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The Short-Period Photometric Variability of Be Stars

Published online by Cambridge University Press:  23 September 2016

L.A. Balona  and
C.A. Engelbrecht
L.A. Balona
Affiliation:
South African Astronomical Observatory, P.O. Box 9, Observatory 7935, Cape, South Africa
C.A. Engelbrecht
Affiliation:
South African Astronomical Observatory, P.O. Box 9, Observatory 7935, Cape, South Africa

Extract

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The fact that some Be stars have periodic light vanations with time scales of the order of one day is well established (eg. Balona and Engelbrecht 1986). The cause of this variability is not yet understood. The explanation which seems to have gained the most acceptance is nonradial pulsation (NRP). It is of great importance to ascertain the proportion of Be stars which are short-period variables and to determine the link between the variations and the emission-line phase. We have started a photometric project to investigate these problems. In this note we present some preliminary results and tentative conclusions.

Type
IIA. The Underlying Stars: Observations
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 87 - 89
Copyright
Copyright © Cambridge University Press 1987

References

Balona, L.A. & Engelbrecht, C.A. (1986). Mon. Not. R. astr. Soc., 219, 131.Google Scholar
Bolton, C.T. (1981). Be stars (IAU symp. 98 ed. Jascheck, M. & Groth, H-G.) Reidel, 181.Google Scholar
Stellingwerf, R. (1978). Astrophys. J., 224, 953.CrossRefGoogle Scholar