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Long–term Variability of π Aqr

Published online by Cambridge University Press:  12 April 2016

K.S. Bjorkman ,
A.S. Miroshnichenko ,
D.A. McDavid  and
T.M. Pogrosheva
K.S. Bjorkman
Affiliation:
Ritter Observatory, University of Toledo, Dept. of Physics and Astronomy, Toledo, OH 43606, USA
A.S. Miroshnichenko
Affiliation:
Ritter Observatory, University of Toledo, Dept. of Physics and Astronomy, Toledo, OH 43606, USA
D.A. McDavid
Affiliation:
Limber Observatory, Pipe Creek, TX 78063-3599, USA
T.M. Pogrosheva
Affiliation:
Fesenkov Astrophysical Institute of the Kazakhstan Academy of Sciences, 480068, Kamenskoye plato, Almaty, Kazakhstan

Abstract

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We present our recent photometric and spectroscopic observations of the bright classical Be star π Aquarii and analyse those available in literature. This star currently shows only weak signs of circumstellar emission and a low optical brightness. Physical parameters of the underlying star are determined from data obtained during quiescence, while those of its circumstellar disk are estimated during the active period.

Type
6. Disks
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 535 - 538
Copyright
Copyright © Astronomical Society of the Pacific 2000

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