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Selfconsistent Models of Winds from Rotating Early-Type Stars – Application to B[e] star winds

Published online by Cambridge University Press:  12 April 2016

P. Petrenz  and
J. Puls
P. Petrenz
Affiliation:
Institute for Astronomy and Astrophysics of the Ludwig-Maximilians-University, Scheinerstr. 1, D - 81679Munich
J. Puls
Affiliation:
Institute for Astronomy and Astrophysics of the Ludwig-Maximilians-University, Scheinerstr. 1, D - 81679Munich

Abstract

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We present results of 2.5-D radiation hydrodynamical simulations of winds from rapidly rotating stars. For the first time, we consider the dependence of the line statistics on local density and radiation temperature implying a spatial variation of the force-multiplier parameters k, α and δ which control the dynamics of the flow.

We apply our models to the problem of disk formation in B[e]-star winds.

Information

Type
6. Disks
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 626 - 631
Copyright
Copyright © Astronomical Society of the Pacific 2000

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