Hostname: page-component-cd9895bd7-gxg78 Total loading time: 0 Render date: 2024-12-26T04:01:26.131Z Has data issue: false hasContentIssue false
  • English
  • Français

Spectral Analysis of the Wolf-Rayet Star HD 50896

Published online by Cambridge University Press:  12 April 2016

W.-R. Hamann ,
W. Schmutz  and
U. Wessolowski
W.-R. Hamann
Affiliation:
Institut für Theoretische Physikund Sternwarte derUniversität KielOlshausenstrasse, Federal Republic of Germany
W. Schmutz
Affiliation:
Institut für Theoretische Physikund Sternwarte derUniversität KielOlshausenstrasse, Federal Republic of Germany
U. Wessolowski
Affiliation:
Institut für Theoretische Physikund Sternwarte derUniversität KielOlshausenstrasse, Federal Republic of Germany

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.

The helium spectrum of the WN5 star HD 50896 (EZ Canis Majoris, WR6) is studied. Our aim is to establish a technique which allows the determination of the parameters of a Wolf-Rayet star from a systematic analysis of its spectral lines. Since the method of “iteration with approximate Lambda operators” became available for application to expanding atmospheres (Hamann, 1986, 1987), we are now able to compare observed spectra to realistic model calculations (Hamann and Schmutz, 1987; Wessolowski et al., 1987).

We consider the non-LTE spectral formation in a spherically expanding atmosphere. The velocity field v(r) is specified in its supersonic part by the usual analytical law with the parameters v∞ (final velocity) and the exponent ß=1. The temperature structure is derived from the assumption of radiative equilibrium, but only approximately evaluated for the grey LTE case. The atmosphere is assumed to consist of pure helium. The model atom has a total of 28 energy levels, among these 17 levels of He I. The line radiation transfer is treated in the “comoving frame”.

Type
Part II. Mass-Losing Stars in Different Stages of Evolution
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 145 - 147
Copyright
Copyright © Springer-Verlag 1988

References

Hamann, W.-R.: 1986, Astron. Astrophys. 160, 347 Google Scholar
Hamann, W.-R.: 1987, in “Numerical Radiation Transfer”, Kalkofen, W. (ed.), Cambridge university Press (in press)Google Scholar
Hamann, W.-R., Schmutz, W.: 1987, Astron. Astrophys. 174, 173 Google Scholar
Hillier, D.J.: 1987, Astrophys. J. Suppl. 63, 965 CrossRefGoogle Scholar
Hogg, D.E.: 1982, in “Wolf-Rayet Stars: Observation, Physics, Evolution”, IAU Symp. 99, de Loore, C.W.H. and Willis, A.J. (eds.), Reidel, Dordrecht, p. 221 CrossRefGoogle Scholar
Lundström, I., Stenholm, B.: 1984, Astron. Astrophys. Suppl. Ser. 58, 163 Google Scholar
Maeder, A., Meynet, G.: 1987, Astron. Astrophys. (preprint)Google Scholar
Wessolowski, U., Schmutz, W., Hamann, W.-R.: 1987, Astron. Astrophys. (in press)Google Scholar