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Mass loss in 2D rotating stellar models

Published online by Cambridge University Press:  12 July 2011

Catherine Lovekin  and
Robert G. Deupree
Catherine Lovekin
Affiliation:
LESIA, Observatoire de Paris, 5 Place Jules Janssen, 92195 Meudon, France email: clovekin@lanl.gov
Robert G. Deupree
Affiliation:
Institute for Computational Astrophysics, Saint Mary's University, 923 Robie St, Halifax, NS B3H 3C3, Canada
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Abstract

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Radiatively driven mass loss is an important factor in the evolution of massive stars. The mass loss rates depend on a number of stellar parameters, including the effective temperature and luminosity. Massive stars are also often rapidly rotating, which affects their structure and evolution. In sufficiently rapidly rotating stars, both the effective temperature and surface flux vary significantly as a function of latitude, and hence mass loss rates can vary appreciably between the poles and the equator. In this work, we discuss the addition of mass loss to a 2D stellar evolution code (ROTORC) and compare evolution sequences with and without mass loss.

Keywords

stars: evolutionstars: mass lossstars: rotation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 93 - 94
Copyright
Copyright © International Astronomical Union 2011

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