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Physics of Mass Loss in Massive Stars

Published online by Cambridge University Press:  23 January 2015

Joachim Puls ,
Jon O. Sundqvist  and
Nevena Markova
Joachim Puls
Affiliation:
Universitätssternwarte, Scheinerstr. 1, D-81679 München; Germany email: uh101aw@usm.uni-muenchen.de
Jon O. Sundqvist
Affiliation:
Universitätssternwarte, Scheinerstr. 1, D-81679 München; Germany email: uh101aw@usm.uni-muenchen.de
Nevena Markova
Affiliation:
Institute of Astronomy with NAO, BAS, PO Box 136, 4700 Smolyan, Bulgaria
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Abstract

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We review potential mass-loss mechanisms in the various evolutionary stages of massive stars, from the well-known line-driven winds of O-stars and BA-supergiants to the less-understood winds of Red Supergiants. We discuss optically thick winds from Wolf-Rayet stars and Very Massive Stars, and the hypothesis of porosity-moderated, continuum-driven mass loss from stars formally exceeding the Eddington limit, which might explain the giant outbursts from Luminous Blue Variables. We finish this review with a glance on the impact of rapid rotation, magnetic fields and small-scale inhomogeneities in line-driven winds.

Keywords

stars: early-typestars: mass lossstars: windsoutflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 25 - 36
Copyright
Copyright © International Astronomical Union 2015 

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