitor. We will give a
  short description of this unique 60 mm aperture imaging telescope,
  dedicated to the investigation of the UV sources of solar variability
  and of the chromospheric and coronal disruptive events (Moreton waves,
  prominences, CMEs, etc.).

---------------------------------------------------------
Title: Frontier full field spectro-imaging with the SOLARNET
    3-telescope interferometric breadboard
Authors: Damé, L.; Fu, X.; Kozlowski, M.; Maury, V.; Montaron, C.
2006cosp...36.3517D    Altcode: 2006cosp.meet.3517D
  The SOLARNET breadboard consists in 3 small objectives of diameter
  60 mm on a 165 mm baseline As such fed by a large siderostat acting
  as the satellite platform it mimics the SOLARNET space mission using 3
  larger 35 cm telescopes on a 1 meter equivalent interferometric baseline
  Because of its compact design and of an appropriate imaging spectrometer
  in the focal plane instantaneous imaging in narrow spectral bands is
  possible The 3-telescopes interferometer design results of an extensive
  laboratory demonstration program of interferometric imaging of extended
  objects started 10 years ago The principles of the interferometric
  compact recombination of the SOLARNET Space Mission capable of
  large field instantaneous spectro-imaging have been demonstrated
  in laboratory since 2000 Over the last 5 years the breadboard was
  completed with active fine pointing and spectro-imaging capabilities
  to directly observe the Sun and the breadboard was moved to the Grand
  Sid erostat de Foucault at Meudon Observatory Ultimate refinements in
  the global three telescopes phase measure by active spatial filtering
  centering of the cophasing reference field of view have recently been
  implemented to guarantee cophasing even on a moving changing reference
  field of view Design and concepts will be explicited and the first
  interferometric images of the Sun obtained at Meudon Observatory with
  the breadboard will be presented validating the concept retained for
  the SOLARNET space mission

---------------------------------------------------------
Title: SOLARNET: a UV, FUV, EUV, XUV high resolution imaging,
    spectro-imaging and spectroscopy mission.
Authors: Damé, L.
2006cosp...36.3513D    Altcode: 2006cosp.meet.3513D
  SOLARNET is a high resolution mission which encompass extremely high
  resolution in the UV and FUV to access process scales of magnetic
  reconnection dissipation emerging flux onset of Flares and CME s origin
  of solar wind The chromosphere to the low corona with emphasis on
  the transition zone where the magnetic confinement is expected to be
  maximum are at the heart of this mission which will open a whole new
  chapter of the physics of solar magnetic field structuring evolution
  and mapping from the photosphere to the heliosphere SOLARNET is an
  inexpensive and compact medium size high resolution solar physics
  mission that will bring together most of the best of SOHO and TRACE
  It is proposed to CNES and ESA for a new start in 2006 and a possible
  launch in 2011-2012 to fill the gap before the first results of the
  Solar Orbiter or Probe results in the late 2018 at best Partnerships
  with India and China are under discussion and several European
  contributions are considered SOLARNET instrumentation consists in a
  multiple instrument payload to achieve both the necessary global view
  of extended events and the detailed high resolution understanding of
  them The major instrument is a 3-telescope interferometer of 1 meter
  baseline capable to provide 50 times the best ever spatial resolution
  achieved in Space with previous current or even planned solar missions
  20 mas -- 20 km on the Sun in the FUV The interferometer is associated
  to an on-axis Subtractive Double Monochromator coupled to an Imaging
  Fourier Transform Spectrometer itself capable of very high spectral

---------------------------------------------------------
Title: An Observational Evidence for Solar Atmospheric G-Mode
    Oscillations From 1600A UV Continuum Observations
Authors: Kariyappa, R.; Dame, L.
2006cosp...36....6K    Altcode: 2006cosp.meet....6K
  An identification and clarification of different modes of oscillations
  may eventually illuminate the solar neutrino problem Particularly the
  internal g-modes of the Sun are the most powerful tool for investigation
  of solar core and a way to solve for instance the neutrino problem We
  have used a high spatial and temporal resolution of long time sequence
  of images obtained under high spatial and temporal resolution with
  TRACE Space Mission in 1600A UV continuum We derived the cumulative
  intensity values of the UV bright points The light curves of the UV
  bright points have been generated The FFT analysis of temporal variation
  of the UV bright points of the transition region indicates an evidence
  of longer periods of oscillations of the order of 45-min and 10-min This
  confirms the results obtained from CaII H -line observations Kariyappa
  et al 2005 and suggest that the longer period of oscillations may be
  related to solar atmospheric g-mode oscillations The detailed results
  of this analysis will be discussed in this paper

---------------------------------------------------------
Title: The New Solar Shape and Oscillations Telescope (NSSOT)
    Experiment for SOLARNET
Authors: Damé, L.
2006cosp...36.3526D    Altcode: 2006cosp.meet.3526D
  The diameter was observed to be constant over the solar cycle and as
  such will never be a proper solar-terrestrial climate indicator ground
  measures with small telescopes are spurius the Maunder Minimum ones of
  Picard during the XVII century not being an exception Large instruments
  like the 45 cm Gregorys of Axel Wittmann in Locarno and Tenerife which
  average seeing cells see no variations ll 40 mas as well as the space
  instrument MDI SOHO naturally not affected by turbulence either We
  present the 4 approaches Wittmann on ground with large telescopes
  Emilio et al 2000 and Kuhn et al 2004 whom used the 6 pixels limb
  data of MDI Antia 2003 with a completely different method since using
  the ultra-precise frequency variation of the f-modes and our approach
  Dam e and Cugnet 2006 using the complete 7 years of filtergrams data
  150 000 photograms and magnetograms of the SOHO MDI experiment These
  4 careful analysis converge towards the same insignificant below 15
  mas variations or even less 0 6 km 0 8 mas in the helioseismology
  approach Following Antia we can conclude that If a careful analysis is
  performed then it turns out that there is no evidence for any variation
  in the solar radius There were no theoretical reasons for large solar
  radius variations and there is no observational evidence for them
  with consistent ground and space observations This being stated and
  admitted the radius measure keeps interest through the solar shape
  that might change along the cycle sub-surface convective flows

---------------------------------------------------------
Title: The Lyman Alpha Imaging-Monitor Experiment (LAIME) for
    TESIS/CORONAS-PHOTON
Authors: Damé, L.; Koutchmy, S.; Kuzin, S.; Lamy, P.; Malherbe,
   J. -M.; Noëns, J. -C.
2006cosp...36.3524D    Altcode: 2006cosp.meet.3524D
  LAIME the Lyman Alpha Imaging-Monitor Experiment is a remarkably
  simple no mechanisms and compact 100x100x400 mm full Sun imager to be
  flown with TESIS on the CORONAS-PHOTON mission launch expected before
  mid-2008 As such it will be the only true chromospheric imager to be
  flown in the next years supporting TESIS EUV-XUV imaging SDO and the
  Belgian LYRA Lyman Alpha flux monitor on the ESA PROBA-2 microsatellite
  launch expected in September 2007 We will give a short description
  of this unique O60 mm aperture imaging telescope dedicated to the
  investigating of the magnetic sources of solar variability in the UV and
  chromospheric and coronal disruptive events rapid waves Moreton waves
  disparitions brusques of prominences filaments eruptions and CMEs onset
  The resolution pixel is 2 7 arcsec the field of view 1 4 solar radius
  and the acquisition cadence could be as high as 1 image minute The back
  thinned E2V CCD in the focal plane is using frame transfer to avoid
  shutter and mechanisms Further more the double Lyman Alpha filtering
  allows a 40 AA FWHM bandwidth and excellent rejection yet providing
  a vacuum seal design of the telescope MgF2 entrance window Structural
  stability of the telescope focal length 1 m is preserved by a 4-INVAR
  bars design with Aluminium compensation in a large pm 10 o around 20 o

---------------------------------------------------------
Title: Contribution of Solar Chromospheric Features to UV Irradiance
    Variability
Authors: Kariyappa, R.; Hiremath, K. M.; Dame, L.
2005BASI...33..364K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Period-brightness relationship in chromospheric bright points
Authors: Kariyappa, R.; Narayanan, A. Satya; Dame, L.
2005BASI...33...19K    Altcode:
  Chromospheric bright points are sites where intense heating takes
  place by 3-min period waves. A 35-min-long time series of photographic
  spectra obtained in CaII H-line on a quiet region at the center of the
  solar disk under high spatial, spectral, and temporal resolution at
  the Vacuum Tower Telescope (VTT) of the Sacramento Peak Observatory
  has been analyzed to show that the period of intensity oscillations
  associated with bright points in the interior of the supergranular
  cells is independent of their intensity enhancements. We find evidence
  for a constant period of oscillations in bright points, independent
  of their peak brightness, and different from the period of network
  oscillations. This suggests that the heating mechanism may be identical
  (by 3-min period waves) in any class of bright points while in the
  case of network elements it may be an entirely different mechanism (by
  5-7 min period waves). In addition, it is shown that the amplitudes of
  the main and the follower pulses of bright points decay exponentially
  with time and the decay rate is constant with their brightness in any
  class of bright points.

---------------------------------------------------------
Title: Solar full field interferometric imaging with 3 telescopes
Authors: Damé, Luc; Cladé, S.; Zhao, B.
2004ESASP.554..373D    Altcode: 2004icso.conf..373D
  For the last 7 years we have been developing a 3-telescopes breadboard
  of the SOLARNET imaging interferometer proposed to CNES (French
  National Space Agency) for a possible Space Mission as early as 2010
  (new start expected in 2006). After having been successfully tested in
  laboratory for phase control (up to λ/300) and interferometric direct
  imaging performances, the setup was moved to Meudon Observatory at
  the "Grand Sidérostat de Foucault" in 2000 for direct testing on
  the Sun. Following the implementation of an automatic guiding and
  dedicated fine pointing for each telescope (capable of one twentieth
  of an arcsec), the complete interferometric setup is now nearly ready
  to observe properly in a coordinated cophased and copointed mode and to
  acquire its first images. We report the progress achieved in developing
  the breadboard and its spectro-imaging capabilities (a subtractive
  double monochromator), and indicate what are the next possible steps
  and prospects of the SOLARNET program both on ground and in Space.

---------------------------------------------------------
Title: SOLARNET: the solution to the high resolution needs of
    solar physics
Authors: Dame, L.; Clade, S.; Malherbe, J. M.
2004cosp...35.3583D    Altcode: 2004cosp.meet.3583D
  Encounter missions like the Solar Orbiter have high resolution
  imaging goals in addition to the plasma measurements. If context,
  arcsec imaging, might be possible and useful to interpret the plasma
  observation, we will demonstrate that the thermal conditions near the
  Sun will prevent to achieve any of the higher resolution goals even
  by taking the most state-of-the-art solar telescope (carbon-carbon
  structure, SiC mirrors, etc.). A far better solution to fulfill the
  high resolution needs is the SOLARNET mission. SOLARNET is a medium
  size high resolution solar physics mission proposed to CNES for a new
  start in 2006 and a possible launch in 2010. Partnerships with Germany,
  Belgium, China and India are under discussion. At the center of the
  SOLARNET mission is a 3-telescopes interferometer of 1 meter baseline
  capable to provide 50 times the best ever spatial resolution achieved
  in Space with previous, current or even planned solar missions: 20
  mas - 20 km on the Sun in the FUV. The interferometer is associated
  to an on-axis subtractive double monochromator (imaging spectrograph)
  capable of high spectral (0.01 nm) and high temporal resolutions (50
  ms) on a field of view of 40 arcsec and over the FUV and UV spectral
  domains (from 117.5 to 400 nm). This will allow to access process
  scales of magnetic reconnection, dissipation, emerging flux and much
  more, from the high chromosphere to the low corona with emphasis on
  the transition zone where the magnetic confinement is expected to be
  maximum. A whole new chapter of the physics of solar magnetic field
  structuring and evolution will be opened. Launched by an Eurockot on a
  high altitude sun-synchronous non-eclipsing orbit, SOLARNET will also
  provide continuous observations at a sustained rate for Helioseismology
  and solar cycle studies. We review the scientific program of SOLARNET
  and its advantages (and complementarities) with an encounter type
  mission (probe or orbiter), describe the interferometer concept and
  design, present the first imaging results of the SOLARNET breadboard
  obtained at Meudon Observatory this spring and give a short overview
  of the mission aspects.

---------------------------------------------------------
Title: No link between the solar activity cycle and the diameter
Authors: Dame, L.; Cugnet, D.
2004cosp...35.3358D    Altcode: 2004cosp.meet.3358D
  We do not understand the physical mechanisms responsible for the solar
  irradiance cycle. Measurements of small variations in the solar diameter
  could have been a critical probe of the Sun 's interior stratification,
  telling us how and where the solar luminosity is gated or stored. We
  have reanalyzed the 7 years of filtregrams data (150 000 photograms
  and magnetograms) of the SOHO/MDI experiment. We used the maximum
  possible sampling compatible with full frame recording, carefully
  avoiding any suspicious filtregram. Going further than the previous
  analysis of 2 years of data by Emilio et al. (Ap. J. 543,1007, 2000),
  we better corrected for changes in optical aberrations and, along
  Turmon et al. (Ap. J., 568, 396, 2002), we reduced radius measurement
  errors by identifying active regions and avoiding radius measurements
  herein. We found that, within the limit of our noise level uncertainties
  (2 mas), the solar diameter could be constant over the half cycle
  investigated. Our results confirm the recent reanalysis of the 7 years
  of MDI data made by Antia (Ap. J. 590, 567, 2003), with a completely
  different method since using the ultra-precise frequency variation
  of the f-modes (fundamental modes linked to the diameter). He found
  (carefully removing the yearly Earth induced variations and avoiding
  the SOHO data gap of 1999) that the diameter is constant over the half
  solar cycle (radius variation are less than 0.6 km, 0.8 mas - nothing
  over noise level). Along Antia, we can conclude that: "If a careful
  analysis is performed, then it turns out that there is no evidence
  for any variation in the solar radius." There were no theoretical
  reasons for large solar radius variations and there is no observational
  evidence for them with consistent space observations. If changes exit,
  they are to be very small.

---------------------------------------------------------
Title: Non-variation of the solar diameter with the cycle: the end
    of a possible link between activity and diameter
Authors: Dame, L.; Cugnet, D.
2004cosp...35.3352D    Altcode: 2004cosp.meet.3352D
  We have reanalyzed the 7 years of filtregrams data (150 000 photograms
  and magnetograms) of the SOHO/MDI experiment. We used the maximum
  possible sampling compatible with full frame recording, carefully
  avoiding any suspicious filtregram. Going further than the previous
  analysis of 2 years of data by Emilio et al. (Ap. J. 543,1007, 2000),
  we better corrected for changes in optical aberrations and, along
  Turmon et al. (Ap. J., 568, 396, 2002), we reduced radius measurement
  errors by identifying active regions and avoiding radius measurements
  herein. We found that, within the limit of our noise level uncertainties
  (2 mas), the solar diameter could be constant over the half cycle
  investigated. Our results confirm the recent reanalysis of the 7 years
  of MDI data made by Antia (Ap. J. 590, 567, 2003), with a completely
  different method since using the ultra-precise frequency variation
  of the f-modes (fundamental modes linked to the diameter). He found
  (carefully removing the yearly Earth induced variations and avoiding
  the SOHO data gap of 1999) that the diameter is constant over the
  half solar cycle (radius variation are less than 0.6 km, 0.8 mas
  - nothing over noise level). Along Antia, we can conclude that:
  "If a careful analysis is performed, then it turns out that there
  is no evidence for any variation in the solar radius." There were no
  theoretical reasons for large solar radius variations and there is no
  observational evidence for them with consistent space observations.

---------------------------------------------------------
Title: SOLARNET: a high resolution mission to complement the ILWS
    programme
Authors: Dame, L.; Clade, S.; Malherbe, J. M.
2004cosp...35.3579D    Altcode: 2004cosp.meet.3579D
  SOLARNET is a medium size high resolution solar physics mission
  proposed to CNES for a new start in 2006 and a possible launch in
  2010. Partnerships with Germany, Belgium, China and India are under
  discussion. At the center of the SOLARNET mission is a 3-telescopes
  interferometer of 1 meter baseline capable to provide 50 times
  the best ever spatial resolution achieved in Space with previous,
  current or even planned solar missions: 20 mas - 20 km on the Sun in
  the FUV. The interferometer is associated to an on-axis subtractive
  double monochromator (imaging spectrograph) capable of high spectral
  (0.01 nm) and high temporal resolutions (50 ms) on a field of view of
  40 arcsec and over the FUV and UV spectral domains (from 117.5 to 400
  nm). This will allow to access process scales of magnetic reconnection,
  dissipation, emerging flux and much more, from the high chromosphere
  to the low corona with emphasis on the transition zone where the
  magnetic confinement is expected to be maximum. A whole new chapter
  of the physics of solar magnetic field structuring and evolution
  will be opened. The interferometer is complemented by several other
  instruments providing larger field of view and higher temperature
  (EUV-XUV coronal imaging) to define the context and extension of
  the solar phenomena. Helioseismology, a strong asset of SOHO, is
  also intended with both velocity and diameter measures, allowed by
  a non-eclipsing Sun synchronous orbit. The SOLARNET interferometer
  design results of an extensive laboratory demonstration program of
  interferometric imaging of extended objects. It started 10 years ago
  and culminates this year with the first interferometric observations
  (images) of the Sun at Meudon Observatory at the "Grand Siderostat
  de Foucault" with a complete 3 telescopes cophased interferometer
  representative of SOLARNET. We will review the scientific program of
  SOLARNET, describe the interferometer concept and design, present the
  first solar imaging results of the breadboard and give a short overview
  of the mission aspects.

---------------------------------------------------------
Title: Solar physics and interferometry mission (SPI)
Authors: Damé, L.; Derrien, M.
2002AdSpR..29.2061D    Altcode:
  This paper presents the scientific objectives of the Solar Physics and
  Interferometry Mission (SPI), describes succinctly the model payload and
  summarizes mission's issues. Novel instrumentation (interferometry) and
  clever mission design (small platform on low orbit with high telemetry
  and dedicated smaller platform on hexapod for permanently Sun-centered
  instruments) allow both spectral imaging and Helioseismology at very
  high spatial and temporal resolutions. Although not retained by ESA,
  this mission could become reality through NASA MIDEX and/or CNES
  PROTEUS opportunities as soon as 2007-2008.

---------------------------------------------------------
Title: Technologies for solar interferometry in space
Authors: Damé, L.; Derrien, M.; Kozlowski, M.; Perrot, S.; Preumont,
   A.
2002AdSpR..29.2075D    Altcode:
  This paper summarizes, on one part, the results of a 3-telescope
  breadboard used to demonstrate the cophasing and imaging capabilities
  of the Solar Imaging Interferometer, SOLARNET, of the Solar Physics
  and Interferometry Mission (SPI) and, on the other, possibilities for
  state-of-the-art recombination optics (molecular binding) and novel
  delay lines using magnetic bearing to achieve unprecedented cophasing
  quality and ease of interferometric recombination and imaging.

---------------------------------------------------------
Title: Preface
Authors: Damé, Luc; Marsch, Eckart
2002AdSpR..29.1997D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: PICARD: solar diameter measure and g-mode search
Authors: Damé, L.; Appourchaux, T.; Berthomieu, G.; Boumier, P.;
   Cugnet, D.; Gelly, B.; Provost, J.; Toutain, T.
2001ESASP.464..321D    Altcode: 2001soho...10..321D
  The PICARD microsatellite mission will provide 3 to 4 years simultaneous
  measurements of the solar diameter, differential rotation and
  solar constant to investigate the nature of their relations and
  variabilities. The major instrument, SODISM, is a whole Sun imaging
  telescope of Ø 110 mm which will deliver an absolute measure
  (better than 4 mas) of the solar diameter and solar shape. Now in
  Phase B, PICARD is expected to be launched by 2005. We recall the
  scientific goals linked to the diameter measurement with emphasis on the
  helioseismology g-mode interest, present the instrument optical concept
  and present design, and give a brief overview of the program aspects.

---------------------------------------------------------
Title: Results from a revisit to the K<SUB>2V</SUB> bright points
Authors: Sivaraman, K. R.; Gupta, S. S.; Livingston, W. C.; Damé,
   L.; Kalkofen, W.; Keller, C. U.; Smartt, R.; Hasan, S. S.
2000A&A...363..279S    Altcode:
  We have used pairs of temporally simultaneous CaII K-line
  spectroheliograms and magnetic area scans to search for spatial
  correlation between the CaII K<SUB>2V</SUB> bright points in the
  interior of the network and corresponding magnetic elements. We find
  that about 60% of the K<SUB>2V</SUB> bright points spatially coincide
  with magnetic elements of flux density &gt; 4 Mx cm<SUP>-2</SUP>. About
  25% of the K<SUB>2V</SUB> bright points with equally enhanced emission
  lie over bipole elements where the fields are &gt; 4 Mx cm<SUP>-2</SUP>
  for both polarity elements which merge and presumably cancel and
  result in low fields. The rest, 15%, of the bright points coincide
  with areas of fields &lt; 4 Mx cm<SUP>-2</SUP> which is the noise
  level set by us for the magnetic scans. When magnetic elements of
  opposite polarity merge and form bipoles, the associated K<SUB>2V</SUB>
  bright points show excess emission. Although such excess emission is a
  magnetic-field-driven phenomenon, the measured value of the field at the
  site of the bipole is typically low, and these cases would therefore be
  excluded in the count of coincidences of excess emission with excess
  magnetic fields. In our opinion, these cases of excess emission at
  the sites of the bipoles, as well as at the sites of fields &gt;
  4 Mx cm<SUP>-2</SUP>, are both instances of magnetic-field-related
  emissions. If the former are not taken into account as coincidences,
  the correlation will drop down and this might be interpreted as not an
  obvious correlation. Our present results, taking into account the low
  fields of merging bipoles, establish the association of K<SUB>2V</SUB>
  bright points with magnetic elements.

---------------------------------------------------------
Title: New High Resolution Observations of the Solar Diameter from
    Space and Ground with the Microsatellite Program PICARD
Authors: Damé, L.
2000JApA...21..135D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: PICARD: Solar Diameter, Irradiance and Climate
Authors: Damé, L.; Cugnet, David; Herse, Michel; Crommelynck,
   Dominique; Dewitte, Stevens; Joukoff, Alexandre; Ruedi, Isabelle;
   Schmutz, Werner; Wehrli, Christoph; Delmas, Christian; Laclare,
   Francis; Rozelot, Jean-Pierre
2000ESASP.463..223D    Altcode: 2000sctc.proc..223D
  No abstract at ADS

---------------------------------------------------------
Title: PICARD: simultaneous measurements of the solar diameter,
    differential rotation, solar constant and their variations
Authors: Damé, Luc; Hersé, Michel; Thuillier, Gérard; Appourchaux,
   Thierry; Crommelynck, Dominique; Dewitte, Steven; Joukoff, Alexandre;
   Fröhlich, Claus; Laclare, Francis; Delmas, Christian; Boumier, Patrick
1999AdSpR..24..205D    Altcode:
  PICARD is a CNES micro-satellite mission due for flight by the end
  of 2002, named after the name of a French astronomer who first
  observed with consistency the solar diameter changes during the
  Maunder minimum in the 16th century. It consists of two instruments
  measuring (i) the solar diameter and differential rotation, and (ii)
  the total solar irradiance. These quantities are fundamental for the
  understanding of the solar-Terrestrial relations, e.g. the influence
  of the Sun on the Earth's climate, and of the internal structure
  of the Sun. The continuous - or nearly continuous - viewing of the
  Sun from an appropriate orbit, the 5 minutes sampling rate and the
  very low noise measurements, will allow g-modes detection and precise
  diameter measurements besides accurately establishing the relationship
  between irradiance and diameter changes. Providing an absolute measure
  of the solar diameter to 1 milliarcsecond, PICARD is the first step
  towards instruments capable of accurate and perennial measurements,
  for the centuries to come, of the solar-terrestrial influence. The
  objectives of the mission, instrument capabilities, observing modes
  and performances are described.

---------------------------------------------------------
Title: High Resolution Solar Physics by Interferometry: SOLARNET
Authors: Damé, L.; Derrien, M.; Kozlowski, M.; Merdjane, M.
1998ESASP.417..109D    Altcode: 1998cesh.conf..109D
  No abstract at ADS

---------------------------------------------------------
Title: Laboratory and Sky Demonstrations of Solar Interferometry
    Possibilities
Authors: Damé, L.; Derrien, M.; Kozlowski, M.; Merdjane, M.
1998ESASP.417..345D    Altcode: 1998cesh.conf..345D
  No abstract at ADS

---------------------------------------------------------
Title: Low orbit high resolution solar physics with the solar
    interferometer
Authors: Damé, L.
1998AdSpR..21..295D    Altcode:
  Following several years of design studies of Solar Interferometers
  (mainly for Space Missions), we have reached a very complete and
  mature mechanical and optical concept, as well as a comprehensive image
  reconstruction scenario. Furthermore, we demonstrated recently, on a
  laboratory representative breadboard -- but also directly on the Sun --
  the feasibility and performances of the cophasing of two telescopes on
  extended objects. This definitively proves the validity of the pupil
  plane synchronous detection technique (applied to an extended object:
  the Sun) that we proposed and developed since 1988, These recent
  results really open the possibility to use and discover from solar
  interferometers either on ground or in Space. With a 1 meter baseline
  and 5 telescopes of 25 cm or so, permanent spatial resolution of 0.1”
  on a 30” field-of-view can be reached from the ground in the visible
  while 0.02” could be achieved in the far UV, from Space, all with an
  adjustable spectral bandwidth of 0.01 to 10 nm.

---------------------------------------------------------
Title: The MUST/3T Solar Interferometer: AN Interferometric Technology
    Testbed on the Iss
Authors: Damé, L.
1996ESASP.385..369D    Altcode: 1996ssu..conf..369D
  No abstract at ADS

---------------------------------------------------------
Title: Simultaneous UV and X-ray Observations of Coronal Bright Points
Authors: Bruner, M. E.; Nitta, N.; Wuelser, J. P.; Harvey, K.; Handy,
   B.; Dame, L.
1996AAS...188.8607B    Altcode: 1996BAAS...28..964B
  High resolution ultraviolet filtergrams recorded during the 1992 and
  1994 flights of the Solar Plasma Diagnostics Experiment (SPDE) sounding
  rocket payload revealed a number of coronal bright points that were
  simultaneously observed with the Yohkoh soft x-ray telescope. UV images
  made at 1550 Angstroms/, which include substantial contributions from
  the C IV resonance lines, reveal pairs of sources under the x-ray bright
  points; consistent with the conventional interpretation of the latter
  as un-resolved loops. The 1994 flight also recorded high resolution
  EUV images at 171 and 195 Angstroms/, corresponding to strong lines
  of Fe IX and Fe XII, respectively. Excellent correspondence was found
  between coronal bright points seen in these lines, which are formed at
  relatively low coronal temperatures (1 -- 2 x 10(6) k), and the 2 --
  5 x 10(6) k that typifies the Yohkoh SXT images. In this study, we
  use the Yohkoh database to study the temporal development of several
  coronal bright points both before and after each rocket flight in order
  to determine the stage of evolution of the sources at the epoch of the
  flight. The relationship between the plasma properties of the sources
  and their stages of evolution will be discussed.

---------------------------------------------------------
Title: Coordinated SPDE rocket, YOHKOH and ground observations of
    an emerging flux region and a filament
Authors: Damé, L.; Martic, M.; Brown, W. A.; Bruner, M. E.; Strong,
   K.; Suematsu, Y.; Tsuneta, S.; Schmieder, B.
1996AdSpR..17d.189D    Altcode: 1996AdSpR..17..189D
  During the first flight of the Solar Plasma Diagnostic Experiment
  (SPDE), May 12, 1992, we obtained UV filtergrams at high resolution
  (full Sun 0.82” spatial resolution in the 160 nm continuum, the
  CIV lines and Lyman alpha) with the Ultraviolet Filtergrap Camera
  (UVFC). Closely coordinated observations were obtained with the Soft
  X-ray Telescope (SXT) of the Yohkoh satellite and from dedicated ground
  programs in particular at Sacramento Peak, La Palma and Pic-du-Midi
  observatories. With this unique set of data we cover the solar
  atmosphere as a whole, from the temperature minimum to the high corona
  with essential steps in the chromosphere and transition region. After
  the necessary calibrations of the data set, we present the first results
  of the multitemperature development of an emerging flux region and of
  a filament that rapidly changed right during the rocket short lifetime.

---------------------------------------------------------
Title: SIMURIS: a UV and XUV Mission for high resolution solar physics
Authors: Damé, L.; Derrien, M.; Kozlowski, M.; Antonucci, E.;
   Ragazzoni, R.; Tondello, G.
1996AdSpR..17d.377D    Altcode: 1996AdSpR..17..377D
  Advances in electronics and servo-control allow to envisage extremely
  high spatial resolution observations of the Sun through the use of
  a compact array of phased telescopes. We present the SIMURIS Mission
  (Solar Interferometric Mission for Ultrahigh Resolution Imaging and
  Spectroscopy) which is the first to propose high resolution ultraviolet
  imaging coupled to high time and spectral resolutions through the
  use of an interferometric array of five 20 cm telescopes feeding a
  subtractive double monochromator tunable over a large spectral range
  and providing narrow band filtergrams. In addition to the ultraviolet
  imaging interferometer SIMURIS has soft X-ray and EUV imagers and
  spectrometers for complete coverage of the solar atmosphere.

---------------------------------------------------------
Title: Instrumental prospects in solar interferometric imaging.
Authors: Damé, L.; Derrien, M.; Kozlowski, M.; Ruillier, C.
1996joso.proc...52D    Altcode:
  The authors briefly recall the concepts of the Solar Interferometer,
  explain the constraints imposed by the measurement of a phase over
  extended objects and present the laboratory and sky results of the
  first solar interferometric experiment of cophasing.

---------------------------------------------------------
Title: Global Oscillations at Low Frequency from the SOHO Mission
    (GOLF)
Authors: Gabriel, A. H.; Grec, G.; Charra, J.; Robillot, J. -M.; Roca
   Cortés, T.; Turck-Chièze, S.; Bocchia, R.; Boumier, P.; Cantin, M.;
   Cespédes, E.; Cougrand, B.; Crétolle, J.; Damé, L.; Decaudin, M.;
   Delache, P.; Denis, N.; Duc, R.; Dzitko, H.; Fossat, E.; Fourmond,
   J. -J.; García, R. A.; Gough, D.; Grivel, C.; Herreros, J. M.;
   Lagardère, H.; Moalic, J. -P.; Pallé, P. L.; Pétrou, N.; Sanchez,
   M.; Ulrich, R.; van der Raay, H. B.
1995SoPh..162...61G    Altcode:
  The GOLF experiment on the SOHO mission aims to study the internal
  structure of the sun by measuring the spectrum of global oscillations in
  the frequency range 10<SUP>−7</SUP> to 10<SUP>−2</SUP> Hz. Bothp
  andg mode oscillations will be investigated, with the emphasis on
  the low order long period waves which penetrate the solar core. The
  instrument employs an extension to space of the proven ground-based
  technique for measuring the mean line-of-sight velocity of the viewed
  solar surface. By avoiding the atmospheric disturbances experienced
  from the ground, and choosing a non-eclipsing orbit, GOLF aims to
  improve the instrumental sensitivity limit by an order of magnitude
  to 1 mm s<SUP>−1</SUP> over 20 days for frequencies higher than
  2.10<SUP>−4</SUP> Hz. A sodium vapour resonance cell is used in
  a longitudinal magnetic field to sample the two wings of the solar
  absorption line. The addition of a small modulating field component
  enables the slope of the wings to be measured. This provides not only
  an internal calibration of the instrument sensitivity, but also offers a
  further possibility to recognise, and correct for, the solar background
  signal produced by the effects of solar magnetically active regions. The
  use of an additional rotating polariser enables measurement of the
  mean solar line-of-sight magnetic field, as a secondary objective.

---------------------------------------------------------
Title: Active phase stabilization at the I2T: implementation of the
    ASSI table
Authors: Robbe, Sylvie; Sorrente, Beatrice; Cassaing, Frederic;
   Rabbia, Yves; Rousset, Gerard; Dame, Luc; Cruzalebes, Pierre;
   Schumacher, Gerard
1994SPIE.2200..222R    Altcode: 1994aisi.conf..222R
  We present the Active Stabilization in Stellar Interferometry (ASSI)
  beam combining optical table which was installed on the 2- telescope
  interferometer (I2T) of the Observatoire de la Cote d'Azur in 1993. To
  achieve very high angular resolution, the 26- centimeter telescopes can
  be positioned along a 140-meter North- South baseline. The limiting
  magnitude of the instrument depends dramatically on its ability to
  stabilize the fringe pattern despite the atmospheric disturbances. The
  function of the ASSI table is to perform this task. Three adaptive
  mirrors are used. The first two are fine pointing mirrors which correct
  the fluctuations of the angle of arrival of the two wavefronts. The
  other corrects the optical path difference fluctuations between the
  two telescopes. These corrections, e.g. tip-tilt and piston phase, are
  required to obtain high precision visibility measurements. We present
  our first observing results obtained on bright stars that have allowed
  the evaluation of the ASSI table performance in image tracking.

---------------------------------------------------------
Title: Solar interferometric imaging from the moon
Authors: Dame, L.; Martic, M.; Porteneuve, J.
1994AdSpR..14f..49D    Altcode: 1994AdSpR..14...49D
  We present the concept of a Lunar Interferometer for Solar Physics. In
  particular we explain the rationale for a compact 2D array and we
  propose the use of a novel mechanical support structure based on linear
  mounting rods - these optimizing room and mass issues for transportation
  to the Moon.

---------------------------------------------------------
Title: Solar interferometry: space and ground instrumental prospects
Authors: Dame, Luc
1994SPIE.2200...35D    Altcode: 1994aisi.conf...35D
  Recent advances in electronics and fast computer control allow to
  envisage extremely high spatial resolution observations of the Sun
  through the use of a compact array of phased telescopes. Several
  space missions (SUN/SIMURIS, SUN-SV, MUST/SIMURIS) have been
  proposed in that respect and will be briefly presented. Prospects
  for use of the space techniques for a solar array on ground are also
  indicated. Independently from the different mission concepts, solar
  interferometric imaging presents a unique case in the domain of optical
  aperture synthesis since the field- of-view is extended (larger than
  the diffraction spot of a telescope) and because the high resolution
  structures are evolving very rapidly and are naturally complex (low
  fringe visibility). These severe constraints drive solar arrays'
  design towards `compact' configurations (i.e. in which the spatial
  frequencies plane is filled) and real-time `cophasing' (direct--
  hardware--zeroing of phase fluctuations by fine delay lines). They also
  influence the choice of the focal instrumentation which is optimum when
  using a subtractive double monochromator tunable over a large spectral
  range and providing narrow band filtergrams (up to 0.1 angstrom). We
  review the concepts and design issues of a solar interferometer and
  present numerical simulations and laboratory experiments of the system
  required to cophase an array of telescopes on a complex and extended
  field-of-view. Aperture configurations and image reconstruction are
  also discussed as well as the specific real-time metrology aspects of
  a ground array (atmospheric constraints derived from the performances
  evaluation of the ASSI Program).

---------------------------------------------------------
Title: The SIMURIS interferometric mission: Solar physics objectives
    and model payload
Authors: Dame, L.; Rutten, R. J.; Thorne, A. P.; Vial, J. C.
1994AdSpR..14d.167D    Altcode: 1994AdSpR..14..167D
  We describe the SIMURIS Mission with emphasis on the scientific goals
  and related capabilities of the major instruments of the model payload.

---------------------------------------------------------
Title: Actively cophased interferometry with SUN/SIMURIS
Authors: Dame, Luc
1993SPIE.1947..161D    Altcode:
  The Solar Ultraviolet Network (SUN) is an instrument based on
  interferometric concepts, and capable of observations with a spatial
  resolution of 0.013' (10 km) on the Sun, in the UV and visible
  wavelength ranges. In this paper we present results on fringe pattern
  acquisition and stabilization as performed on a Mach-Zehnder set up
  representative of the interferometer cophasing system. The system
  algorithm is based on 'white light' fringe tracking controlled in a
  reference interferometer by a synchronous detection. This servo-system
  drives a two-stages delay line for real-time compensation of the optical
  path delays. Acquisition capabilities and stability possibilities
  are investigated as a function of flux and noise levels. Being
  stabilized, actively cophased, and in a 'compact' configuration, the SUN
  interferometer possesses remarkable imaging capabilities allowing high
  resolution diffraction-limited imaging on an extended field of view
  of 6 X 6 arcsec(superscript 2). The dynamics of reconstructed images
  is superior to 400 for phase stabilities &gt;= (lambda) /6 and photon
  flux of approximately 10,000 ph s(superscript -1) pixel(superscript -1)
  (on average). The SUN instrument is part of the Solar Interferometric
  Mission for Ultrahigh Resolution Imaging and Spectroscopy (SIMURIS)
  which was proposed to ESA in the framework of the Next Medium Size
  Mission (M2) in November 1989, and which completed a First Phase of
  Study in the context of the Space Station in August 1991.

---------------------------------------------------------
Title: Golf: A resonance spectrometer for the observation of solar
    oscillations I) Numerical model of the sodium cell response
Authors: Boumier, P.; Dame, L.
1993ExA.....4...87B    Altcode:
  GOLF (Global Oscillations at Low Frequencies) is an instrument to study
  the line-of-sight velocity of the solar photosphere, to be flown on
  the SOHO satellite in 1995. It uses a sodium vapour cell in resonance
  scattering mode, in order to measure the absolute Doppler shift of
  the solar sodium absorption lines. We have developed a model of the
  resonance cell performance. We describe here the main characteristics
  of the model, and report the most important results concerning the
  performance of the cell and its dependance on temperature.

---------------------------------------------------------
Title: Multitemperature Observations of an Emerging Flux Region
Authors: Bruner, M. E.; Acton, L. W.; Brown, W. A.; Lemen, J. R.;
   Shine, R.; Strong, K. T.; Tarbell, T.; Dulk, G.; Tsuneta, S.; Bastian,
   T.; Dame, L.
1993BAAS...25.1179B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Observations of an Emerging Flux Region
Authors: Brown, W. A.; Acton, L. W.; Bruner, M. E.; Lemen, J. R.;
   Shine, R.; Strong, K. T.; Tarbell, T.; Dulk, G.; Tsuneta, S.; Bastian,
   T.; Dame, L.
1993BAAS...25Q1214B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Prospects for very-high-resolution solar physics with the
    Simuris interferometric mission.
Authors: Dame, L.; Martic, M.; Rutten, R. J.
1993ESASP1157..119D    Altcode: 1993srfs.book..119D
  Simuris - the Solar, Solar System, and Stellar Interferometric Mission
  for Ultra-high Resolution Imaging and Spectroscopy - employs advanced
  interferometric techniques. Its payload includes two major instruments,
  which are the Solar Ultraviolet Network (SUN), an interferometric
  array of four 20 cm telescopes on a 2 m baseline, and the Imaging
  Fourier-Transform Spectrometer (IFTS), which uses light from a 40 cm
  Gregory telescope. Both instruments have active pointing capabilities of
  3 mas stability, and in addition SUN has an active co-phasing control
  to 1/50th of a wavelength. EUV multi-layer telescopes complete the
  payload for diagnostics of the very-high-temperature plasma.

---------------------------------------------------------
Title: Stellar objectives of SIMURIS
Authors: Damé, L.; Coradini, M.; Foing, B.; Rutten, R. J.; Thorne,
   A.; Vial, J. C.
1993MmSAI..64..345D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: SIMURIS: High-Resolution Solar Physics
Authors: Rutten, R. J.; Dame, L.
1993ASPC...46..184R    Altcode: 1993mvfs.conf..184R; 1993IAUCo.141..184R
  No abstract at ADS

---------------------------------------------------------
Title: The SIMURIS interferometric mission: solar physics objectives
    and model payload (invited paper)
Authors: Damé, L.; Coradini, M.; Foing, B.; Rutten, R. J.; Thorne,
   A.; Vial, J. C.
1993MmSAI..64..333D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The SUN/SIMURIS interferometer.
Authors: Dame, L.
1992ESASP.354...71D    Altcode: 1992tsbi.rept...71D
  The author presents the Solar Ultraviolet Network (SUN), which is a
  four 20 cm diameter telescopes interferometer of 2 m baseline. SUN is
  the major instrument of the SIMURIS Mission now under study by ESA for
  a possible accommodation on the Space Station Freedom. SUN concepts and
  design will be reviewed with emphasis on the unique particularities
  of this cophased interferometer dedicated to imaging of complex and
  extended objects.

---------------------------------------------------------
Title: Study of an optimized configuration for interferometric
    imaging of complex and extended solar structures.
Authors: Dame, L.; Martic, M.
1992ESASP.354..201D    Altcode: 1992tsbi.rept..201D
  The authors present image reconstruction by optical aperture synthesis
  of complex and extended objects alike those to be observed with the
  Solar Ultraviolet Network. They show, in particular, the importance
  of a compact array when such observations are intended

---------------------------------------------------------
Title: The lunar interferometer for solar physics.
Authors: Dame, L.; Martic, M.; Porteneuve, J.; Schnur, G. F. O.
1992ESASP.354..123D    Altcode: 1992tsbi.rept..123D
  The author present the concept of a Lunar Interferometer for Solar
  Physics (LISP). In particular they explain the rationale for a compact
  2D array and they propose the use of a novel mechanical support
  structure based on linear mounting rods. These two conceptual choice
  optimize imaging capacities and room and mass issues for transportation
  to the Moon.

---------------------------------------------------------
Title: Model payload and system design of the SIMURIS interferometric
    mission
Authors: Dame, L.; Rutten, R. J.; Thorne, A. P.; Vial, J. C.
1992wadc.iafcZ....D    Altcode:
  SIMURIS (Solar, Solar System, and Stellar Interferometric Mission
  for Ultrahigh Resolution Imaging and Spectroscopy) has been proposed
  to ESA as a Mission in the context of the Space Station in November
  1989 in answer to the Call for the Next Medium Size Mission (M2). It
  has completed, since, an Assessment Study, and is now proceeding for
  a Phase A. SIMURIS employs advanced interferometric techniques. The
  payload includes two major instruments which are the Solar Ultraviolet
  Network (SUN), an interferometric array of four 20-cm telescopes on
  a 2-m baseline, and the Imaging Fourier Transform Spectrometer (IFTS)
  which uses light from a 40-cm Gregory telescope. Both instruments have
  active pointing capabilities of 3 milliarcsec stability, and SUN has,
  in addition, an active cophasing control to 1/50th of a wavelength. EUV
  multilayer telescopes complete the payload for diagnostics of the very
  high temperature plasma. The SIMURIS model payload will be described
  with emphasis on the system design of the interferometric aspects of
  the instruments.

---------------------------------------------------------
Title: The imaging Fourier transform spectrometer performance and
    tolerance analysis.
Authors: Kruizinga, B.; Snijders, B.; Braam, B. C.; Thorne, A. P.;
   Maxwell, J.; Dame, L.
1992ESASP.344..290K    Altcode: 1992spai.rept..290K
  An abstract and an outline of an analysis of the Imaging Fourier
  Transform Spectrometer (IFTS), one of the core instruments of SIMURIS
  (Solar Interferometric Mission for Ultrahigh Resolution Imaging
  and Spectroscopy), is given. The quality of the optical system
  (including diffraction effects and aberrations of the nominal system)
  were evaluated. The performance figures were determined in the course
  of the instrument design process. Detailed information on components
  and other instrumental considerations lead to a readjustment of some
  of the requirements. The tolerance analysis and its implications
  were addressed. The influence of component manufacturing errors,
  assembly and alignment errors, and environmental disturbances on the
  optical quality were evaluated. The quality of the instrument including
  tolerances was determined in terms of the following: spot sizes in the
  detector, wavefront errors of interfering beams, pointing errors, and
  accuracy of the selected center wavelength. For each of these aspects
  the contributing optical components were identified. The permissable
  error budget was distributed over these components. The component
  tolerances were calculated.

---------------------------------------------------------
Title: Solar Physics and Astrophysics at Interferometric Resolution
Authors: Dame, L.; Guyenne, T. -D.
1992ESASP.344.....D    Altcode: 1992spai.rept.....D
  No abstract at ADS

---------------------------------------------------------
Title: SUN: the Solar Ultraviolet Network.
Authors: Dame, L.
1992ESASP.344..171D    Altcode: 1992spai.rept..171D
  The Solar Ultraviolet Network (SUN) is a space interferometer especially
  designed to observe the solar fine structure from the photosphere
  to the corona. It is a "compact" optical interferometer formed with
  four telescopes of 20 cm diameter distributed non-redundantly on
  a linear baseline of 2 meters. In addition to its intrinsic high
  spatial resolution (10 km on the Sun at λ = 120 nm), SUN has an
  elaborated focal plane instrument providing 6 simultaneous images
  of high spectral resolution and tunable from the far UV to the near
  IR. The compact array configuration, the cophased recording of fringes
  and the spectral properties of the double monochromator of SUN, allow
  interferometric imaging of the complex and extended solar structures
  with exceptional detail.

---------------------------------------------------------
Title: Solar physics and astrophysics at interferometric
    resolution. Proceedings.
Authors: Dame, L.; Guyenne, T. D.
1992spaa.book.....D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The imaging Fourier transform spectrometer optical design.
Authors: Kruizinga, B.; Snijders, B.; Braam, B. C.; Thorne, A. P.;
   Maxwell, J.; Dame, L.
1992ESASP.344..288K    Altcode: 1992spai.rept..288K
  An abstract and an outline of a paper on the optical design of the
  Imaging Fourier Transform Spectrometer (IFTS), one of the two main
  instruments of SIMURIS (Solar Interferometric Mission for Ultrahigh
  Resolution Spectroscopy) is presented. The following were studied:
  the modes of operation, based on the scientific requirements; the
  preliminary design of the telescope and the pointing system; a design
  of one of the prefilters, the subtractive double monochromator;
  the implementation of the FI and the imaging camera; photometry
  and the detection system; the instruments housing, mechanisms, and
  other mechanical aspects. The optimum quality of the entire system
  was determined by an extensive ray tracing analysis. A preliminary
  outline of the instrument's mechanical structure was generated.

---------------------------------------------------------
Title: Interferometric imaging with the Solar Ultraviolet Network.
Authors: Dame, L.; Cornwell, T. J.
1992ESASP.344..185D    Altcode: 1992spai.rept..185D
  Extensive simulations have been performed to investigate the image
  reconstruction potential of the Solar Ultraviolet Network. They
  establish that excellent images are obtained with compact optical
  arrays despite errors in visibility data caused by photon noise, beams'
  mispointing and residual phase errors. Imaging fidelity in optical
  interferometry, and with emphasis on extended objects, is a complex
  function of flux level, source complexity, recombination errors,
  and spatial frequency coverage of the so-called u,v plane. "Holes"
  in the u,v coverage would result in artifacts and in a significant
  degradation of the quality of the complex and extended images which
  could be reconstructed from the data.

---------------------------------------------------------
Title: Prospects with SIMURIS.
Authors: Dame, L.; Rutten, R. J.
1992ESASP.344...21D    Altcode: 1992spai.rept...21D
  The authors give an introductory overview of the SIMURIS payload by
  briefly presenting its goals and concepts.

---------------------------------------------------------
Title: Demonstration and performances of real-time fringe tracking:
    a step towards cophased interferometers.
Authors: Dame, L.
1992ESASP.344..277D    Altcode: 1992spai.rept..277D
  Imaging of complex and extended objects by the Solar Ultraviolet
  Network (SUN) require a real-time monitoring of the coalignment and
  cophasing functions of the interferometer. The cophasing of the input
  beams, i.e. the equalization (zero-ing) of the optical path delays,
  is specific to interferometry, and is required to high precision if
  diffraction limited imaging with the interferometer is expected. The
  author reports preliminary results on fringe pattern acquisition and
  stabilization as performed on a Mach-Zehnder set up representative of
  the interferometer cophasing system. The system algorithm is based on
  "white light" fringe tracking controlled in a reference interferometer
  by a synchronous detection. This servo-system drives a two-stages delay
  line for realtime compensation of the optical path delays. Acquisition
  capacities and stability possibilities are investigated as a function
  of flux and noise levels.

---------------------------------------------------------
Title: Laboratory Demonstration of Realtime Monitoring of a Two-Beam
    Interferometer by a Synchronous Detection Technique
Authors: Dame, L.
1992ESOC...39.1169D    Altcode: 1992hrii.conf.1169D
  No abstract at ADS

---------------------------------------------------------
Title: Imaging with a Compact Optical Interferometer - Influence of
    Photon Noise Pointing and Phase Errors on Image Dynamic
Authors: Dame, L.; Cornwell, T. J.
1992ESOC...39..815D    Altcode: 1992hrii.conf..815D
  No abstract at ADS

---------------------------------------------------------
Title: Design Rationale of the Solar Ultraviolet Network / Sun
Authors: Dame, L.; Acton, L.; Bruner, M. E.; Connes, P.; Cornwell,
   T. J.; Curdt, W.; Foing, B. H.; Hammer, R.; Harrison, R.; Heyvaerts,
   J.; Karabin, M.; Marsch, E.; Martic, M.; Mattic, W.; Muller, R.;
   Patchett, B.; Roca-Cortes, T.; Rutten, R. J.; Schmidt, W.; Title,
   A. M.; Tondello, G.; Vial, J. C.; Visser, H.
1992ESOC...39..995D    Altcode: 1992hrii.conf..995D
  No abstract at ADS

---------------------------------------------------------
Title: TRC 4: Correlation of the Tmin fine structure with the
    chromospheric bright points
Authors: Martic, Milena; Dame, Luc; Bruner, M. E.; Foing, Bernard H.
1991AdSpR..11e.241M    Altcode: 1991AdSpR..11..241M
  Simultaneous ground based observations in the Ca II K<SUB>2V</SUB>
  line and high resolution UV filtergrams (at λ160 nm) obtained during
  the 4th rocket flight of TRC (Transition Region Camera) were used for
  comparative studies of the fine structure in active regions, network,
  and supergranulation cells interior. In this paper we report similar
  time evolution and spatial correspondence between chromospheric cell
  bright points and continuum emission form the solar Tmin region. These
  results support the existence of a standing wave phenomena in the
  cell interiors.

---------------------------------------------------------
Title: A solar interferometric mission for ultrahigh resolution
imaging and spectroscopy: SIMURIS
Authors: Damé, L.; Acton, L.; Bruner, M.; Connes, P.; Cornwell, T.;
   Foing, B. H.; Heyvaerts, J.; Lemaire, P.; Martić, M.; Muller, R.;
   Porteneuve, J.; Roca Cortés, T.; Riehl, J.; Rutten, R.; Séchaud,
   M.; Smith, P.; Thorne, A. P.; Title, A. M.; Vial, J. -C.; Visser,
   H.; Weigelt, G.
1991AdSpR..11a.383D    Altcode: 1991AdSpR..11..383D
  SIMURIS is an interferometric investigation of the very fine structure
  of the solar atmosphere from the photosphere to the corona. It was
  proposed to ESA /1/, November 30 1989, for the Next Medium Size
  Mission - M2, and accepted in February 1990 for an Assessment Study
  in the context of the Space Station. The main scientific objectives
  will be outlined, and the ambitious model payload featuring the Solar
  Ultraviolet Network (SUN), a 2 m long monolithic array of 4 telescopes
  of Ø20 cm, and the Imaging Fourier Transform Spectrometer (IFTS),
  an UV and Visible Imaging Fourier Transform Spectrometer coupled to
  a Ø40 cm Gregory, described.

---------------------------------------------------------
Title: Solar physics at ultrahigh resolution from the space station
    with the Solar Ultraviolet Network (SUN)
Authors: Damé, L.; Acton, L.; Bruner, M.; Connes, P.; Cornwell,
   T.; Foing, B.; Heyvaerts, J.; Lemaire, P.; Martić, M.; Muller, R.;
   Roca Cortés, T.; Riehl, J.; Rutten, R.; Title, A. M.; Vial, J. -C.;
   Visser, H.; Weigelt, G.
1991AdSpR..11e.267D    Altcode: 1991AdSpR..11..267D
  The SUN experiment is a UV and visible Space Interferometer aimed at
  ultra-high resolution in the solar atmosphere. It has been proposed
  to ESA as part of the SIMURIS Mission Proposal which has recently
  been accepted for an Assessment Study in the framework of the
  Space Station. The 4 × 20 cm telescopes of the SUN linear array are
  non-redundantly placed to cover a 2 m baseline, and the instrument makes
  full use of stabilized interferometry potential, the 4 telescopes being
  co-aligned and co-phased on a reference field on the sun. After a brief
  outline of the scientific objectives, the concept of the instrument
  is described, and its image reconstruction potential is illustrated.

---------------------------------------------------------
Title: Preliminary performance of a 4-point resonance scattering
    experiment to access long-period global oscillations from space
Authors: Boumier, P.; Bocchia, R.; Damé, L.; Martic, M.; Pallé,
   P.; van der Raay, H. B.; Robillot, J. M.; Roca Cortés, T.
1991AdSpR..11d.199B    Altcode: 1991AdSpR..11..199B
  The first data of a SOHO-GOLF type instrument are presented
  hereafter. The slopes of the solar sodium lines profiles D1 and
  D2, and their variations with the excursion of the working point
  are shown. Two methods of determining the oscillation velocity are
  compared, one usually used with 2-point spectrometers and one using
  the 4-point information. We show that the second method gives spectra
  which are significantly less noisy in the very low frequency range
  (up to 300 μHz). For higher frequencies, terrestrial atmospheric
  fluctuations alter the measurement, and as far as ground based
  instruments are concerned, the 4-point method loses its efficiency
  if the magnetic modulation commutation time (in our case 20 seconds)
  is not significantly reduced.

---------------------------------------------------------
Title: SIMURIS: Solar, Solar System and Stellar Interferometric
    Mission for Ultrahigh Resolution Imaging and Spectroscopy
Authors: Coradini, M.; Dame, L.; Foing, B.
1991ssss.book.....C    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Rocket observations and modelling of flux-tubes
Authors: Foing, Bernard H.; Dame, Luc; Martic, Milena
1991AdSpR..11e.245F    Altcode: 1991AdSpR..11..245F
  The solar observations at high angular resolution have led to the
  discovery that the solar magnetic field is structured in filamentary
  fields at the photospheric level. Manifestations of these fluxtubes can
  be diagnosed with EUV images (with the Transition Region Camera Rocket
  Experiment, TRC) at 220nm in the middle photosphere, at 160nm in the
  temperature minimum region or in the Ly alpha and C IV lines formed
  at temperatures 20 000K and 100 000K in the transition region. In the
  frame of a thin flux tube modelling of the TRC data, the vertical
  variation of tube parameters and the conditions for thermalisation
  in the upper photosphere are discussed. We consider constraints from
  EUV observations on current models of flux-tubes and coronal loops
  including non LTE calculations, dynamic and magnetic effects.

---------------------------------------------------------
Title: Possibilities for quantification and reduction of solar
    velocity noise induced by active regions
Authors: Ulrich, R. K.; Dame, L.; Martic, M.
1991AdSpR..11d.203U    Altcode: 1991AdSpR..11..203U
  Active regions on the solar surface induce a velocity signal in a
  variety of measurements of doppler shifts including the integrated
  sunlight measurements made by resonance cells using the NaD lines. These
  signals may be an important limitation on the ability of the GOLF
  investigation to detect solar g-modes. Although the power spectrum of
  this velocity signal is not well studied, it is in principal possible
  to develop techniques based on other properties of the spectral line
  to isolate the active region induced component and remove it from
  the observed velocity. This paper describes efforts to develop such
  a method and verify its utility using ground-based measurements.

---------------------------------------------------------
Title: The Solar Ultraviolet Network (SUN) (With 3 Figures)
Authors: Damé, L.
1991mcch.conf...73D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: SIMURIS: a High Resolution Solar Physics Interferometric
    Mission in Answer to the Chromospheric and Coronal Heating Problem
    (With 2 Figures)
Authors: Damé, L.
1991mcch.conf...66D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Possible scenarios of coronal loops reconnection/heating
    processes to be observed at high spatial resolution
Authors: Dame, L.; Heyvaerts, J.; Foing, B. H.
1991AdSpR..11a.327D    Altcode: 1991AdSpR..11..327D
  Recent improvements in interferometric techniques could allow to
  achieve 0.01 arcsec angular resolution on the Sun, i.e. 10 km. Such
  a high resolution is of direct interest to understand the coronal
  loop structure since current observations at low resolution cannot
  distinguish between major dissipation/heating theories which all involve
  very small scale dissipating processes. Three simplified scenarios of
  loop instabilities are investigated in this paper and the resulting fine
  structure and contrast that they might induce on observable quantities
  (temperature, density) are deduced.

---------------------------------------------------------
Title: The imaging fourier transform spectrometer for the SIMURIS
    mission
Authors: Foing, B. H.; Dame, L.; Thorne, A. P.; Lemaire, P.
1991AdSpR..11a.387F    Altcode: 1991AdSpR..11..387F
  The Solar Interferometric Mission for Ultrahigh Resolution Imaging and
  Spectroscopy (SIMURIS) is an interferometric investigation in space
  at ultraviolet and visible wavelengths aimed at reconnaissance of
  solar features at angular scales from 0.3 to 0.01 arcsec. The Imaging
  Fourier Transform Spectrometer (IFTS) is, with the Solar Ultraviolet
  Network (SUN), one of the core instruments of the proposed SIMURIS
  mission. It consists of a 40 cm Gregory telescope feeding a double
  grating pre-dispersive spectrometer before entering a Fourier transform
  spectrometer for a field of 10 × 10 arcsec<SUP>2</SUP> at 0.3 arcsec
  resolution. The SIMURIS/IFTS requires upgrading of existing FTS down
  to 120 nm, with imaging capabilities. For the IFTS imaging a detector
  with fast readout must be used. There are also demanding constraints
  on the real time processing, and the subsequent important data rate,
  and requirements on an upgraded instrument pointing system (IPS),
  within the resources and capabilities of the Space Station.

---------------------------------------------------------
Title: Laboratory experiments on fringe-pattern acquisition and
    stabilization
Authors: Dame, Luc; Beal, Denis; Sorrente, Beatrice; Prieto, Eric
1990SPIE.1237..639D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Optical recombination tolerances of the Solar Ultraviolet
    Network
Authors: Dame, Luc; Moreau, Bernard G.; Riehl, Jacques
1990SPIE.1237..654D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Magnetic Field Modulation Issues for Improving Global Solar
    Oscillation Measurements from Space
Authors: Damé, L.; Ulrich, R. K.; Martić, M.; Boumier, P.
1990LNP...367..265D    Altcode: 1990psss.conf..265D
  The measurement of global oscillations of the Sun from space will
  provide the ultimate means by which we will assess the existence, and
  hopefully observe some of the expected gravity modes. The SOHO-GOLF
  experiment, with a 4-point measurement in the line profile (resonance
  scattering method with a variable magnetic field applied to a sodium
  cell), may be able to distinguish between magnetic effects and true
  velocities. In this paper we characterize the effects of the magnetic
  fields and active regions on all aspects of the solar D lines in
  order to determine the best way to extract this signal from the solar
  background noise. These preliminary findings are then used to quantify
  the precision requirements for the GOLF Magnetic Field Modulation
  measurement method.

---------------------------------------------------------
Title: High Resolution Solar Physics from the Space Station with
Interferometric Techniques: The Solar Ultraviolet Network (SUN) -
    Instrument &amp;Objectives
Authors: Damé, L.; Acton, L.; Bruner, M.; Connes, P.; Cornwell, T.;
   Foing, B.; Heyvaerts, J.; Jalin, R.; Lemaire, Ph.; Martic, M.; Moreau,
   B.; Muller, R.; Roca Cortés, T.; Riehl, J.; Rutten, R.; Title, A. M.;
   Vial, J. -C.; Visser, H.; Weigelt, G.
1990PDHO....7..262D    Altcode: 1990dysu.conf..262D; 1990ESPM....6..262D
  No abstract at ADS

---------------------------------------------------------
Title: Solar Ultraviolet Network: an interferometric investigation
    of the fundamental solar astrophysical scales
Authors: Dame, Luc; Moreau, Bernard G.; Cornwell, Timothy J.;
   Visser, H.; Title, Alan M.; Acton, Loren W.; Aime, Claude; Braam,
   Bart M.; Bruner, Marilyn E.; Connes, Pierre; Faucherre, Michel; Foing,
   B. H.; Haisch, Bernhard M.; Hoekstra, Roel; Heyvaerts, Jean; Jalin,
   Rene; Lemaire, Philippe; Martic, Milena; Muller, R.; Noens, J. C.;
   Porteneuve, Jacques; Schulz-Luepertz, E.; von der Luehe, Oskar
1989SPIE.1130..126D    Altcode:
  The Solar UV Network (SUN) presently proposed is an interferometric
  system, based on the principles of stabilized interferometry, which
  will be capable of solar observations with spatial resolutions better
  than 0.013 arcsec. SUN will consist of four 20-cm diameter telescopes
  aligned nonredundantly on a 2-m baseline. SUN is judged to be ideally
  deployable by the NASA Space Station, if implemented on a pointing
  platform whose performance is of the order of the Instrument Pointing
  System flown on Spacelab 2. The compact, nonredundant configuration of
  SUN's telescopes will allow high-resolution imaging of a 2 x 2 arcsec
  field on the solar disk.

---------------------------------------------------------
Title: ASSI: an optimized fringe tracking stellar interferometer.
Authors: Damé, L.; Decaudin, M.; Faucherre, M.; Boutry, P.; Martic,
   M.; Coron, N.; Bourbon, M.; Carteron, J. -R.; Dambier, G.; Jegoudez,
   G.; Haro, J.; Lagardère, H.; Leblanc, J.; Lepeltier, J. P.; Lizambert,
   C.; Bourdet, G.; Moreau, B.; Jalin, R.; Séchaud, M.; Rabbia, Y.;
   Schumacher, G.; Dugué, M.
1989SPIE.1114..225D    Altcode:
  The authors present the ASSI (Active Stabilization in Stellar
  Interferometry) interferometric experiment presently under realisation
  for use with the 2-Telescope interferometer of CERGA (I2T). They
  review the principles and expected performances of the system and,
  in particular, the real time, flux optimized, fringe tracking system
  that they developed using synchronous detection technique on cooled
  silicium diodes in the near infrared.

---------------------------------------------------------
Title: High Resolution Diagnostic of the Mesocells in the Solar
    Temperature Minimum Region
Authors: Martič, M.; Damé, L.
1989ASIC..263..207M    Altcode: 1989ssg..conf..207M
  No abstract at ADS

---------------------------------------------------------
Title: The GOLF helioseismometer on board SOHO.
Authors: Dame, Luc
1988ESASP.286..367D    Altcode: 1988ssls.rept..367D
  The authors present the GOLF (Global Oscillations at Low Frequencies)
  investigation that was recently accepted on board the SOHO satellite
  of the ESA/NASA Solar Terrestrial Science Programme. The GOLF
  instrument is an improved version of ground based instruments using
  the resonant-scattering spectrometric technique to measure global
  velocities of the Sun and Stars. It has the unique capability of a 4
  points measurement in the line profile for both the global velocity
  and magnetic field measurements.

---------------------------------------------------------
Title: GOLF: Simulations of the re-emission of the resonance cell.
Authors: Boumier, P.; Dame, Luc
1988ESASP.286..425B    Altcode: 1988ssls.rept..425B
  Applied to the GOLF (Global Oscillations at Low Frequencies)
  helioseismometric instrument to be flown on SOHO, the authors
  analyse the re-emission process in the resonance cell, heart of
  the instrument. The cell is filled with a sodium vapor and absorbs
  selectively in the two sodium lines D1 and D2. The authors simulated
  the different influence of the physical parameters (cell geometry,
  temperature) and report herein the temperature analysis which allow
  to constrain the nominal temperature working point and the required
  stability, as a function of the operational conditions (orbital
  velocity variation).

---------------------------------------------------------
Title: GOLF: Global Oscillations at Low Frequencies for the SOHO
    mission
Authors: Gabriel, A. H.; Bocchia, R.; Bonnet, R. M.; Cesarsky, C.;
   Christensen-Dalsgaard, J.; Dame, L.; Delache, Ph.; Deubner, F. L.;
   Foing, B.; Fossat, E.
1988sohi.rept...13G    Altcode:
  The GOLF (global oscillations at low frequencies) SOHO (solar
  heliospheric observatory) mission is described. It aims to study
  the internal structure of the Sun by measuring the spectrum of free
  global oscillations. GOLF will measure both p and g mode oscillations,
  with emphasis on low order long period waves which penetrate the
  solar core. The instrument aims to measure frequencies between 10-7
  and 6 10-3 Hz, with a sensitivity of 1 mm/s. The method involves an
  extension to space of the ground based technique for measuring the mean
  line-of-sight velocity of the solar surface. A sodium vapor resonance
  scattering filter is used in a longitudinal magnetic field to sample the
  two wings of the solar absorption line. The use of a modulating magnetic
  field provides a continuous internal calibration of the sensitivity. By
  adding an additional rotating polarizer, measurements are also made
  of the average solar magnetic field. Efforts are made to correct the
  data for the spurious effects caused by solar magnetic active regions.

---------------------------------------------------------
Title: Active stabilization in stellar interferometry (ASSI):
    progress report on the two bandpass fringe tracking interferometer.
Authors: Damé, L.; Faucherre, M.; Bourdet, G.; Decaudin, M.; Jegoudez,
   G.; Rabbia, Y.; Aubry, G.; Passedat, G.
1988ESOC...29.1079D    Altcode: 1988hrii.conf.1079D
  The authors report the progress done on the new interferometric
  table presently beeing built at LPSP for use with the 2-telescope
  interferometer of CERGA (I2T). The instrument is featuring an accurate
  fine pointing (shared quad-cell type ecartometer set up) and a real
  time, flux optimized, white light fringe tracking using the synchronous
  detection technique. After a short justification of the adopted
  technique, the authors review some of the particularities of their
  apparatus, their need, and the gain in performances that they provide.

---------------------------------------------------------
Title: Oscillatory Properties of Meso-Scale Intensity Structures at
    Chromospheric Level
Authors: Dame, L.; Martic, M.
1988IAUS..123..433D    Altcode:
  The authors show the evidence at chromospheric level (Ca II K line)
  of meso structures, "mesocells", reminiscent of the mesogranulation by
  their spatial size (8 Mm). These cells present very regular oscillations
  in intensity, preferably in the 3 - 5 min period range, and it is shown
  that the phase of the sustaining wave extends smoothly (coherently)
  over the mesocell area.

---------------------------------------------------------
Title: Tilt correction in stabilized interferometry: difficulties
    and remedies.
Authors: Faucherre, M.; Damé, L.; Decaudin, M.; Boutry, P.; Chirouze,
   M.; Jegoudez, G.; Lagardère, H.; Rabbia, Y.; Terrier, G.; Vakili, F.
1988ESOC...29.1093F    Altcode: 1988hrii.conf.1093F
  Real-time tilt correction proposed for the I2T at CERGA will be
  operationnal in June 88. The construction of this active tracking system
  raised some interesting questions that the authors state in this paper,
  together with appropriate solutions. They focus here on problems common
  to most stellar interferometers: how to get a constant magnification
  for pupil image and pupil-star distance whatever the baseline? How to
  measure and minimize path delays introduced by tilt correction mirrors
  or other moving elements? The authors end up with a discussion on
  field rotation compensation and its implication on the optical design.

---------------------------------------------------------
Title: Rocket flight observations of the meso-scale structure in
    the temperature minimum region
Authors: Martic, M.; Dame, L.
1988AdSpR...8g.173M    Altcode: 1988AdSpR...8..173M
  A time sequence of high resolution images, obtained during the last
  rocket flight of the Transition Region Camera, was used to make
  a detailed study of the mesostructures in the Temperature Minimum
  Region. In our previous investigations we showed that meso-scale
  structures of 8 Mm spatial size observed in the chromosphere (Ca II K
  line) possess a characteristic oscillatory behaviour. Here, we present
  a new evidence of large amplitude intensity variations with a clearly
  defined 3 min. oscillation period involving all the mesocells of 105
  × 105 arcsec<SUP>2</SUP> field on the quiet sun.

---------------------------------------------------------
Title: Performances of an actively stabilized stellar interferometer
(ASSI): faint magnitudes, low fringe contrast measurements and
    operationality
Authors: Dame, L.; Faucherre, M.
1987ESASP.273..205D    Altcode: 1987ois..work..205D
  The authors describe the performances of a new approach to long baseline
  Michelson interferometry using a real time active stabilization of
  the central fringe position ("fringe tracking"). In this approach the
  monitoring function (star pointing and optical path delay information)
  is clearly dissociated (and flux optimized) from the scientific analysis
  function, in which time integration and stability are favored, for
  evident reasons of precision on the fringe contrast measurement.

---------------------------------------------------------
Title: A test-bed for space interferometry: SPI
Authors: Faucherre, M.; Dame, L.; Stachnik, R. V.; Traub, W. A.
1987ESASP.273..197F    Altcode: 1987ois..work..197F
  The Space Platform Interferometer (SPI), a 20-m two-mirror Michelson
  interferometer, which can reach magnitude 14 at UV and visible
  wavelengths, is described. The SPI is attached to a platform serviced
  from the space station. In addition to its ability to produce unique
  science in the UV, SPI is intended to demonstrate the feasibility
  of larger projects in the field. Dynamical behavior of the structure
  in the gravity gradient environment and fringe stabilization at low
  photon rate are studied by picking up an adjacent bin (in the near
  IR) on the same object and using it to track the white light fringe
  in a separate differential interferometer. The same subsystem also
  corrects for tilt. Active control of critical parameters ensures
  optical rigidity. Performances are evaluated in low orbit.

---------------------------------------------------------
Title: Diagnostics of solar coronal loops at interferometric angular
    resolution
Authors: Foing, B. H.; Faucherre, M.; Dame, L.
1987ESASP.273..217F    Altcode: 1987ois..work..217F
  The advent of very high angular resolution (equivalent to 20 km on the
  sun) for extreme ultraviolet observations would allow to diagnose the
  fine structure in density and temperature of solar coronal loops. In the
  framework of the variety and uncertainties of the existing theoretical
  models of loops, the high angular resolution is of particular importance
  to estimate the filling factor of loops by hot and cool material, to
  measure radial gradients of temperature and density, to observe flows,
  spatiotemporal evolution due to heating mechanisms and interaction
  between loops.

---------------------------------------------------------
Title: Solar interferometry with a 4-aperture non-redondant and
    stabilised network
Authors: Dame, L.; Aime, C.; Faucherre, M.; Heyvaerts, J.
1987ESASP.273..189D    Altcode: 1987ois..work..189D
  The design of a solar interferometer is intrinsically complex since
  many requirements, often found separately, and difficult by themselves,
  are brought together: UV spectral range, limb observations, resolved
  structures (low contrast) and time resolution. The stabilized
  interferometry technique, applied to a non-redundant array of 4
  telescopes, provides an elegant solution to those complex problems.

---------------------------------------------------------
Title: Inversion of line profile disturbances - A nonlinear method
    applied to solar CaII lines
Authors: Mein, P.; Mein, N.; Malherbe, J. M.; Dame, L.
1987A&A...177..283M    Altcode:
  Thermodynamical disturbances in the solar atmosphere can be deduced from
  observations of line profiles. The authors propose a non-linear method
  based on Fourier analysis: each profile is converted into a "double
  profile" for a fast convergence of Fourier expansions. Disturbances
  of Fourier coefficients are connected theoretically with physical
  disturbances by second order developments. Temperature and velocity
  fluctuations are derived from a least square inversion of these
  developments. The authors apply this method to a time sequence of
  high resolution profiles of the Ca II 3968 Å line. The accuracy of
  the results is discussed. The enhanced blue peaks occurring in the
  asymmetric profiles are interpreted as downward velocity gradients,
  associated with temperature excesses.

---------------------------------------------------------
Title: Observation and Oscillatory Properties of Mesostructures in
    the Solar Chromosphere
Authors: Dame, L.; Martic, M.
1987ApJ...314L..15D    Altcode:
  Two-dimensional filtergrams of a 90 x 90-arcsec solar field, obtained
  with time resolution 12 s and spatial resolution 1 arcsec using a
  Halle birefringent filter (bandwidth 60 pm) centered on the blue peak
  of the Ca II K line and a CCD array on the Vacuum Tower Telescope at
  Sacramento Peak Observatory in a 20-min observing run on November 11,
  1983, are presented and analyzed. Cells of extent about 8 Mm (i.e.,
  on the scale of mesogranulation) are observed and found to exhibit
  significant intensity variations of period 3-5 min, the phase cells
  determined by Fourier analysis being of about the same size as the
  observed structures. The possibility that mesogranulation may be
  closely related to the 5-min solar oscillation is discussed.

---------------------------------------------------------
Title: Structures fines chromosphériques: nouveaux résultats de
    la caméra de la région de transition.
Authors: Foing, B. H.; Dame, L.; Vial, J. C.; Gouttebroze, P.; Martic,
   M.; Bonnet, R. M.
1987JAF....29...15F    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: La haute résolution en physique solaire: perspectives pour
    l'avenir.
Authors: Damé, L.; Foing, B.; Vial, J. C.
1987JAF....29...16D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Interférométrie stellaire stabilisée: une approche nouvelle
    plus performante et plus précise.
Authors: Dame, L.; Bourdet, G.; Faucherre, M.
1987JAF....29Q..15D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: XSST/TRC rocket observations of 13 July 1982 flare.
Authors: Foing, B. H.; Bonnet, R. M.; Dame, L.; Bruner, M.; Acton,
   L. W.; Brown, W. A.
1986lasf.conf..319F    Altcode: 1986lasf.symp..319F
  The authors analyse the UV filtergrams of the 13 July
  1982 solar flare, taken by the Transition Region Camera,
  during the third flight of the joint Lockheed/LPSP rocket
  experiment XSST/TRC. From the calibrated intensities of the flare
  components, they estimate directly the Lyα line flux (from 230 to
  650×10<SUP>3</SUP>erg cm<SUP>-2</SUP>s<SUP>-1</SUP>sr<SUP>-1</SUP>),
  differentially the C IV line flux (from 30 to 130×10<SUP>3</SUP>erg
  cm<SUP>-2</SUP>s<SUP>-1</SUP>sr<SUP>-1</SUP>), and the excess of 160 nm
  continuum temperature brightness (from 100 to 250K) over the underlying
  plage. No detectable variation is observed in the 220-nm channel
  formed in the medium photosphere. These values are small compared to
  other observed or calculated equivalent quantities from Machado model
  of flare F1. The authors estimate the corresponding power required to
  heat the temperature minimum accordingly over the 1200 Mm<SUP>2</SUP>
  area, to be 3.6×10<SUP>25</SUP>erg s<SUP>-1</SUP> for this small
  X-ray C6 flare, 7 minutes after the ground based observed flare maximum.

---------------------------------------------------------
Title: New ultra-violet filtergrams and results from the transition
    region camera rocket experiment
Authors: Damé, L.; Foing, B. H.; Martic, M.; Bruner, M.; Brown, W.;
   Decaudin, M.; Bonnet, R. M.
1986AdSpR...6h.273D    Altcode: 1986AdSpR...6..273D
  The rocket-borne solar ultra-violet telescope named Transition Region
  Camera (T.R.C.) was launched successfully for the fourth time on
  25th october 1985. Calibrated photographic images of the sun were
  obtained at Lyman alpha and in two adjacent bands at 156 nm and 169
  nm. The angular resolution achieved was equivalent to 0.7 arcsec. Fine
  structures in Lyman alpha were observed in the network and above
  supergranular cells. From the 156 nm filtergram (including a strong C
  IV contribution) and the 169 nm filtergram, we study the differential
  contribution of the C IV lines and of the continuum emission, from
  the quiet sun, an active region and at the limb.

---------------------------------------------------------
Title: On the origin of the blue continuum of white-light flares
Authors: Dame, L.; Vial, J. -C.
1985ApJ...299L.103D    Altcode:
  A new model for white-light flares is proposed in order to explain
  the observed blue continuum (i.e., the higher contrast longward of
  the Balmer jump, around 4000 A). Its broad temperature plateau between
  60,000 and 90,000 K is compatible with chromospheric evaporation. The
  predicted UV emission, computed here in the Si IV resonance lines
  (1402 and 1393 A), is, however, too large by two orders of magnitude,
  as compared to the emission from weak flares. Because of the lack of a
  comprehensive set of measurements in white-light flares, the validity
  of such a model is still open.

---------------------------------------------------------
Title: Meso-Scale Structures - an Oscillatory Phenomenon
Authors: Dame, L.
1985tphr.conf..244D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Chromospheric Dynamic of Fine Structures
Authors: Dame, L.
1985tphr.conf..241D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The chromospheric dynamics of fine structures.
Authors: Dame, L.
1985MPARp.212..241D    Altcode:
  A Ca II K line movie is presented, which directly enhances the intricate
  imbrication of the inner cell emission in fine structures (the "bright
  points") and the underlying waves driven mechanism. The exceptionally
  high spatial and temporal resolutions (0.5 arcsec and 5 s) of this
  52 minutes laps time movie clearly illustrate the non-linear though
  very regular brightenings of fine structures by seemingly incoming
  wavefronts.

---------------------------------------------------------
Title: Hundredths of Arcsec Resolutions with New Optical Correctors
    on Deep UV Photoresist
Authors: Dame, L.; Decaudin, M.
1985LNP...233..128D    Altcode: 1985hrsp.proc..128D
  This paper describes new optical correctors which are phase conjugated
  to a mirror and allow, in most cases, a residual distorsion of the
  outgoing wavefront as low as λ/40 (16 nm) peak to peak. Such a high
  resolution system is possible with deep U.V. photoresist correctors
  registered at 257 nm in a diverging Michelson-Twyman interferometer
  directly by the mirror to be corrected itself, without any intermediary
  steps. Some results obtained with this technique are given. They show
  the potential interest of this method for optical imaging system in
  space involving large mirror and/or ultraviolet imaging.

---------------------------------------------------------
Title: Meso-scale structures: an oscillatory phenomenon?
Authors: Dame, L.
1985MPARp.212..244D    Altcode:
  A 20 minutes time sequence of simultaneous filtergrams taken in
  the blue peak of the Ca II K line and magnetic field maps taken
  in the photospheric line Fe 6302.5 Å is used to investigate the
  phase coherence of the 3 - 5 minutes oscillation. The extent of the
  coherence eddies in the calcium line is typically 8 Mm (11 arcsec)
  which is comparable to the dimension of the "mesogranulation" observed
  by November et al. (1979). The extension of this phase coherence of
  the oscillatory wavefront is only slightly influenced by the period
  of the wave in the 3 - 5 minutes range. The same analysis done on
  the magnetic field gives a totally different picture with an extended
  phase coherence on active regions superimposed to a "noisy background".

---------------------------------------------------------
Title: Atmospheric structure deduced from disturbed line profiles -
    application to Ca II lines.
Authors: Mein, N.; Mein, P.; Malherbe, J. -M.; Dame, L.; Dumont, S.
1985cdm..proc..167M    Altcode:
  A new method is described in order to derive physical quantities
  (temperature, pressure, radial velocities) from the observation of
  disturbed line profiles. The authors suggest a method of Fourier
  analysis with double profiles and a non linear expansion of the
  coefficient of the Fourier terms. An application to a sequence of H -
  Ca II line is attempted. The method seems a powerful tool allowing
  the determination of at least 4 physical quantities simultaneously.

---------------------------------------------------------
Title: Intensity oscillations in the calcium - K line
Authors: Gouttebroze, P.; Dame, L.; Malherbe, J. -M.
1984MmSAI..55..245G    Altcode:
  An analysis is undertaken of a time sequence of quiet sun filtergrams
  taken in the core of the K line, in order to investigate the oscillatory
  properties of the chromosphere. The physical significance of these
  intensity variations and their diagnostic capabilities are discussed,
  and an oscillatory power vs. frequency and mean intensity diagram
  is noted to indicate the different behaviors of bright regions
  dominated by low frequency waves and darker regions dominated by high
  frequency waves. A diagnostic wavenumber-frequency diagram indicates
  two oscillatory power concentrations which approximately correspond to
  acoustic and gravity waves, in chromospheric conditions. A theoretical
  diagnostic diagram computed on the basis of a solar atmosphere model
  exhibits a 'g-1' chromospheric mode; this corresponds almost exactly
  to the location of the observed ridge.

---------------------------------------------------------
Title: Small-Scale Dynamical Processes in the Solar Chromosphere
Authors: Dame, L.
1984ssdp.conf...54D    Altcode:
  Two time series of high resolution and long duration observations - H
  line spectra and filtergrams in the core of the K-line - were analyzed
  to investigate the physical and oscillatory properties of chromospheric
  fine structures. Time-resolved spectroscopy of the H-line data and
  frequency analysis (frequency maps, diagram brightness-frequency) of the
  K-line filtergrams allow to draw a coherent picture of the relationships
  between the chromospheric field of oscillation and the "cell points".

---------------------------------------------------------
Title: Ultraviolet resolution of large mirrors via Hartmann tests
    and two-dimensional fast Fourier transform analysis.
Authors: Dame, L.; Vakili, F.
1984OptEn..23..759D    Altcode:
  Large mirrors appear to be limited in resolution by their medium scale
  defects (mirror surface "ripples" of small amplitude and of 4 to 12
  cycles per diameter). The ultraviolet resolutions of the Pic du Midi
  (PDM) 2 m mirror, the Canada-France-Hawaii (CFH) 3.6 m mirror, and
  the Space Telescope (ST) 2.4 m mirror have been studied. Hartmann
  screen tests were used to determine the wavefront error of the PDM
  and CFH mirrors, while only semiquantitative reports were used in the
  case of the ST mirror. Point spread function and modulation transfer
  function were determined by two-dimensional fast Fourier transform
  analysis, a necessary technique in the ultraviolet, where the small
  phase defects of mirrors are no longer negligible (and also because
  the mirrors' irregularities do not possess a particular arrangement
  or a given symmetry). If the three mirrors appear to be nearly limited
  by diffraction in the visible (except the CFH), in the ultraviolet at
  Lyman a 121.6 nm the resolution is inferior by more than a factor of 10
  to the diffraction-limited resolution. While the ultra-violet wavelength
  range and very high resolution (0.014 arcsec with a diffrac-tion-limited
  Space Telescope at Lyman a) are highly desirable, such a limitation
  imposed by mirror surface quality has to be mentioned. The effects
  of the correlation length, amplitude of defects, and Hartmann screen
  sampling are presented, as well as some comments on the inadequacy
  in the ultraviolet of analytical methods compared to two-dimensional
  numerical simulations.

---------------------------------------------------------
Title: Observation and analysis of intensity oscillations in the
    solar K-line
Authors: Dame, L.; Gouttebroze, P.; Malherbe, J. -M.
1984A&A...130..331D    Altcode:
  Chromospheric oscillations are investigated with a time sequence
  of filtergrams of the sun taken in the core of the Ca II K-line at
  the Sacramento Peak Observatory. The relations between oscillation
  frequency and wavenumber are analyzed, as are those between frequency
  and mean intensity. Intensity analysis reveals that low frequency waves
  are associated mainly with bright (chromospheric network) regions,
  while the '3-min' oscillation dominates in cell interiors. As the mean
  brightness of the observed region increases, the high frequency limit
  of oscillatory power decreases. This is interpreted as the decrease of
  the resonance frequency of the chromospheric cavity with increasing
  temperatures, which confirms the chromospheric origin of the 3-min
  oscillations. Diagnostic diagrams suggest that both acoustic and
  internal gravity waves occur in the chromosphere and appear to have
  a modal structure.

---------------------------------------------------------
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.
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: A UV Corrector for Large Space-Borne Telescopes
Authors: Dame, L.
1984ssdp.conf...90D    Altcode:
  A new interferometric method is presented which allows for the creation
  of a primary mirror corrector of small size and of very high precision
  (a few nanometers of surface distortions). This corrector allows the
  suppression of large and medium scale defects (classical aberrations,
  ripples up to 10 - 20 cycles per diameter). Used with space-borne
  telescopes, such correctors would allow extremely high resolution
  (hundreds of arcsecs) while their use on ground-based telescopes
  could improve the resolution of short-exposure imagery (speckle)
  when limitation is a result of the telescope quality rather than the
  seeing conditions.

---------------------------------------------------------
Title: White-light radiation from semi-empirical flare models.
Authors: Dame, L.; Cram, L.
1983SoPh...87..329D    Altcode:
  We show that some recently published semi-empirical models for solar
  flares predict a significant flux of visible continuum radiation,
  due to bound-free radiation from hydrogen atoms and H<SUP>−</SUP>
  ions in the chromospheric flare. The ratio of the emergent intensity in
  one flare model to that in the quiet Sun is more than 100% at the head
  of the Balmer continuum for a flare close to the limb, and 8% at disk
  centre. The predicted flare spectrum has a relatively strong Balmer
  jump. We compare the theoretical flare continuum with observations and
  find disagreement in several important respects. The main disagreements
  are: (1) the fact that few flares are observed to emit a white-light
  continuum, while the models suggest that they should do so; (2)
  the prediction of a strong Balmer jump, which is not observed in
  most white-light flares; and (3) the absence of a `blue continuum'
  in the theoretical prediction. We conclude that observations of flare
  continua provide useful constraints on semi-empirical models, and that
  at present the models do not satisfy these constraints.

---------------------------------------------------------
Title: High spatial and temporal resolution observations of the
    solar CA II H line
Authors: Cram, L. E.; Dame, L.
1983ApJ...272..355C    Altcode:
  A 24 minute time series of photographic Ca II H line spectra made with
  high spatial and spectral resolution has been analyzed to provide data
  on the range of line profile variations in the quiet sun. Distribution
  functions of the line-core intensity and the ratio of emission peak
  intensities are exhibited and are used to classify the associated
  line profiles. It is shown that the range of profile variation is
  significantly larger than that covered by the models A-F of Vernazza,
  Avrett, and Loeser, especially in relation to the darkest profiles
  in which no core emission can be detected. Time-resolved spectra are
  used to show that the 3-minute chromospheric oscillation involves
  upward-propagating excitation which leads to intense heating in the
  cell points. It is conjectured that these observations provide a direct
  picture of the processes responsible for a significant part of the
  nonradiative heating of the quiet chromosphere.

---------------------------------------------------------
Title: Space-time Analysis of Oscillations Observed in the Solar Ca
    II Resonance Lines
Authors: Dame, L.; Gouttebroze, P.
1982BAAS...14..922D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Relationships between CaII H Line Fine Structure and the
    Integrated Solar H Line
Authors: Damé, L.; Cram, L.
1981BAAS...13..829D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Radiative Processes in White-Light Flares
Authors: Damé, L.; Cram, L.
1981BAAS...13Q.820D    Altcode:
  No abstract at ADS