Abstract
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.
Publisher
Cambridge University Press (CUP)
Cited by
1 articles.
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1. Rotation and Properties of Be Stars;Symposium - International Astronomical Union;2004