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The Evolution of Rapidly Rotating B/Be Stars

Published online by Cambridge University Press:  14 August 2015

A. S. Endal
A. S. Endal*
Affiliation:
Dept. of Physics and Astronomy, Louisiana State University, U.S.A.

Abstract

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Rotation can significantly change the moment-of-inertia of a main sequence star. As a result, the ZAMS rotation rate need only be within ~30% of the critical value in order to reach critical rotation during the hydrogen burning stage. Calculations of the evolution of rotating stars show that the Be stars result from a normal (Maxwellian) distribution of B-star rotation velocities.

Type
V. Rotation and Binarity
Information
Symposium - International Astronomical Union , Volume 98: Be Stars , 1982 , pp. 299 - 302
Copyright
Copyright © Reidel 1982 

References

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