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Observations of Rapid Variability in Be Stars (Review Paper)

Published online by Cambridge University Press:  23 September 2016

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

Abstract

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Photometric and/or spectroscopic variability on time scales of approximately 0.2 to 2 days has been observed in over 40 Be stars, and is suspected in many more. This paper reviews the observational aspects of this phenomenon: both surveys and studies of individual objects. This phenomenon is not easy to study and interpret: (i) the time scale is inconvenient (ii) there have been very few simultaneous photometric and spectroscopic studies of individual objects (iii) the photometric variability is small, often irregular and superimposed on longer-term variability and (iv) the spectroscopic variability is usually observed as absorption line profile variability, which requires special instrumentation. For these and other reasons, there is not yet a universal agreement about the nature of this phenomenon. Nevertheless, it deserves further intensive study, not only because it is common, but also because in one or two stars, there is evidence that the rapid variability may be related (causally perhaps?) to the longer-term variability in these stars - variability whose ultimate cause is still not known.

Type
IIA. The Underlying Stars: Observations
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 49 - 65
Copyright
Copyright © Cambridge University Press 1987

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