Volume 398, Number 2, February I 2003
|Page(s)||677 - 685|
|Section||Stellar structure and evolution|
|Published online||21 January 2003|
A photometric mode identification method, including an improved non-adiabatic treatment of the atmosphere*
Institut d'Astrophysique et de Géophysique de l'Université de Liège, allée du 6 Août 17, 4000 Liège, Belgium
2 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200, 3001 Leuven, Belgium
Corresponding author: M.-A. Dupret, firstname.lastname@example.org
Accepted: 7 November 2002
We present an improved version of the method of photometric mode identification of Heynderickx et al. ([CITE]). Our new version is based on the inclusion of precise non-adiabatic eigenfunctions determined in the outer stellar atmosphere according to the formalism recently proposed by Dupret et al. ([CITE]). Our improved photometric mode identification technique is therefore no longer dependent on ad hoc parameters for the non-adiabatic effects. It contains the complete physical conditions of the outer atmosphere of the star, provided that rotation does not play a key role. We apply our method to the two slowly pulsating B stars HD 74560 and HD 138764 and to the β Cephei star EN (16) Lac. Besides identifying the degree of the pulsating stars, our method is also a tool for improving the knowledge of stellar interiors and atmospheres, by imposing constraints on parameters such as the metallicity and the mixing-length parameter α (a procedure we label non-adiabatic asteroseismology).
Key words: stars: oscillations / stars: atmospheres / stars: variables: general
© ESO, 2003
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