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Evolution of a 30 Mʘ star: the interplay of nuclear burning and mass loss

Published online by Cambridge University Press:  12 April 2016

H.J. Falk  and
R. Mitalas
H.J. Falk*
Affiliation:
University of Western Ontario, London, Canada
R. Mitalas
Affiliation:
University of Western Ontario, London, Canada
*
*present address: University of Sussex, Brighton,U.K.

Abstract

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Evolutionary tracks for a 30 Mʘ star with various mass loss rates (MLR) were evolved to core He exhaustion. The “overluminosity” of mass losing (ML) stars is explained in terms of the well known mass-luminosity (M-L) law. A critical ZAMS MLR above which mass loss leads to evolution to fainter luminosities is derived. Two tracks showed reversals in their direction of evolution across the HR diagram. These have been shown to be a consequence of mass loss dominating over the effects of the shell source. An analytic criterion for this condition has been derived.

Type
Session V - Mass Loss and Stellar Evolution: Massive Stars
Information
International Astronomical Union Colloquium , Volume 59: Effects of Mass Loss on Stellar Evolution , 1981 , pp. 261 - 263
Copyright
Copyright © Reidel 1981

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