Evolution of the Most Massive Stars

We discuss the physics of the $\mathrm{\Omega }\mathrm{\Gamma }$– Limit, i.e. when the star is unbound as a result of {\emph{both}} rotation and radiation pressure. We suggest that the $\mathrm{\Omega }\mathrm{\Gamma }$– Limit is what makes the Humphreys–Davidson Limit. Stellar filiations are discussed, with an emphasis on the final stages, in particular on the final masses, their angular momentum and the chemical yields with account of rotation. A possible relation between WO stars and GRB is emphasized.