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New determinations of the chemical composition of Wolf-Rayet stars

Published online by Cambridge University Press:  07 August 2017

T. Nugis
T. Nugis*
Affiliation:
Tartu Astrophysical Observatory, EE2444 Tõravere, Estonia

Abstract

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The formation of the lines of ions He, H, N and C in the WR stars of different spectral subtypes has been studied using clumped wind models. Our new results agree well with the previous results obtained with smooth wind codes which make use of highly excited lines of different ions.

Keywords

stars: Wolf-Rayetclumped windsabundances
Type
Session II - Model atmospheres for single Wolf-Rayet stars
Information
Symposium - International Astronomical Union , Volume 163: Wolf-Rayet Stars: Binaries, Colliding Winds, Evolution , 1995 , pp. 162 - 163
Copyright
Copyright © Kluwer 1995 

References

Antokhin, I.I., Nugis, T., Cherepashchuk, A.M. 1992, Astron. Zh. 69, 516 Google Scholar
Crowther, P.A. 1993, PhD Thesis, University of London Google Scholar
Hamann, W.-R., Dünnebeil, G., Koesterke, L., Schmutz, W., Wessolowski, U. 1991, A&A 249, 443 Google Scholar
Nugis, T. 1991, in: Michaud, G. & Tutukov, A. (eds.), Evolution of Stars: the Photospheric Abundance Connection, Proc. IAU Symp. No. 145 (Dordrecht: Kluwer), p. 209 Google Scholar
Nugis, T., Niedzielski, A. 1994, A&A submitted Google Scholar