Abstract 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. (Astron. Astrophys. 334:911, 1998) and revised by Karami (Chin. J. Astron. Astrophys. 8:285, 2008), was used. I quantify by numerical calculations the effect of rotation on the oscillation frequencies of a uniformly rotating β-Cephei star with 12 M . For an equatorial velocity of 90 km s −1 , it is found that the second- and 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.
