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Nonradial Oscillations in Zeta Ophiuchi in 1991

Published online by Cambridge University Press:  12 April 2016

E. Kambe ,
H. Ando  and
R. Hirata
E. Kambe
Affiliation:
Department of Geoscience, National Defense Academy, Yokosuka, Kanagawa 239, Japan
H. Ando
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan
R. Hirata
Affiliation:
Department of Astrophysics, Kyoto University, Kitashirakawa, Kyoto 606, Japan

Extract

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The line-profile variations have been found in many early-type stars surrounding the classical β Cephei variables in the H-R diagram. The feature of the variations has not been known enough mainly because of their periods of about one day. To specify the cause of the variations, however, it is necessary to make clear their features such as the multi-periodicity, the relation between the photometric variations and the spectroscopic ones, and the cause of existence or non-existence of mode (or period) switching (Balona 1991, Smith 1991). In Be stars, the correlation of the amplitude of the variations with their emission cycle is also important (Ando 1986).

Type
II. Observational Facts
Information
International Astronomical Union Colloquium , Volume 134: Nonlinear Phenomena in Stellar Variability , 1993 , pp. 219 - 221
Copyright
Copyright © Kluwer 1993

References

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