  Very high precision seismic space missions such as CoRoT and Kepler provide
the means of testing the modeling of transport processes in stellar interiors.
For some stars, such as solar-like and red giant stars, a rotational splitting
is measured. However, in order to fully exploit these splittings and constrain
the rotation profile, one needs to be able to calculate them accurately. For
some other stars, such as $\delta$ Scuti and Be stars, for instance, the
observed pulsation spectra are modified by rotation to such an extent that a
perturbative treatment of the effects of rotation is no longer valid. We
present here a new two-dimensional non-perturbative code, called ACOR
(\textit{Adiabatic Code of Oscillation including Rotation}) which allows us to
compute adiabatic non-radial pulsations of rotating stars, without making any
assumptions on the sphericity of the star, the fluid properties (i.e.
baroclinicity) or the rotation profile. The 2D non-perturbative calculations
fully take into account the centrifugal distortion of the star and include the
full influence of the Coriolis acceleration. The numerical method is based on a
spectral approach for the angular part of the modes, and a fourth-order finite
differences approach for the radial part. We test and evaluate the accuracy of
the calculations by comparing them with those coming from TOP
(\textit{Two-dimensional Oscillation Program}) for the same polytropic models.
We illustrate the effects of rapid rotation on stellar pulsations through the
phenomenon of avoided crossings. As shown by the comparison with TOP for simple
models, the code is stable, and gives accurate results up to near-critical
rotation rates.
