Stars are rotating and magnetic bodies. Moreover, more and more constraints are obtained on such dynamical processes using, for example, seismology and spectropolarimetry. Therefore, it is now necessary to get a complete and coherent picture of dynamical processes in stellar interiors. However, to simulate such processes in a star in full details would require treating length scales and time scales spanning many orders of magnitude. This is clearly not feasible, even with the most powerful computers available today. This is the reason why it is nowadays necessary to use and couple 1-D, 2-D, and 3-D modelings to get a global picture of macroscopic MHD transport processes in stellar interiors. In this review, we report the state of the art of the modeling of transport processes in stellar interiors (both in radiation and in convection zones) aimed to study the stars angular momentum history, the related profile of differential rotation, and their magnetism.