Domain of validity of a 1D second order perturbative approach for the effects of rotation on stellar oscillations
Abstract
At rotational velocities such as that of upper Main Sequence stars - between 50 to 200 km/s - the effects of rotation on oscillation frequencies must be included. Considering the accuracy reached by available ground-based and space observations, the aim of this study is to determine the limits - in terms of rotational velocity - of a perturbative approach to model the effects of rotation on oscillation frequencies. We thus compare the oscillation frequencies computed by 1D second order perturbative methods to the ones obtained in Reese et al. (2006) - direct integration of a 2D eigenvalue system. To do so, we use polytropic models (N=3) in uniform rotation, and we discuss the results for a β Cephei star (8.2 M_{⊙}, 5.04 R_{⊙}).
- Publication:
-
Communications in Asteroseismology
- Pub Date:
- July 2009
- Bibcode:
- 2009CoAst.158..283O