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Rotation and Properties of Be Stars

Published online by Cambridge University Press:  26 May 2016

J. Zorec
J. Zorec*
Affiliation:
Institut d'Astrophysique de Paris, UMR7095/CNRS, 98bis bd. Arago, F-75014 Paris, France ([email protected])

Abstract

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The actual characteristic average surface angular velocity ratio of the Be phenomenon may be higher than Ω/Ωc = 0.8 ± 0.1 derived from v sin i values not corrected from gravity darkening effects. Late Be Stars need not only higher values of Ω/Ωc, but also larger main sequence age ratios τ/τMS than early Be Stars to display the Be phenomenon. Galactic field Be Stars appear at any MS phase, but their frequency is higher for τ/τMS ≳ 0.5. Be Stars are probably neat differential rotators, i.e. they rotate with energy ratios kinetic/|gravitational| larger than withstood by critical rigid rotators. Initial formation conditions must favor the existence of fast rotators, while only a small fraction of them could be accounted for by mass transfer in close binary systems. Bn stars could perhaps represent a pre-Be phase.

Type
Session 1 Observations of Rotating Stars
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 73 - 82
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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