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Non-spherical Radiation-Driven Wind Models

Published online by Cambridge University Press:  12 April 2016

Joachim Puls ,
Peter Petrenz  and
Stanley P. Owocki
Joachim Puls
Affiliation:
Universitätssternwarte, Scheinerstraße 1, D-81679 München, Germany
Peter Petrenz
Affiliation:
Universitätssternwarte, Scheinerstraße 1, D-81679 München, Germany
Stanley P. Owocki
Affiliation:
Bartol Research Institute of the University of Delaware, Newark, DE 19716, USA

Abstract

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The present state of modelling radiatively driven stellar winds from rapidly rotating stars is reviewed. Various processes affecting the actual, still controversial wind structure are highlighted, in particular non-radial line-forces and gravity darkening, and useful scaling relations are provided. The importance of accounting for consistent NLTE line-forces depending both on the actual density structure and radiation field (as function of latitude and radius) is stressed, and some independent test calculations confirming earlier numerical results are reported.

Type
Section II Theory of Non-spherical Winds
Information
International Astronomical Union Colloquium , Volume 169: Variable and Non-spherical Stellar Winds in Luminous Hot Stars , 1999 , pp. 131 - 139
Copyright
Copyright © Springer-Verlag 1999

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