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On the Chemical Abundances, Evolutionary Stage and Bolometric Magnitude of WR Stars

Published online by Cambridge University Press:  14 August 2015

D. Vanbeveren
D. Vanbeveren*
Affiliation:
Astrophysical Institute, Vrije Universiteit Brussel, Brussels, Belgium

Extract

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I will comment on 3 problems concerning WR stars:

  1. a. are WR stars core hydrogen/core helium burning?

  2. b. are WR stars H-poor or do they have normal abundances?

  3. c. can we use B.C. for WR stars which are similar as for 0 stars?

Type
SESSION 2 — THE CHEMISTRY OF THE WOLF-RAYET STARS
Information
Symposium - International Astronomical Union , Volume 99: Wolf-Rayet Stars: Observations, Physics, Evolution , 1982 , pp. 117 - 120
Copyright
Copyright © Reidel 1982 

References

Maeder, A. 1981, Astron. Astrophys. (in press).Google Scholar
Noels, A., Conti, P.S., Gabriel, M., Vreux, J.M. 1980, Astron. Astrophys. 92, 242.Google Scholar
Underhill, A.B. 1980, Astrophys. J. 239, 220.Google Scholar
Underbill, A.B. 1981, Astrophys. J. 244, 963.Google Scholar