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The chemical nature and evolutionary status of the Wolf-Rayet stars

Published online by Cambridge University Press:  14 August 2015

A. J. Willis  and
R. Wilson
A. J. Willis
Affiliation:
Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT
R. Wilson
Affiliation:
Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT

Extract

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Much interest has been shown in recent years concerning the possible link in stellar evolutionary terms between the O-type (particularly Of) and the WR stars, arising from both observational studies of O stars (Conti 1976, Bohannon and Conti 1977) and theoretical studies of the evolution of massive hot stars with high mass loss (Chiosi and Nasi 1974, de Loore et al. 1977, 1978). These investigations and ideas coincided with a renewed attack on the abundance problem in the WR stars based on the acquisition of new ultraviolet observations and the application of recently developed techniques for treating line transfer in rapidly expanding atmospheres (Willis and Wilson 1978a). The aim of this paper is to summarize some of the salient aspects of this latter reference and to examine the evolutionary status of the WR stars in the light of these new results.

Type
Session 8: Evolutionary Scenario and the WR Connection
Information
Symposium - International Astronomical Union , Volume 83: Mass Loss and Evolution of O-Type Stars , 1979 , pp. 461 - 469
Copyright
Copyright © Reidel 1979 

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