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Winds of Hot Stars as a Diagnostic Tool of Stellar Evolution

Published online by Cambridge University Press:  12 April 2016

R.P. Kudritzki ,
A. Pauldrach  and
J. Puls
R.P. Kudritzki
Affiliation:
Institut für Astronomieund Astrophysik derUniversität MünchenScheinerstr. 1, D-8000 München 80
A. Pauldrach
Affiliation:
Institut für Astronomieund Astrophysik derUniversität MünchenScheinerstr. 1, D-8000 München 80
J. Puls
Affiliation:
Institut für Astronomieund Astrophysik derUniversität MünchenScheinerstr. 1, D-8000 München 80

Extract

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Modern quantitative spectroscopy of hot stars has two aspects: the analysis of photospheric lines and stellar wind lines. The first one is meanwhile established as an almost classical tool to determine stellar parameters. NLTE model atmosphere and line formation calculations yield Teff, log g and abundances with high precision (see recent reviews by Husfeld (this meeting), Kudritzki (1987), Kudritzki and Hummer (1986), Kudritzki, (1985)). The second aspect, however, the quantitative analysis of stellar wind lines is still at its very beginning. For long time the stellar wind lines have been used to determine mass-loss rates and terminal velocities v∞ only. While these studies were pioneering and of enormous importance, it was also clear that very approximate calculations were done with respect to NLTE ionization and excitation and the radiative transfer in stellar winds. Thus, stellar wind lines could be used only in a more qualitative comparative sense, with no theory behind, which allowed the determination of precise and reliable numbers.

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. 114 - 126
Copyright
Copyright © Springer-Verlag 1988

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