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Disks of Classical Be Stars

Published online by Cambridge University Press:  12 April 2016

Stanislav Štefl
Stanislav Štefl*
Affiliation:
Astronomical Institute, Academy of Sciences, CZ-25165 Ondřejov, Czech Republic

Abstract

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Observational methods used in investigation of circumstellar disks of Be stars significantly changed during the last decade. While mostly the studies of line profiles in the optical and near-IR region were used in the 70th and 80th, the present progress is done also thanks to interferometric and polarimetric observations. These techniques enable to determine the geometrical parameters of the circumstellar disks directly for the first time. They are flattened and axially symmetric. Their H α emission region extends typically up to several tens of stellar radii. Systematic long-term spectroscopic monitoring helped to define and partly interpret the line-profile variability of emission lines on different time-scales. Variations on a time-scale of hours may appear after the matter is ejected during the outburst. The V/R variations with periods of the order of 10 years reflect the global disk oscillations.

Type
Section I Observations of Non-spherical Winds
Information
International Astronomical Union Colloquium , Volume 169: Variable and Non-spherical Stellar Winds in Luminous Hot Stars , 1999 , pp. 24 - 31
Copyright
Copyright © Springer-Verlag 1999

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