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Non-Radial Pulsation In Be Stars

Published online by Cambridge University Press:  30 March 2016

John R. Percy
John R. Percy*
Affiliation:
Erindale College and Department of Astronomy, University of Toronto Toronto, Canada M5S 1A1

Extract

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Be stars are B stars in which emission has been observed in at least one hydrogen line on at least one occasion. Some Be stars are pre-main-sequence stars, mass-transfer binaries, or supergiant stars with extended atmospheres. The majority, however, are classical Be stars: single stars on or near the main sequence. An important characteristic of these stars seems to be their rapid rotation – close to but not at the “critical” velocity at which the effective gravity vanishes at the equator.

Type
Joint Discussions
Information
Highlights of Astronomy , Volume 7: Highlights of Astronomy. As presented at the XIXth General Assembly of the IAU, 1985 , 1986 , pp. 265 - 272
Copyright
Copyright © Reidel 1986

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