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Identifying near-IR variable Be stars

Published online by Cambridge University Press:  26 May 2016

S.M. Dougherty  and
A.R. Taylor
S.M. Dougherty
Affiliation:
John Moores University, Liverpool, England
A.R. Taylor
Affiliation:
University of Calgary, Calgary, Canada

Abstract

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Near-IR variable Be stars are identified from multi-epoch observations spanning 20 years using a statistical technique. In this manner, observations from different observing sites can be meaningfully combined and compared. A more thorough investigation of the incidence and properties of IR variability in Be stars as a class of stars is then possible.

Type
6. Be Stars: Circumstellar Environment
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 416 - 417
Copyright
Copyright © Kluwer 1994 

References

Coté, J. and Waters, L.B.F.M., 1987, Astronomy and Astrophysics , 176, 93 Google Scholar
Dougherty, S.M., Waters, L.B.F.M., Burki, G., Coté, J., Cramer, N., van Kerkwijk, M.H., and Taylor, A.R., 1994, Astronomy and Astrophysics, submitted. Google Scholar
Dougherty, S.M., and Taylor, A.R., 1994, Monthly Notices of the RAS, submitted. Google Scholar