Stellar rotation has several effects on stellar structure. It induces instabilities that mix chemical elements and angular momentum, deforms the star through the centrifugal force, and, together with convection, generates a dynamo that maintains stellar activity. Understanding how angular momentum is distributed in stellar radiation zones is therefore important to measure stellar ages, model surface chemical evolution and understanding the evolution of stellar activity.

New results from the space missions CoRoT and Kepler have provided stringent asteroseismic constraints on the internal rotation of several types of stars. They have shown the inadequacy of current modelling of transport of angular momentum inside stars. In this talk I will describe the mechanisms of transport of angular momentum in stellar radiative zones, and how they are currently included in stellar evolution codes. I will outline our current efforts to solve the stellar rotation problem, and how we are developing them in the stellar evolution code CESTAM.