Differential rotation in intermediate mass stars

Rotation constitutes an important element to take into account when modelling A type and hotter Main Sequence stars. Nowadays, despite the progress made in the treatment of rotation, it remains a significant problem for the analysis of observations from this kind of stars. One of the main problems connected to rotation is the transport of angular momentum in stellar interiors. In this work, I am interested in the study of differential rotation in intermediate mass stars, using the tools given by the asteroseismology. This talk contains preliminary numerical results of adiabatic oscillation frequencies in an intermediate mass star model, using a perturbation method up to the second order, taking into account a radial differential rotation. We show, as we predicted, that $g$ and mixed modes are the most affected by differential rotation. Comparing uniform rotating models with models including a rotation profile given by a local conservation of the angular momentum, we find differences up to 4 microHz in first and second order corrections to the frequency in the mixed modes region, and up to 2 microHz, in the p-modes region. with respect to results obtained for uniform rotating models. This kind of differences can be "observed" with the precissions given by the future data from space (COROT, EDDINGTON, MOST).