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The Evolution of Rapidly Rotating B Stars (Review Paper)

Published online by Cambridge University Press:  23 September 2016

Robert Connon Smith
Robert Connon Smith*
Affiliation:
Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH, U.K.

Abstract

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Be stars are located in or near the main-sequence band for non-rotating stars. Although this stage of evolution is relatively well understood, there are two main effects that make it impossible to say whether all Be stars are in the same stage of evolution and, if so, what that stage is. One effect is the spread in observed magnitude and colour as a result of rotation. Correction for rotation is not possible because of the unknown inclination of any particular star's rotation axis to the line of sight and because it is not clear what the internal angular momentum distribution is or how it changes as a result of evolution. The other effect is that there are uncertainties in the theoretical evolutionary tracks because the amount of convective overshooting is unclear. Other mixing mechanisms that might in principle also confuse the tracks seem to be small near the main sequence. If Be stars are related to the β Cephei and 53 Persei stars in the same part of the HR diagram, then the non-radial pulsation properties of Be stars may give a clue to their evolutionary state. The existence of a circumstellar disc or ring, however, tells us very little about the evolutionary stage of the underlying star. A useful way forward may be to try to understand individual stars in as much detail as possible.

Type
V. Evolutionary Status of Be Stars
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 486 - 499
Copyright
Copyright © Cambridge University Press 1987

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