Mass-Loss Rates of Very Massive Stars

Vink, Jorick S.

doi:10.1007/978-3-319-09596-7_4

Jorick S. Vink³

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 412))

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Abstract

We discuss the basic physics of hot-star winds and we provide mass-loss rates for (very) massive stars. Whilst the emphasis is on theoretical concepts and line-force modelling, we also discuss the current state of observations and empirical modelling, and we address the issue of wind clumping.

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Notes

1.
Note however that these winds are also driven by a myriad of lines, forming a “pseudo” continuum of lines.
2.
Note that for every Fe atom there are as many as 2,500 H atoms (for a solar abundance pattern; see Anders and Grevesse 1989).
3.
Note that Pauldrach et al. (2012) argue that VMS winds remain optically thin.
4.
This might be different for B supergiants below the bi-stability jump (see Petrov et al. 2014).

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Armagh Observatory, Armagh, Ireland
Jorick S. Vink

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Senior Research Astronomer, Armagh Observatory, Armagh, Ireland
Jorick S. Vink

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Vink, J.S. (2015). Mass-Loss Rates of Very Massive Stars. In: Vink, J. (eds) Very Massive Stars in the Local Universe. Astrophysics and Space Science Library, vol 412. Springer, Cham. https://doi.org/10.1007/978-3-319-09596-7_4

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DOI: https://doi.org/10.1007/978-3-319-09596-7_4
Published: 27 September 2014
Publisher Name: Springer, Cham
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