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Mass loss and evolution of hot massive stars

Published online by Cambridge University Press:  01 April 2008

Jorick S. Vink
Jorick S. Vink*
Affiliation:
Armagh Observatory, College Hill, Armagh, BT61 9DG, Northern Ireland, United Kingdom email: [email protected]
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Abstract

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We discuss the role of mass loss for the evolution of the most massive stars, highlighting the role of the predicted bi-stability jump that might be relevant for the evolution of rotational velocities during or just after the main sequence. This mechanism is also proposed as an explanation for the mass-loss variations seen in the winds from Luminous Blue Variables (LBVs). These might be relevant for the quasi-sinusoidal modulations seen in a number of recent transitional supernovae (SNe), as well as for the double-throughed absorption profile recently discovered in the Hα line of SN 2005gj. Finally, we discuss the role of metallicity via the Z-dependent character of their winds, during both the initial and final (Wolf-Rayet) phases of evolution, with implications for the angular momentum evolution of the progenitor stars of long gamma-ray bursts (GRBs).

Keywords

Stars: windsstars: mass lossstars: supergiantsstars: rotationstars: supernovae
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. 271 - 281
Copyright
Copyright © International Astronomical Union 2008

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