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Mass Loss and Stellar Rotation
Published online by Cambridge University Press: 26 May 2016
Abstract
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.
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- Session 4 Rotation and Stellar Evolution
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- Copyright © Astronomical Society of the Pacific 2004
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