We briefly report on an ongoing numerical project that aims at simulating, with the ASH code, the intricate magnetohydrodynamic processes present in the inner region of A-type stars. We mainly focus our attention, on the dynamics of the convective core, its associated differential rotation and meridional ciculation and the dynamo action than can occur in such tubulent MHD system. We indeed find that magnetic fields with amplitude greater than 10 kG are likely to be present in the core of A-type stars.