Third order effect of rotation on stellar oscillations of a B star

The present paper aims at investigating the effect of rotation up to third order in the angular velocity of a star on p and g modes, based on the formalism developed by Soufi et al. (1998). Our ultimate goal is the study of oscillations of β Cephei stars which are often rapidly rotating stars. Our study shows that the third-order perturbation formalism presented by Soufi et al. (1998) must be 2 K. Karami et al.: Third order effect of rotation corrected for some missing terms and some misprints in the equations. As a first step in our study of β Cephei stars, we quantify by numerical calculations the effect of rotation on the oscillation frequencies of a uniformly rotating zero-age main-sequence star with 12 M⊙. For an equatorial velocity of 100 kms , it is found that the secondand third-order corrections for (l,m) = (2, 2), for instance, are of order of 0.01% of the frequency for radial order n = 6 and reaches up to 0.5% for n = 14.