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Evolution of the Most Massive Stars

André Maeder·Georges Meynet·Raphael Hirschi
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Abstract

We discuss the physics of the $ΩΓ$-- Limit, i.e. when the star is unbound as a result of {\emph{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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André Maeder, Georges Meynet, Raphael Hirschi. 2004-08-18. Evolution of the Most Massive Stars. https://arxiv.org/abs/astro-ph/0408320

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