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Mass Loss and Stellar Rotation

Published online by Cambridge University Press:  26 May 2016

Henny J.G.L.M. Lamers
Henny J.G.L.M. Lamers*
Affiliation:
Astronomical Institute and SRON Laboratory for Space Research, Utrecht University, Princetonplein 5, NL-3584 CC, Utrecht, the Netherlands, [email protected]

Abstract

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The observational evidence for non-spherical winds of rapidly rotating hot and cool stars is presented. Models to explain equatorially enhanced winds of AGB stars and of hot B[e]-supergiants are discussed. We distinguish between models with a disk due to an increased equatorial mass flux and those with a disk due to spherical mass loss with a wind flowing towards the equatorial plane.

Type
Session 4 Rotation and Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 479 - 490
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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