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Author name code: martic
ADS astronomy entries on 2022-09-14
author:"Martic, Milena"
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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.
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.
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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
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.
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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
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<SUP>+0.55</SUP> <SUB>-0.49</SUB> days,
which is significantly shorter than the 2-4 days seen in the Sun.
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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.
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.
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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
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<SUP>-1</SUP> (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<SUP>+ 1.9</SUP><SUB>-0.8</SUB> 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.
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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.
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.
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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.
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<SUP>-1</SUP>, which
is much smaller than the precision of 6ms<SUP>-1</SUP> 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<SUP>-1</SUP>
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.
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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.
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. <BR
/>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. <BR />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. <BR
/>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. <P />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
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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.
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. <P />(1 data file).
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Title: Asteroseismology and evolutionary status of Procyon A
Authors: Provost, J.; Berthomieu, G.; Martić, M.; Morel, P.
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 δν<SUB>01</SUB>
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.
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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.
2006ESASP.624E..24T Altcode: 2006soho...18E..24T
No abstract at ADS
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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.
2006ESASP.617E.164L Altcode: 2006soho...17E.164L
No abstract at ADS
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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.
2006ESASP.617E.165W Altcode: 2006soho...17E.165W
No abstract at ADS
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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.
2006ESASP.617E.162T Altcode: 2006soho...17E.162T
No abstract at ADS
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Title: About Procyon modeling
Authors: Provost, J.; Berthomieu, G.; Martić, M.
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.
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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.
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.
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Title: About Models and Oscillations of the Solar-Like Star Procyon a
Authors: Provost, J.; Martic, M.; Berthomieu, G.
2004ESASP.559..594P Altcode: 2004soho...14..594P
No abstract at ADS
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Title: a Radial Velocity Search for P-Modes in VIR
Authors: Martic, M.; Lebrun, J. C.; Appourchaux, T.; Schmitt, J.
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.
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Title: p-mode frequencies in solar-like stars. I. Procyon A
Authors: Martić, M.; Lebrun, J. -C.; Appourchaux, T.; Korzennik, S. G.
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. <P />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.
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.
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.
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.
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.
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.
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.
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<SUP>-1</SUP>
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.
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) M<SUB>sun</SUB> 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.
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.
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.
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.
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.
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.
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.
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: 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: 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: 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 &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: 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: 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.
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.
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: 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: Diagnostics à haute résolution des méso-cellules solaires
au minimum de température.
Authors: Martic, M.
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.
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.
