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Modelling of line-profile variability in WC stars

Published online by Cambridge University Press:  25 May 2016

Lydia M. Oskinova ,
Alexander F. Kholtygin  and
F.V. Kostenko
Lydia M. Oskinova
Affiliation:
Department of Physics and Astronomy, University of Glasgow, UK
Alexander F. Kholtygin
Affiliation:
Astronomical Institute, St. Petersburg University, Russia
F.V. Kostenko
Affiliation:
Astronomical Institute, St. Petersburg University, Russia

Extract

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Suppose that the atmosphere of a WC star is formed by clumps embedded in the homogeneous spherically symmetric stellar wind. A single clump may be modeled as a part of the spherical layer restricted with a surface of a cone. Present the gas density in the cone as a sum of gas density in homogeneous atmosphere and gas density in a clump: Here nk(r) is the gas density in the homogeneous atmosphere, Dcl is the ratio of gas densities at a point r = rcl, and δ is the size of the clumps in units rcl.

Type
Part 2. Models for single star evolution of massive stars: wind + atmosphere + interior
Information
Symposium - International Astronomical Union , Volume 193: Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies , 1999 , pp. 258 - 259
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

Kholtygin, A.F., Kostenko, F.V. 1998, Astrofizika 41, 423 Google Scholar
Moffat, A.F.J., Lépine, S., Henriksen, R.N., Robert, C. 1994, ApSS 216, 55 Google Scholar