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: email@example.com
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
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.