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Spectral Analyses of Wolf-Rayet Stars: The Impact of Clumping

Published online by Cambridge University Press:  12 April 2016

Wolf-Rainer Hamann  and
Lars Koesterke
Wolf-Rainer Hamann
Affiliation:
Universität Potsdam, Am Neuen Palais 10, D-14469 Potsdam, Germany
Lars Koesterke
Affiliation:
Universität Potsdam, Am Neuen Palais 10, D-14469 Potsdam, Germany

Abstract

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Inhomogeneities are accounted for in our non-LTE stellar wind models in a first-order approximation. When applied for spectral analyses, clumpy models yield lower mass-loss rates than homogeneous models, while other parameters are not affected. For representative WR stars, we determine the density contrast from the electron-scattering line wings and obtain mass-loss rate reductions by a factor of two, typically.

Type
Section III Variable Winds
Information
International Astronomical Union Colloquium , Volume 169: Variable and Non-spherical Stellar Winds in Luminous Hot Stars , 1999 , pp. 239 - 242
Copyright
Copyright © Springer-Verlag 1999

References

Hamann, W.-R., Koesterke, L., 1998a, A&A 333, 251 Google Scholar
Hamann, W.-R., Koesterke, L., 1998b, A&A 335, 1003 Google Scholar
Hillier, D.J., 1984, ApJ 280, 744 CrossRefGoogle Scholar
Schmutz, W., Hamann, W.-R., Wessolowski, U., 1989, A&A 210, 236 Google Scholar