Hostname: page-component-669899f699-rg895 Total loading time: 0 Render date: 2025-05-04T11:50:01.424Z Has data issue: false hasContentIssue false
  • English
  • Français

Observations of Wolf-Rayet Binaries

Published online by Cambridge University Press:  14 August 2015

Virpi S. Niemela
Virpi S. Niemela*
Affiliation:
51 esq. 11, Villa Elisa, Buenos Aires, Argentina

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

In many recent papers dealing with computations of evolutionary sequences for massive stars with mass loss, the evolutionary status of Wolf- Rayet stars has been discussed. When one whishes to compare these theoretical computations with observations, it is of great importance to know the masses of Wolf-Rayet stars, which unfortunately are well determined only in a few cases. Estimates of the masses are provided by binaries with WR type components. I will report here preliminary results of spectrographic observations for 4 WN+OB systems, with new information about the masses of their components.

Type
IV. Massive Binary Systems
Information
Symposium - International Astronomical Union , Volume 88: Close Binary Stars: Observations and Interpretation , 1980 , pp. 177 - 180
Copyright
Copyright © Reidel 1980 

References

Moffat, A.F.J. and Seggewiss, W.: 1979, in IAU Symp. No. 83, eds. Conti, P.S. and de Loore, C.W.H., p.447.CrossRefGoogle Scholar
Munch, G.: 1950, Astrophys.J. 112, p. 226.CrossRefGoogle Scholar
Niemela, V.S.: 1976, Astrophys. and Space Sci. 45, p. 191.CrossRefGoogle Scholar