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Rotation and Evolution of Be Stars

Published online by Cambridge University Press:  12 April 2016

Johannes Hardorp  and
Peter A. Strittmatter
Johannes Hardorp
Affiliation:
Institute of Theoretical Astronomy, Cambridge, England
Peter A. Strittmatter
Affiliation:
Mt. Stromlo and Siding Spring Observatories, Canberra, Australia, and Institute of Theoretical Astronomy, Cambridge, England

Abstract

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The evidence in favor of the hypothesis that Be stars owe their emission properties to material rotationally ejected from the equator is reviewed. The evolutionary state of Be Stars is then discussed with reference to evolutionary sequences of stellar models. It is concluded that (i) Be stars are not confined to the secondary contraction phase as previously proposed (ii) evolution probably proceeds with uniform rotation at least outside the initial convective core. Mechanisms for transporting angular momentum are briefly discussed.

Type
Part I / The Effects of Rotation on Stellar Interiors and Evolution
Information
International Astronomical Union Colloquium , Volume 4: Stellar Rotation , 1970 , pp. 48 - 59
Copyright
Copyright © Reidel 1970

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