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Mass loss and the Eddington parameter

Published online by Cambridge University Press:  29 August 2024

Joachim M. Bestenlehner Open the ORCID record for Joachim M. Bestenlehner [Opens in a new window]
Joachim M. Bestenlehner*
Affiliation:
Department of Physics & Astronomy, Hounsfield Road, University of Sheffield, S3 7RH, UK
*
email: j.m.bestenlehner@sheffield.ac.uk
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Abstract

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Mass loss through stellar winds plays a dominant role in the evolution of massive stars. Very massive stars (VMSs, > 100Mȯ) display Wolf-Rayet spectral morphologies (WNh) whilst on the main-sequence. Bestenlehner (2020) extended the elegant and widely used stellar wind theory by Castor, Abbott & Klein (1975) from the optically thin (O star) to the optically thick main-sequence (WNh) wind regime. The new mass-loss description is able to explain the empirical mass-loss dependence on the Eddington parameter and is suitable for incorporation into stellar evolution models for massive and very massive stars. The prescription can be calibrated with the transition mass-loss rate defined in Vink & Gräfener (2012). Based on the stellar sample presented in Bestenlehner et al. (2014) we derive a mass-loss recipe for the Large Magellanic Cloud using the new theoretical mass-loss prescription of Bestenlehner (2020).

Keywords

stars: early-typestars: massivestars: mass lossstars: windsoutflowsstars: atmospheresstars: evolution
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 163 - 167
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

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