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Mass loss and evolution of massive stars in the Magellanic Clouds

Published online by Cambridge University Press:  19 July 2016

Claus Leitherer  and
Norbert Langer
Claus Leitherer
Affiliation:
STScI, 3700 San Martin Drive, Baltimore, MD 21218. Affiliated with the Astrophysics Division, Space Science Department of ESA
Norbert Langer
Affiliation:
Universitätssternwarte, Geismarlandstrasse 11, D-3400 Göttingen, Germany

Abstract

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The structure and evolution of massive stars is significantly influenced by effects of chemical composition in a low-metallicity environment (as compared to the solar neighbourhood, SN), such as the Magellanic Clouds. A fundamental ingredient in evolutionary models is the stellar mass-loss rate M. Lower metal content decreases the mass-loss rates derived theoretically, which in turn affects the stellar evolution models. On the other hand, different evolutionary models predict different stellar parameters (especially L), which again influence M so that an iterative procedure is required to achieve self-consistency.

Type
The LMC-SMC-Galaxy System
Information
Symposium - International Astronomical Union , Volume 148: The Magellanic Clouds , 1991 , pp. 480 - 482
Copyright
Copyright © Kluwer 1991 

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