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On Expected Constraints on Stellar Transport Processes from Space Seismic Missions: EVRIS, COROT

Published online by Cambridge University Press:  12 April 2016

M.J. Goupil ,
E. Michel ,
S. Cassisi ,
W.A. Dziembowski ,
Y. Lebreton ,
A. Baglin ,
M. Auvergne  and
C. Catala
M.J. Goupil
Affiliation:
Observatoire de Paris, URA 335, 92190 Meudon, France
E. Michel
Affiliation:
Observatoire de Paris, URA 335, 92190 Meudon, France
S. Cassisi
Affiliation:
Observatoire de Paris, URA 335, 92190 Meudon, France
W.A. Dziembowski
Affiliation:
Copernicus Astronomical Center, 00-716 Warsaw, Poland
Y. Lebreton
Affiliation:
Observatoire de Paris, URA 335, 92190 Meudon, France
A. Baglin
Affiliation:
Observatoire de Paris, URA 335, 92190 Meudon, France
M. Auvergne
Affiliation:
Observatoire de Paris, URA 335, 92190 Meudon, France
C. Catala
Affiliation:
Observatoire de Midi-Pyrénées, 31400 Toulouse, France

Extract

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The first space seismological experiment, EVRIS (Baglin 1991) will be launched in 1996 and will observe ∼ 10 stars over ∼ 20 days each. A second one, COROT (Catala et al., 1994), should follow soon after (1999-2000), which should monitore ∼ 5 stars over ∼ 5 months each. The observed stars will be main sequence stars. For an optimum scientific outcome of EVRIS mission, one must select the best possible target stars. The first step of this selection is outlined. What would be further gained with COROT project is discussed.

Specifications of both missions imply that among possible target stars, δ Scuti stars should present a large number of self excited modes, likely many more than presently observed from ground based networks.

Type
Part 2. Poster Papers
Information
International Astronomical Union Colloquium , Volume 155: Astrophysical Applications of Stellar Pulsation , 1995 , pp. 453 - 454
Copyright
Copyright © Astronomical Society of the Pacific 1995

References

Baglin, A., 1991, Solar Physics, 132, 155 Google Scholar
Cassisi, S., Baglin, A., Michel, E., & Goupil, M.J., 1995 in prep.Google Scholar
Catala, C. et al., 1994, GONG 94 Conf., ASP Conf. Series, in pressGoogle Scholar
Goupil, M.J, Diembowski, W.A., Goode, P., & Michel, E., 1995, A&A, submittedGoogle Scholar
Gough, D.O., 1990, Lecture Notes in Physics 367, Eds Osaki, Y., Shibahashi, H., Springer Verlag, p. 283 Google Scholar
Lebreton, Y., Michel, E., Goupil, M.J., & Baglin, A., 1994, in ‘Stellar age determinations and accurate parallaxes’, IAU Symp. 166 Google Scholar