Volume 432, Number 1, March II 2005
|Page(s)||189 - 198|
|Section||Stellar structure and evolution|
|Published online||22 February 2005|
Frequency ratio method for seismic modeling of γ Doradus stars
Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain e-mail: firstname.lastname@example.org
2 LESIA, Observatoire de Paris-Meudon, UMR 8109, 92190 Meudon, France
Accepted: 20 October 2004
A method for obtaining asteroseismological information of a γ Doradus oscillating star showing at least three pulsation frequencies is presented. This method is based on a first-order asymptotic g-mode expression, in agreement with the internal structure of γ Doradus stars. The information obtained is twofold: 1) a possible identification of the radial order n and degree of observed frequencies (assuming that these have the same ), and 2) an estimate of the integral of the buoyancy frequency (Brunt-Väisälä) weighted over the stellar radius along the radiative zone. The accuracy of the method as well as its theoretical consistency are also discussed for a typical γ Doradus stellar model. Finally, the frequency ratios method has been tested with observed frequencies of the γ Doradus star HD 12901. The number of representative models verifying the complete set of constraints (the location in the HR diagram, the Brunt-Väisälä frequency integral, the observed metallicity and frequencies and a reliable identification of n and ) is drastically reduced to six.
Key words: stars: oscillations / stars: interiors / stars: evolution / stars: individual: HD 12901
© ESO, 2005
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