Author name code: martic ADS astronomy entries on 2022-09-14 author:"Martic, Milena" ------------------------------------------------------------------------ Title: Asteroseismology of solar-type stars with Kepler I: Data analysis Authors: Karoff, C.; Chaplin, W. J.; Appourchaux, T.; Elsworth, Y.; Garcia, R. A.; Houdek, G.; Metcalfe, T. S.; Molenda-Żakowicz, J.; Monteiro, M. J. P. F. G.; Thompson, M. J.; Christensen-Dalsgaard, J.; Gilliland, R. L.; Kjeldsen, H.; Basu, S.; Bedding, T. R.; Campante, T. L.; Eggenberger, P.; Fletcher, S. T.; Gaulme, P.; Handberg, R.; Hekker, S.; Martic, M.; Mathur, S.; Mosser, B.; Regulo, C.; Roxburgh, I. W.; Salabert, D.; Stello, D.; Verner, G. A.; Belkacem, K.; Biazzo, K.; Cunha, M. S.; Gruberbauer, M.; Guzik, J. A.; Kupka, F.; Leroy, B.; Ludwig, H. -G.; Mathis, S.; Noels, A.; Noyes, R. W.; Roca Cortes, T.; Roth, M.; Sato, K. H.; Schmitt, J.; Suran, M. D.; Trampedach, R.; Uytterhoeven, K.; Ventura, R. Bibcode: 2010AN....331..972K Altcode: 2010arXiv1005.0507K We report on the first asteroseismic analysis of solar-type stars observed by Kepler. Observations of three G-type stars, made at one-minute cadence during the first 33.5 days of science operations, reveal high signal-to-noise solar-like oscillation spectra in all three stars: About 20 modes of oscillation can clearly be distinguished in each star. We discuss the appearance of the oscillation spectra, including the presence of a possible signature of faculae, and the presence of mixed modes in one of the three stars. Title: Search for HDO in the astronomical spectroscopic archives of the Observatoire de Haute-Provence Authors: Sarkissian, Alain; Martic, Milena; Alkasm, Sulaf; Hoareau, Christophe; Keckhut, Philippe; Hauchecorne, Alain Bibcode: 2010EGUGA..1212402S Altcode: Astronomical spectroscopic archives of Observatoire de Haute Provence is a database of high-resolution spectra of astronomical objects (spectral domain: 385 nm to 680 nm; sampling 0.005 nm; resolution: 0.0065 nm) obtained with the Elodie spectrograph on a 193-cm diameter telescope at Observatoire de Haute Provence (5 ° 42' E, +43° 55' N, altitude 681 m). Note that Sophie spectrograph replaced the Elodie Spectrograph in July 2005 and the Sophie archive is also open to the community. More than 20 000 spectra of stars and other astrophysical objects are available in these archives accessible using an online web service or php protocol. This database is updated regularly, when spectra with restricted access are opened to the community, or after updating the pipeline of the processing. Our spectral analysis to retrieve H2O is composed of cyclic procedures, varying spectral resolution of water vapor cross-section, spectral shift of water vapor cross-section and the total column of water vapor molecules per surface area in line-of-sight for each individual spectra. Seasonal variability of water vapor as well as a preliminary study of its trend above the observatory is possible because of the high quality of the available data. Astronomy can provide valuable past and present observations useful for atmospheric science, and this should be explored further. We are exploring here the possibility to retrieve HDO using similaire technique and extending it to differential methods. Results of our study will be presented here. Title: A Multi-Site Campaign to Measure Solar-Like Oscillations in Procyon. II. Mode Frequencies Authors: Bedding, Timothy R.; Kjeldsen, Hans; Campante, Tiago L.; Appourchaux, Thierry; Bonanno, Alfio; Chaplin, William J.; Garcia, Rafael A.; Martić, Milena; Mosser, Benoit; Butler, R. Paul; Bruntt, Hans; Kiss, László L.; O'Toole, Simon J.; Kambe, Eiji; Ando, Hiroyasu; Izumiura, Hideyuki; Sato, Bun'ei; Hartmann, Michael; Hatzes, Artie; Barban, Caroline; Berthomieu, Gabrielle; Michel, Eric; Provost, Janine; Turck-Chièze, Sylvaine; Lebrun, Jean-Claude; Schmitt, Jerome; Bertaux, Jean-Loup; Benatti, Serena; Claudi, Riccardo U.; Cosentino, Rosario; Leccia, Silvio; Frandsen, Søren; Brogaard, Karsten; Glowienka, Lars; Grundahl, Frank; Stempels, Eric; Arentoft, Torben; Bazot, Michaël; Christensen-Dalsgaard, Jørgen; Dall, Thomas H.; Karoff, Christoffer; Lundgreen-Nielsen, Jens; Carrier, Fabien; Eggenberger, Patrick; Sosnowska, Danuta; Wittenmyer, Robert A.; Endl, Michael; Metcalfe, Travis S.; Hekker, Saskia; Reffert, Sabine Bibcode: 2010ApJ...713..935B Altcode: 2010arXiv1003.0052B We have analyzed data from a multi-site campaign to observe oscillations in the F5 star Procyon. The data consist of high-precision velocities that we obtained over more than three weeks with 11 telescopes. A new method for adjusting the data weights allows us to suppress the sidelobes in the power spectrum. Stacking the power spectrum in a so-called échelle diagram reveals two clear ridges, which we identify with even and odd values of the angular degree (l = 0 and 2, and l = 1 and 3, respectively). We interpret a strong, narrow peak at 446 μHz that lies close to the l = 1 ridge as a mode with mixed character. We show that the frequencies of the ridge centroids and their separations are useful diagnostics for asteroseismology. In particular, variations in the large separation appear to indicate a glitch in the sound-speed profile at an acoustic depth of ~1000 s. We list frequencies for 55 modes extracted from the data spanning 20 radial orders, a range comparable to the best solar data, which will provide valuable constraints for theoretical models. A preliminary comparison with published models shows that the offset between observed and calculated frequencies for the radial modes is very different for Procyon than for the Sun and other cool stars. We find the mean lifetime of the modes in Procyon to be 1.29+0.55 -0.49 days, which is significantly shorter than the 2-4 days seen in the Sun. Title: The Asteroseismic Potential of Kepler: First Results for Solar-Type Stars Authors: Chaplin, W. J.; Appourchaux, T.; Elsworth, Y.; García, R. A.; Houdek, G.; Karoff, C.; Metcalfe, T. S.; Molenda-Żakowicz, J.; Monteiro, M. J. P. F. G.; Thompson, M. J.; Brown, T. M.; Christensen-Dalsgaard, J.; Gilliland, R. L.; Kjeldsen, H.; Borucki, W. J.; Koch, D.; Jenkins, J. M.; Ballot, J.; Basu, S.; Bazot, M.; Bedding, T. R.; Benomar, O.; Bonanno, A.; Brandão, I. M.; Bruntt, H.; Campante, T. L.; Creevey, O. L.; Di Mauro, M. P.; Doǧan, G.; Dreizler, S.; Eggenberger, P.; Esch, L.; Fletcher, S. T.; Frandsen, S.; Gai, N.; Gaulme, P.; Handberg, R.; Hekker, S.; Howe, R.; Huber, D.; Korzennik, S. G.; Lebrun, J. C.; Leccia, S.; Martic, M.; Mathur, S.; Mosser, B.; New, R.; Quirion, P. -O.; Régulo, C.; Roxburgh, I. W.; Salabert, D.; Schou, J.; Sousa, S. G.; Stello, D.; Verner, G. A.; Arentoft, T.; Barban, C.; Belkacem, K.; Benatti, S.; Biazzo, K.; Boumier, P.; Bradley, P. A.; Broomhall, A. -M.; Buzasi, D. L.; Claudi, R. U.; Cunha, M. S.; D'Antona, F.; Deheuvels, S.; Derekas, A.; García Hernández, A.; Giampapa, M. S.; Goupil, M. J.; Gruberbauer, M.; Guzik, J. A.; Hale, S. J.; Ireland, M. J.; Kiss, L. L.; Kitiashvili, I. N.; Kolenberg, K.; Korhonen, H.; Kosovichev, A. G.; Kupka, F.; Lebreton, Y.; Leroy, B.; Ludwig, H. -G.; Mathis, S.; Michel, E.; Miglio, A.; Montalbán, J.; Moya, A.; Noels, A.; Noyes, R. W.; Pallé, P. L.; Piau, L.; Preston, H. L.; Roca Cortés, T.; Roth, M.; Sato, K. H.; Schmitt, J.; Serenelli, A. M.; Silva Aguirre, V.; Stevens, I. R.; Suárez, J. C.; Suran, M. D.; Trampedach, R.; Turck-Chièze, S.; Uytterhoeven, K.; Ventura, R.; Wilson, P. A. Bibcode: 2010ApJ...713L.169C Altcode: 2010arXiv1001.0506C We present preliminary asteroseismic results from Kepler on three G-type stars. The observations, made at one-minute cadence during the first 33.5 days of science operations, reveal high signal-to-noise solar-like oscillation spectra in all three stars: about 20 modes of oscillation may be clearly distinguished in each star. We discuss the appearance of the oscillation spectra, use the frequencies and frequency separations to provide first results on the radii, masses, and ages of the stars, and comment in the light of these results on prospects for inference on other solar-type stars that Kepler will observe. Title: A Multisite Campaign to Measure Solar-like Oscillations in Procyon. I. Observations, Data Reduction, and Slow Variations Authors: Arentoft, Torben; Kjeldsen, Hans; Bedding, Timothy R.; Bazot, Michaël; Christensen-Dalsgaard, Jørgen; Dall, Thomas H.; Karoff, Christoffer; Carrier, Fabien; Eggenberger, Patrick; Sosnowska, Danuta; Wittenmyer, Robert A.; Endl, Michael; Metcalfe, Travis S.; Hekker, Saskia; Reffert, Sabine; Butler, R. Paul; Bruntt, Hans; Kiss, László L.; O'Toole, Simon J.; Kambe, Eiji; Ando, Hiroyasu; Izumiura, Hideyuki; Sato, Bun'ei; Hartmann, Michael; Hatzes, Artie; Bouchy, Francois; Mosser, Benoit; Appourchaux, Thierry; Barban, Caroline; Berthomieu, Gabrielle; Garcia, Rafael A.; Michel, Eric; Provost, Janine; Turck-Chièze, Sylvaine; Martić, Milena; Lebrun, Jean-Claude; Schmitt, Jerome; Bertaux, Jean-Loup; Bonanno, Alfio; Benatti, Serena; Claudi, Riccardo U.; Cosentino, Rosario; Leccia, Silvio; Frandsen, Søren; Brogaard, Karsten; Glowienka, Lars; Grundahl, Frank; Stempels, Eric Bibcode: 2008ApJ...687.1180A Altcode: 2008arXiv0807.3794A We have carried out a multisite campaign to measure oscillations in the F5 star Procyon A. We obtained high-precision velocity observations over more than three weeks with 11 telescopes, with almost continuous coverage for the central 10 days. This represents the most extensive campaign so far organized on any solar-type oscillator. We describe in detail the methods we used for processing and combining the data. These involved calculating weights for the velocity time series from the measurement uncertainties and adjusting them in order to minimize the noise level of the combined data. The time series of velocities for Procyon shows the clear signature of oscillations, with a plateau of excess power that is centered at 0.9 mHz and is broader than has been seen for other stars. The mean amplitude of the radial modes is 38.1 +/- 1.3 cm s-1 (2.0 times solar), which is consistent with previous detections from the ground and by the WIRE spacecraft, and also with the upper limit set by the MOST spacecraft. The variation of the amplitude during the observing campaign allows us to estimate the mode lifetime to be 1.5+ 1.9-0.8 days. We also find a slow variation in the radial velocity of Procyon, with good agreement between different telescopes. These variations are remarkably similar to those seen in the Sun, and we interpret them as being due to rotational modulation from active regions on the stellar surface. The variations appear to have a period of about 10 days, which presumably equals the stellar rotation period or, perhaps, half of it. The amount of power in these slow variations indicates that the fractional area of Procyon covered by active regions is slightly higher than for the Sun. Title: Oscillations in Procyon A: First results from a multi-site campaign Authors: Hekker, S.; Arentoft, T.; Kjeldsen, H.; Bedding, T. R.; Christensen-Dalsgaard, J.; Reffert, S.; Bruntt, H.; Butler, R. P.; Kiss, L. L.; O'Toole, S. J.; Kambe, E.; Ando, H.; Izumiura, H.; Sato, B.; Hartmann, M.; Hatzes, A. P.; Appourchaux, T.; Barban, C.; Berthomieu, G.; Bouchy, F.; García, R. A.; Lebrun, J. -C.; Martić, M.; Michel, E.; Mosser, B.; Nghiem, P. A. P.; Provost, J.; Samadi, R.; Thévenin, F.; Turck-Chièze, S.; Bonanno, S. A.; Benatti, S.; Claudi, R. U.; Cosentino, R.; Leccia, S.; Frandsen, S.; Brogaard, K.; Grundahl, F.; Stempels, H. C.; Bazot, M.; Dall, T. H.; Karoff, C.; Carrier, F.; Eggenberger, P.; Sosnowska, D.; Wittenmyer, R. A.; Endl, M.; Metcalfe, T. S. Bibcode: 2008JPhCS.118a2059H Altcode: 2007arXiv0710.3772H Procyon A is a bright F5IV star in a binary system. Although the distance, mass and angular diameter of this star are all known with high precision, the exact evolutionary state is still unclear. Evolutionary tracks with different ages and different mass fractions of hydrogen in the core pass, within the errors, through the observed position of Procyon A in the Hertzsprung-Russell diagram. For more than15 years several different groups have studied the solar-like oscillations in Procyon A to determine its evolutionary state. Although several studies independently detected power excess in the periodogram, there is no agreement on the actual oscillation frequencies yet. This is probably due to either insufficient high-quality data (i.e., aliasing) or due to intrinsic properties of the star (i.e., short mode lifetimes). Now a spectroscopic multi-site campaign using 10 telescopes world-wide (minimizing aliasing effects) with a total time span of nearly 4 weeks (increase the frequency resolution) is performed to identify frequencies in this star and finally determine its properties and evolutionary state. Title: Development of Iodine Cells for Subaru HDS and Okayama HIDES. III. An Improvement on the Radial-Velocity Measurement Technique Authors: Kambe, Eiji; Ando, Hiroyasu; Sato, Bun'ei; Izumiura, Hideyuki; Sekii, Takashi; Paulson, Daine B.; Yanagisawa, Kenshi; Masuda, Seiji; Shibahashi, Hiromoto; Hatzes, Artie P.; Martic, Milena; Lebrun, Jean-Claude; Mkrtichian, David E.; Kiss, Laszlo L.; Bruntt, Hans; O'Toole, Simon J.; Bedding, Timothy R. Bibcode: 2008PASJ...60...45K Altcode: An improvement of the radial-velocity measurement accuracy is crucial for the detection of tiny stellar oscillations and exoplanets. Through the analysis of week-long extensive observations of solar-type stars (Procyon in 2000, 2002, and 2006/2007 and τ Cet in 2002 and 2006/2007), we have carefully examined, revised, and finely tuned the widely used multiple Gaussian IP fitting method for the spectrograph, HIDES. By determining a necessary and sufficient number of free parameters in the model as well as introducing an iterative process in the radial-velocity analysis, we can reach a precision of below 3ms-1, which is much smaller than the precision of 6ms-1 officially announced so far for HIDES. We also make our technique refined for the 2002 McDonald Procyon data. Even with our revised method, slow radial velocity variations with an amplitude of about 10ms-1 are left in the Procyon data. We emphasize that it is neither due to particular observing instruments nor radial-velocity analysis, and thus could be due to stellar origin. The analysis presented here makes the foundations of our next scientific analysis of the radial-velocity variations of Procyon, which will be presented in our forthcoming papers. Title: Asteroseismology of Procyon with SOPHIE Authors: Mosser, B.; Bouchy, F.; Martić, M.; Appourchaux, T.; Barban, C.; Berthomieu, G.; Garcia, R. A.; Lebrun, J. C.; Michel, E.; Provost, J.; Thévenin, F.; Turck-Chièze, S. Bibcode: 2008A&A...478..197M Altcode: 2007arXiv0712.1368M Context: This paper reports a 9-night asteroseismic observation program conducted in January 2007 with the new spectrometer sophie at the OHP 193-cm telescope, on the F5 IV-V target Procyon A.
Aims: This first asteroseismic program with sophie was intended to test the performance of the instrument with a bright but demanding asteroseismic target and was part of a multisite network.
Methods: The sophie spectra have been reduced with the data reduction software provided by OHP. The Procyon asteroseismic data were then analyzed with statistical tools. The asymptotic analysis has been conducted considering possible curvature in the échelle diagram analysis.
Results: These observations have proven the efficient performance of sophie used as an asteroseismometer, and succeed in a clear detection of the large spacing. An échelle diagram based on the 54-μHz spacing shows clear ridges. Identification of the peaks exhibits large spacings varying from about 52 μHz to 56 μHz. Outside the frequency range [0.9, 1.0 mHz] where the identification is confused, the large spacing increases at a rate of about dΔν/dn ≃ 0.2 μHz. This may explain some of the different values of the large spacing obtained by previous observations.

Based on observations collected with the sophie échelle spectrometer mounted on the 1.93-m telescope at OHP, France (program 06B.PNPS.BOU); http://www.obs-hp.fr/www/guide/ sophie/sophie-eng.html Table of radial velocity measurements is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/478/197 Title: VizieR Online Data Catalog: Procyon (alpha CMi) radial velocities (Mosser+, 2008) Authors: Mosser, B.; Bouchy, F.; Martic, M.; Appourchaux, T.; Barban, C.; Berthomieu, G.; Garcia, R. A.; Lebrun, J. C.; Michel, E.; Provost, J.; Thevenin, F.; Turck-Chieze, S. Bibcode: 2007yCat..34780197M Altcode: Time series of the radial velocities of Procyon recorder with the echelle spectrometer SOPHIE at Observatoire de Haute Provence in January 2007.

(1 data file). Title: Asteroseismology and evolutionary status of Procyon A Authors: Provost, J.; Berthomieu, G.; Martić, M.; Morel, P. Bibcode: 2006A&A...460..759P Altcode: Models of Procyon A satisfying the actual observational constraints, particularly the asteroseismic ones, are discussed. The oscillations of these models were computed and analysed. We looked for seismic signatures of the evolutionary status of Procyon A. We show that the behavior of the small frequency spacings, particularly δν01 allows us to distinguish between main sequence and post-main sequence models, all satisfying the observational constraints on mass, effective temperature, radius, and surface metallicity of Procyon A. We also introduce a new seismic evolution criterion, varepsilon, based on the comparison of the low and high frequency parts of the power spectrum. The comparison of the seismic properties of the models with the available asteroseismic observations does not allow us to definitely decide on the stage of evolution of Procyon A. Much more accurate frequencies must be obtained especially in the low-frequency domain to distinguish between the models. Title: The DynaMICS perspective Authors: Turck-Chièze, S.; Schmutz, W.; Thuillier, G.; Jefferies, S.; Pallé; Dewitt, S.; Ballot, J.; Berthomieu, G.; Bonanno, A.; Brun, A. S.; Christensen-Dalsgaard, J.; Corbard, T.; Couvidat, S.; Darwich, A. M.; Dintrans, B.; Domingo, V.; Finsterle, W.; Fossat, E.; Garcia, R. A.; Gelly, B.; Gough, D.; Guzik, J.; Jiménez, A. J.; Jiménez-Reyes, S.; Kosovichev, A.; Lambert, P.; Lefebvre, S.; Lopes, I.; Martic, M.; Mathis, S.; Mathur, S.; Nghiem, P. A. P.; Piau, L.; Provost, J.; Rieutord, M.; Robillot, J. M.; Rogers, T.; Roudier, T.; Roxburgh, I.; Rozelot, J. P.; Straka, C.; Talon, S.; Théado, S.; Thompson, M.; Vauclair, S.; Zahn, J. P. Bibcode: 2006ESASP.624E..24T Altcode: 2006soho...18E..24T No abstract at ADS Title: Scientific Objectives of the Novel Formation Flying Mission Aspiics Authors: Turck-Chièze, S.; Schmutz, W.; Thuillier, G.; Jefferies, S.; Pallé; Dewitt, S.; Ballot, J.; Berthomieu, G.; Bonanno, A.; Brun, A. S.; Christensen-Dalsgaard, J.; Corbard, T.; Couvidat, S.; Darwich, A. M.; Dintrans, B.; Domingo, V.; Finsterle, W.; Fossat, E.; Garcia, R. A.; Gelly, B.; Gough, D.; Guzik, J.; Jiménez, A. J.; Jiménez-Reyes, S.; Kosovichev, A.; Lambert, P.; Lefebvre, S.; Lopes, I.; Martic, M.; Mathis, S.; Mathur, S.; Nghiem, P. A. P.; Piau, L.; Provost, J.; Rieutord, M.; Robillot, J. M.; Rogers, T.; Roudier, T.; Roxburgh, I.; Rozelot, J. P.; Straka, C.; Talon, S.; Théado, S.; Thompson, M.; Vauclair, S.; Zahn, J. P. Bibcode: 2006ESASP.617E.164L Altcode: 2006soho...17E.164L No abstract at ADS Title: The EUV Variability Experiment (EVE) on the Solar Dynamics Observatory (SDO): Science Plan and Instrument Overview Authors: Turck-Chièze, S.; Schmutz, W.; Thuillier, G.; Jefferies, S.; Pallé; Dewitt, S.; Ballot, J.; Berthomieu, G.; Bonanno, A.; Brun, A. S.; Christensen-Dalsgaard, J.; Corbard, T.; Couvidat, S.; Darwich, A. M.; Dintrans, B.; Domingo, V.; Finsterle, W.; Fossat, E.; Garcia, R. A.; Gelly, B.; Gough, D.; Guzik, J.; Jiménez, A. J.; Jiménez-Reyes, S.; Kosovichev, A.; Lambert, P.; Lefebvre, S.; Lopes, I.; Martic, M.; Mathis, S.; Mathur, S.; Nghiem, P. A. P.; Piau, L.; Provost, J.; Rieutord, M.; Robillot, J. M.; Rogers, T.; Roudier, T.; Roxburgh, I.; Rozelot, J. P.; Straka, C.; Talon, S.; Théado, S.; Thompson, M.; Vauclair, S.; Zahn, J. P. Bibcode: 2006ESASP.617E.165W Altcode: 2006soho...17E.165W No abstract at ADS Title: The Dynamics Project Authors: Turck-Chièze, S.; Schmutz, W.; Thuillier, G.; Jefferies, S.; Pallé; Dewitt, S.; Ballot, J.; Berthomieu, G.; Bonanno, A.; Brun, A. S.; Christensen-Dalsgaard, J.; Corbard, T.; Couvidat, S.; Darwich, A. M.; Dintrans, B.; Domingo, V.; Finsterle, W.; Fossat, E.; Garcia, R. A.; Gelly, B.; Gough, D.; Guzik, J.; Jiménez, A. J.; Jiménez-Reyes, S.; Kosovichev, A.; Lambert, P.; Lefebvre, S.; Lopes, I.; Martic, M.; Mathis, S.; Mathur, S.; Nghiem, P. A. P.; Piau, L.; Provost, J.; Rieutord, M.; Robillot, J. M.; Rogers, T.; Roudier, T.; Roxburgh, I.; Rozelot, J. P.; Straka, C.; Talon, S.; Théado, S.; Thompson, M.; Vauclair, S.; Zahn, J. P. Bibcode: 2006ESASP.617E.162T Altcode: 2006soho...17E.162T No abstract at ADS Title: About Procyon modeling Authors: Provost, J.; Berthomieu, G.; Martić, M. Bibcode: 2006MmSAI..77..474P Altcode: Models of Procyon satisfying the actual observational constraints, particularly the asteroseismic ones, are discussed. It is shown that much more accurate frequencies must be obtained by asteroseismic observations especially in the low frequency domain below 800 mu Hertz to determine the Procyon evolutionary stage. Title: The non-detection of oscillations in Procyon by MOST: Is it really a surprise? Authors: Bedding, T. R.; Kjeldsen, H.; Bouchy, F.; Bruntt, H.; Butler, R. P.; Buzasi, D. L.; Christensen-Dalsgaard, J.; Frandsen, S.; Lebrun, J. -C.; Martić, M.; Schou, J. Bibcode: 2005A&A...432L..43B Altcode: 2005astro.ph..1662B We argue that the non-detection of oscillations in Procyon by the MOST satellite reported by [CITE] is fully consistent with published ground-based velocity observations of this star. We also examine the claims that the MOST observations represent the best photometric precision so far reported in the literature by about an order of magnitude and are the most sensitive data set for asteroseismology available for any star other than the Sun. These statements are not correct, with the most notable exceptions being observations of oscillations in α Cen A that are far superior. We further disagree that the hump of excess power seen repeatedly from velocity observations of Procyon can be explained as an artefact caused by gaps in the data. The MOST observations failed to reveal oscillations clearly because their noise level is too high, possibly from scattered Earthlight in the instrument. We did find an excess of strong peaks in the MOST amplitude spectrum that is inconsistent with a simple noise source such as granulation, and may perhaps indicate oscillations at roughly the expected level. Title: About Models and Oscillations of the Solar-Like Star Procyon a Authors: Provost, J.; Martic, M.; Berthomieu, G. Bibcode: 2004ESASP.559..594P Altcode: 2004soho...14..594P No abstract at ADS Title: a Radial Velocity Search for P-Modes in VIR Authors: Martic, M.; Lebrun, J. C.; Appourchaux, T.; Schmitt, J. Bibcode: 2004ESASP.559..563M Altcode: 2004astro.ph..9126M; 2004soho...14..563M Spectroscopic high-resolution observations were performed with fiber-fed cross-dispersed echelle spectrographs in order to measure the fluctuations in radial velocities of a sample of bright stars that are likely to undergo solar-like oscillations. Here we report the results for beta Vir (HR4540) from two observing runs carried out in February 2002 with FEROS at the ESO 1.52 m telescope in La Silla (Chile) and ELODIE spectrograph at 1.93 OHP telescope (Observatoire de Haute Provence, France). The analysis of the time series of Doppler shifts from both sites has revealed the presence of an excess power around 1.7 mHz. We discuss the interpretation of this data set in terms of possible p-mode oscillations. Title: p-mode frequencies in solar-like stars. I. Procyon A Authors: Martić, M.; Lebrun, J. -C.; Appourchaux, T.; Korzennik, S. G. Bibcode: 2004A&A...418..295M Altcode: 2004astro.ph..3035M As a part of an on-going program to explore the signature of p-modes in solar-like stars by means of high-resolution absorption line spectroscopy, we have studied four stars (α CMi, η Cas A, ζ Her A and β Vir). We present here new results from two-site observations of Procyon A acquired over twelve nights in 1999. Oscillation frequencies for l=1 and 0 (or 2) p-modes are detected in the power spectra of these Doppler shift measurements. A frequency analysis points out the difficulties of the classical asymptotic theory in representing the p-mode spectrum of Procyon A.

Based on observations obtained at the Observatoire de Haute-Provence (CNRS, France) and at the Whipple Observatory (Arizona, USA). Title: On the properties of solar-like oscillations: application to Procyon Authors: Provost, J.; Martić, M.; Berthomieu, G.; Morel, P. Bibcode: 2002ESASP.485..309P Altcode: 2002sshp.conf..309P In order to interpret the ground-based observations of solar-like stellar oscillations and prepare the scientific exploitation of future spatial asteroseismic observations, we have studied the theoretical properties of the frequencies of possible models for a given stellar target, taking into account its observational constraints in the Hertzsprung-Russell diagram. We have computed a set of "calibrated" stellar models satisfying these constraints for a star of solar metallicity. We present some results on the sensitivity of the oscillation frequencies to the description of the convective transport and to physical processes entering in the stellar modeling, like core overshoot. We compare the seismic properties of our models with the observations of Procyon by Martić et al. (2001). Title: Observing solar-like oscillations with ELODIE spectrograph Authors: Martić, M.; Lebrun, J. C.; Schmitt, J.; Bertaux, J. L.; Appourchaux, T. Bibcode: 2001sf2a.conf..219M Altcode: We have used ELODIE fiber-fed cross-dispersed echelle spectrograph and the 1.93m-telescope of Observatoire de Haute Provence to obtain precise Doppler measurements of a sample of bright stars that are likely to undergo solar-like oscillations. Here we report the results for Procyon from three observing runs (5, 10 and 15 nights) in Decembre 1997, Novembre 1998, and January 1999. The individual frequencies of p-modes were searched in the interval of excess power around 1 mHz found in the frequency spectra of each time series. The echelle diagram of the observed and predicted p-mode frequencies from the standard model (Chaboyer et al., 1999) for Procyon A is presented. We show also some preliminary results for two other solar-like stars (eta Cas and z Her). Title: Observing solar-like oscillations: α CMi, η Cas A and ζ Her A Authors: Martić, M.; Lebrun, J. C.; Schmitt, J.; Appourchaux, T.; Bertaux, J. L. Bibcode: 2001ESASP.464..431M Altcode: 2001soho...10..431M We have used ELODIE fiber-fed cross-dispersed echelle spectrograph and the 1.93m-telescope of Observatoire de Haute Provence to obtain precise Doppler measurements of a sample of bright stars that are likely to undergo solar-like oscillations. Here we report the results for Procyon from three observing runs carried out in December 1997, November 1998, and January 1999. We show also some preliminary results for two other solar-like stars (η Cas A and ζ Her A). Title: Solar-like Oscillations on Procyon (CD-ROM Directory: contribs/martic) Authors: Martic, M.; Lebrun, J. -C.; Schmitt, J.; Bertaux, J. L.; Barban, C.; Michel, E.; Baglin, A. Bibcode: 2001ASPC..223..703M Altcode: 2001csss...11..703M No abstract at ADS Title: Search for p-mode Frequencies on Procyon A Authors: Martic, M.; Lebrun, J. C.; Schmitt, J.; Bertaux, J. L. Bibcode: 2001IAUS..203..121M Altcode: Following the recent evidence for the presence of an excess of power around 1 mHz in the frequency spectrum of the Doppler shift measurements for Procyon (Martic et al., 1999), we searched for individual frequencies of p-modes from three independent observing runs (5, 10 and 15 nights). All observations (Decembre 1997, Novembre 1998, January 1999) were made with the ELODIE fibre-fed cross-dispersed echelle spectrograph on the 1.93 m telescope at Observatoire de Haute Provence. The individual peaks in clean spectra of each time series in the interval of excess power are compared with the predicted p-mode frequencies from stellar models (Chaboyer et al., 1999) for Procyon A. Title: Solar-Like Oscillations of Procyon A: Stellar Models and Time Series Simulations versus Observations Authors: Barban, C.; Michel, E.; Martic, M.; Schmitt, J.; Lebrun, J. C.; Baglin, A.; Bertaux, J. L. Bibcode: 2000ASPC..203..461B Altcode: 2000ilss.conf..461B; 2000IAUCo.176..461B The aim of this paper (further developed in Barban et al. 1999) is to present new evidence of the possible stellar origin of the observed excess power in the power spectrum of Procyon A presented in Martic et al. (1999) by comparing these observational data with theoretical predictions and numerical simulations. Title: Evidence for global pressure oscillations on Procyon Authors: Martić, M.; Schmitt, J.; Lebrun, J. -C.; Barban, C.; Connes, P.; Bouchy, F.; Michel, E.; Baglin, A.; Appourchaux, T.; Bertaux, J. -L. Bibcode: 1999A&A...351..993M Altcode: Precise Doppler measurements of the star Procyon (alpha CMi, HR 2943) have been obtained with the ELODIE fiber-fed cross-dispersed echelle spectrograph on the 1.93 m telescope at Observatoire de Haute Provence. Here, we present the analysis of data from 10 days observing run carried out in November 1998. We detect significant excess in the power between 0.5-1.5 mHz in the periodograms of the time series of mean Doppler shifts. Observations of eta Cas made with the same instrument during the same time interval and in almost identical night conditions show a flat spectrum in this frequency range, indicating that the excess of Doppler signal seen on Procyon is of stellar origin. When data from the whole run are jointly analyzed, a period analysis places an upper limit of 0.50-0.60 ms-1 for the amplitude of oscillations, while the frequency cutoff is around 1.5 mHz. The power evidently drops near 0.55 and 1.5 mHz on the average of unfiltered power spectra of individual nights, which is consistent with the expected p-mode oscillation properties for Procyon. Several equispaced peaks in frequency are recurrent in the power spectra of two independent segments of 4 and 3 contiguous nights; the most probable frequency spacing seems to be 55 mu Hz. In conclusion, we now have an instrument set-up which is sufficiently stable and fast to be used for a multi-site campaign involving instruments with comparable velocity precisions, to detect the oscillation modes of sun-like stars. Based on observations obtained at the Observatoire de Haute-Provence (CNRS, France) Title: Solar-like oscillations of Procyon A: stellar models and time series simulations versus observations Authors: Barban, C.; Michel, E.; Martic, M.; Schmitt, J.; Lebrun, J. C.; Baglin, A.; Bertaux, J. L. Bibcode: 1999A&A...350..617B Altcode: The aim of this paper is to discuss the possible stellar origin of the observed excess power presented in Martic et al. (\cite{martic}) by comparing these observational data with theoretical predictions and numerical simulations. Stellar models are calculated for Procyon A with appropriate physics for this star and with the revised astrometric mass (1.46 +/- 0.04) Msun found by Girard (\cite{girard98}). For these models, we compute the expected oscillation spectra for l=0,1,2 modes including mnot =0 according to theoretical amplitude predictions. Time-series are then simulated, in the same conditions as the observations, and compared by Fourier analysis with the observed ones. We show that the characteristics of the signal are in good agreement with what should be expected for such observing runs and we emphasize the importance of obtaining multi-site observations for this star. We confirm the presence of a periodic pattern in the Fourier spectrum, this pattern being interpreted as the so-called large separation. Based on observations collected at the Observatoire de Haute-Provence (CNRS, France). Title: Possible Detection of P-Mode Oscillations on Procyon Authors: Barban, C.; Michel, E.; Martic, M.; Schmitt, J.; Bouchy, F.; Lebrun, J. C.; Connes, P.; Bertaux, J. L.; Baglin, A. Bibcode: 1999ASPC..185..177B Altcode: 1999psrv.conf..177B; 1999IAUCo.170..177B Absolute accelerometry is a technique developed by P. Connes (1985) to detect small radial-velocity changes. We observed Procyon with a preliminary version of the Absolute Astronomical Accelerometer (AAA) coupled with the spectrograph ELODIE at the 193 cm telescope of the Observatoire de Haute Provence (France) during 8 nights December 97-January 98. Here, we present results of a search for solar-like oscillations in Procyon and the performance of the AAA for asteroseismology. Title: Asteroseismology with the Absolute Astronomical Accelerometer (AAA): Preliminary Results Authors: Barban, C.; Martic, M.; Schmitt, J.; Connes, P.; Michel, E.; Baglin, A.; Bertaux, J. L. Bibcode: 1998ASPC..135..366B Altcode: 1998hcsp.conf..366B Absolute accelerometry is a technique developed by P. Connes (1985), to detect small radial-velocity changes, involving a CCD spectrograph, two lasers and a Fabry-Perot. The final output is a beat frequency similar to that from a Doppler radar. To estimate the performance of the Absolute Astronomical Accelerometer (AAA) for asteroseismology, we made specific observations, i.e. long continuous observing runs, with a preliminary version of the AAA coupled with the spectrograph Elodie at the T193 (OHP). The reachable accuracy is estimated from observations and simulations. It is shown that AAA is a well-suited instrument to detect solar-like oscillations in stars. References: Connes P.:1985, Astrophys. Sp. Sc., 110, 211. Title: Demonstration of Photon-Noise Limit in Stellar Radial Velocities Authors: Connes, P.; Martic, M.; Schmitt, J. Bibcode: 1996Ap&SS.241...61C Altcode: We have measured apparent fluctuations in stellar radial velocities with the ELODIE fiber-fed crossed-dispersion spectrograph and the 193-cm telescope of Observatoire de Haute-Provence. Within one given night, the fluctuations consist of two terms which may be sorted out. The first comes from imperfect scrambling of the stellar beam; the second arises from photon noise and agrees closely with our published calculations. So far, scrambler noise dominates for bright stars, but a perfect scrambler could be built by combining adatative optics and a single-mode fiber. The photon-noise results confirm that extrasolar planetary searching by the radial-velocity technique may be implemented with relatively small telescopes for a large number of stars. Consequences for the detection of ‘astrophysical noise” are 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. Bibcode: 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: Solar interferometric imaging from the moon Authors: Dame, L.; Martic, M.; Porteneuve, J. Bibcode: 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: Prospects for very-high-resolution solar physics with the Simuris interferometric mission. Authors: Dame, L.; Martic, M.; Rutten, R. J. Bibcode: 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: Study of an optimized configuration for interferometric imaging of complex and extended solar structures. Authors: Dame, L.; Martic, M. Bibcode: 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. Bibcode: 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: 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. Bibcode: 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. Bibcode: 1991AdSpR..11e.241M Altcode: 1991AdSpR..11..241M Simultaneous ground based observations in the Ca II K2V 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. Bibcode: 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. Bibcode: 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. Bibcode: 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: Rocket observations and modelling of flux-tubes Authors: Foing, Bernard H.; Dame, Luc; Martic, Milena Bibcode: 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. Bibcode: 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: Magnetic Field Modulation Issues for Improving Global Solar Oscillation Measurements from Space Authors: Damé, L.; Ulrich, R. K.; Martić, M.; Boumier, P. Bibcode: 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 &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. Bibcode: 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 Bibcode: 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. Bibcode: 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: Oscillatory Properties of Meso-Scale Intensity Structures at Chromospheric Level Authors: Dame, L.; Martic, M. Bibcode: 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: Extreme ultra-violet filtergrams and X-ray spectroscopy of active regions and flares from TRC/XSST rocket campaigns Authors: Foing, B. H.; Martic, M.; Bonnet, R. M.; Bruner, M. E.; Acton, L. W.; Brown, W. A. Bibcode: 1988AdSpR...8k.153F Altcode: 1988AdSpR...8..153F Ultraviolet filtergrams and X ray spectra were taken by the joint LPSP/Lockheed rocket experiment TRC/XSST during four international campaigns involving also ground observations. XSST spectra in the range 8 to 97A were obtained on the 13 July 1982 flare. From the EUV filtergrams obtained by the TRC (Transition Region Camera), we could derive calibrated fluxes in the 220nm and 160 nm continua, in the Ly alpha and C IV lines, spanning a range of temperatures from medium photosphere (5 000K), temperature minimum (4 200K), and transition region (20 000 and 100 000 K). For active regions and a flare, the TRC fluxes are compared to other data and to corresponding calculations from semiempirical models. Finally, the scientific prospects of an advanced TRC/XSST payload onboard future missions are discussed. Title: Rocket flight observations of the meso-scale structure in the temperature minimum region Authors: Martic, M.; Dame, L. Bibcode: 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 arcsec2 field on the quiet sun. Title: Observation and Oscillatory Properties of Mesostructures in the Solar Chromosphere Authors: Dame, L.; Martic, M. Bibcode: 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. Bibcode: 1987JAF....29...15F Altcode: No abstract at ADS Title: Diagnostics à haute résolution des méso-cellules solaires au minimum de température. Authors: Martic, M. Bibcode: 1987JAF....31R..37M Altcode: No abstract at ADS 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. Bibcode: 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.