Evolution of the Most Massive Stars
André Maeder, Georges Meynet, Raphael Hirschi
Abstract
We discuss the physics of the ΩΓ-- Limit, i.e. when the star is unbound as a result of both rotation and radiation pressure. We suggest that the ΩΓ-- 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.
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