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Massive star evolution: from the early to the present day Universe

Published online by Cambridge University Press:  01 April 2008

Georges Meynet ,
Sylvia Ekström ,
Cyril Georgy ,
André Maeder  and
Raphael Hirschi
Georges Meynet
Affiliation:
Observatory of Geneva University, Switzerland email: georges.meynet@obs.unige.ch
Sylvia Ekström
Affiliation:
Observatory of Geneva University, Switzerland email: georges.meynet@obs.unige.ch
Cyril Georgy
Affiliation:
Observatory of Geneva University, Switzerland email: georges.meynet@obs.unige.ch
André Maeder
Affiliation:
Observatory of Geneva University, Switzerland email: georges.meynet@obs.unige.ch
Raphael Hirschi
Affiliation:
EPSAM, University of Keele, UK email: r.hirschi@epsam.keele.ac.uk
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Abstract

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Mass loss and axial rotation are playing key roles in shaping the evolution of massive stars. They affect the tracks in the HR diagram, the lifetimes, the surface abundances, the hardness of the radiation field, the chemical yields, the presupernova status, the nature of the remnant, the mechanical energy released in the interstellar medium, etc. . . In this paper, after recalling a few characteristics of mass loss and rotation, we review the effects of these two processes at different metallicities. Rotation probably has its most important effects at low metallicities, while mass loss and rotation deeply affect the evolution of massive stars at solar and higher than solar metallicities.

Keywords

stars: abundancesearly-typeevolutionmass lossemission-lineBerotation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 317 - 327
Copyright
Copyright © International Astronomical Union 2008

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