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Monday, July 1 - Session 2 - 17:30 |
An improved photometric mode identification method:
applications to Slowly Pulsating B stars,
![]() ![]() ![]() M.A. Dupret1, R. Garrido2, P. De Cat3,
R. Scuflaire1, and A. Noels1
1 Institut d'Astrophysique et de Géophysique de l'Université de
Liège, 4000 Liège, Belgium
2Instituto de Astrofisica de Andalucia (CSIC), Apartado 3004, 18080 Granada, Spain 3Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, 3001 Heverlee, Belgium
A crucial problem in Asteroseismology is the mode identification,
mainly because the mode selection mechanisms
are not well understood for many kinds of pulsating stars.
Methods of mode identification based on multi-colour photometry
have been developed by different authors~:
Dziembowski 1977, Stamford & Watson 1981, Watson 1988,
Garrido et al. 1990, Heynderickx et al. 1994, Cugier et al. 1994.
We present here an improvement of these methods
based on precise non-adiabatic computations with special care given
to the treatment of the stellar atmosphere (Dupret et al. 2002).
We examine how the discriminant power of the method is
affected by the lack of knowledge of stellar parameters such
as the mixing length parameter Cugier, H., Dziembowski, W., Pamyatnykh A., 1994,
A&A 291, 143
Last changed: 2002/Jun/04
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