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Masses of Magellanic Wolf-Rayet stars: mass loss and evidence for a WR subclass vs. mass relation

Published online by Cambridge University Press:  12 April 2016

A.F.J. Moffat
A.F.J. Moffat*
Affiliation:
Département de Physique, Université de Montréal

Abstract

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New spectroscopic observations in the LMC/SMC combined with published data on Galactic WR stars lead to a correlation between mass ratio, MWR/MO, and WR subclass. As a consequence of this and their high mass loss rates, WR stars probably evolve from cool to hot ionization class in a way which depends on the metallicity.

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. 301 - 305
Copyright
Copyright © Reidel 1981

References

Barlow, M.J. Smith, L.J. Willis, A.J. 1981, this volume.Google Scholar
Conti, P.S. 1976, Mém. Soc. Roy. Sci. Liège,6. Série,9 193.Google Scholar
de Loore, C. 1981, this volume.Google Scholar
Garmany, C.D. Conti, P.S. Massey, P. 1981, preprint.Google Scholar
Hellings, P. Vanbeveren, D. 1981, this volume.Google Scholar
Massey, P. 1981, Ap.J., in press.Google Scholar
Moffat, A.F.J., Seggewiss, W. 1979, A & A 77, 128.Google Scholar
Niemela, V.S. 1981, this volume.Google Scholar
Vanbeveren, D. 1981, this volumeGoogle Scholar
van den Heuvel, E.P.J. 1976, IAU Symp. No. 73, p.35.Google Scholar