Poster abstract details

We present and discuss results of a recently developped two dimensional non-perturbative method to compute accurate oscillation modes of rapidly rotating stars .
The 2D calculations fully take into account the centrifugal distorsion of the star while the non perturbative method includes the full influence of the Coriolis acceleration. These characteristics give access to the computation of oscillation modes of rapid rotators - from high order p-modes in main sequence stars, to low order p- and g-modes in $\beta$Cephei stars.
We compare the oscillation spectra obtained for centrifugally distorted polytropes with those of Reese et al. (2006), and give the first results for realistic models of stars such as the well studied $\beta$Cephei $\theta$Ophiuci and some main sequence stars observed by the CoRoT mission.