Institution(s): 1. University of Geneva
After a brief recall of the physics of rotation, we shall discuss how this physics can be implemented in stellar evolution codes and what are the main calibration processes allowing to constrain some poorly known parameters associated with the description of the turbulence. Models with and without magnetic fields will be discussed. Stellar models predictions will be confronted with observed features. Consequences for the origin of various stellar populations, as red and blue supergiants and Wolf-Rayet stars, of various types of core collapse supernovae will be presented.