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The Onset of Quasi-Periodic Variations in Be Stars

Published online by Cambridge University Press:  12 April 2016

T. Kogure ,
M. Mon  and
M. Suzuki
T. Kogure
Affiliation:
Department of Astronomy, Faculty of Science, Kyoto University, Sakyo-ku, Kyoto 601-01, Japan
M. Mon
Affiliation:
Department of Astronomy, Faculty of Science, Kyoto University, Sakyo-ku, Kyoto 601-01, Japan
M. Suzuki
Affiliation:
Kanazawa Institute of Technology, Kanazawa 921, Japan

Extract

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We present some evidence of the quasi-periodic long-term variations (QPLV) in the violet-to-red ratio of double-peaked emission lines (V/R variation) and/or in the radial velocities of shell absorption lines for some Be stars. Although the V/R variations are rather prevailing phenomena among Be stars, the QPLV is remarkable by the following characteristics:

  1. (1) The QPLV appears as a sudden onset of repeated V/R variations after a long (10 years), almost stable period, and it persists for a few or several periods in ten or more years.

  2. (2) The period and amplitude of V/R variations change from cycle to cycle and from star to star. The variations of radial velocities (RV) of shell absorption lines are usually nearly parallel with the V/R variations.

  3. (3) The QPLV appears usually in early type Be stars with large rotational velocities, regardless whether the stars are normal Be or shell stars, and whether they are close-binaries or single stars.

Type
II. Observational Facts
Information
International Astronomical Union Colloquium , Volume 134: Nonlinear Phenomena in Stellar Variability , 1993 , pp. 223 - 225
Copyright
Copyright © Kluwer 1993

References

References:

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