Monday, July 1 - Session 2 - 17:30

An improved photometric mode identification method: applications to Slowly Pulsating B stars, Cephei, Scuti and Doradus 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 and the limb-darkening law. And finally, we present the results obtained for many Slowly Pulsating B stars, Cephei stars, Scuti stars and Doradus stars.

 

Cugier, H., Dziembowski, W., Pamyatnykh A., 1994, A&A 291, 143
Dupret, M.-A., De Ridder, J., Neuforge C., Aerts C., and Scuflaire R., 2002, A&A 385, 563
Dziembowski, W., 1977, Acta Astron. 27, 203
Garrido, R., Garcia-Lobo, E., \& Rodriguez, E., 1990, A&A, 234, 262
Heynderickx, D., Waelkens, C., Smeyers, P., 1994, A&AS 105, 447
Stamford, P.A., Watson, R.D., 1981, Ap&SS 77, 131
Watson, R.D., 1988, Ap&SS 140, 255

 
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