Third Order Effect of Rotation on Stellar Oscillations of a β-Cephei Star

Here the effect of rotation up to third order in the angular velocity of a star on the p, f and g modes is investigated. To do this, the third-order perturbation formalism presented by Soufi et al. (1998) and revised by Karami (2008), was used. I quantify by numerical calculations the effect of rotation on the oscillation frequencies of a uniformly rotating βCephei star with 12 M⊙. For an equatorial velocity of 90 km s , it is found that the secondand third-order corrections for (l,m) = (5,−4), for instance, are of order of 0.07% of the frequency for radial order n = −3 and reaches up to 0.6% for n = −20.