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A New Driving Mechanism of the Episodic Mass-Loss in Be Stars

Published online by Cambridge University Press:  12 April 2016

Hiroyasu Ando
Hiroyasu Ando*
Affiliation:
Tokyo Astronomical Observatory, University of Tokyo, Mitaka, Tokyo181.

Extract

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Be stars are well known to be rapid rotator and to show intermittent emission-line activity. Such an activity is now interpreted as an abrupt mass-ejection and formation of a cool disk in the equatorial region and then its gradual disappearance mass-loss is called as episodic mass-loss.

Rapid rotation and mass-loss connection in Be stars was suggested for the first time by struve(1931), which necessarily leads to the requirement of break-up velocity in Be stars. However, Vsin i statistics suggests almost all Be stars are well below the break-up velocity. The additional forces have been searched for so far; i.e., stellar wind, magnetic field, mass accretion, and so on. At the moment, none of them can succeed in explaining the episodic mass-loss in Be stars.

Type
Part II. Mass-Losing Stars in Different Stages of Evolution
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 154 - 155
Copyright
Copyright © Springer-Verlag 1988

References

Ando, H. 1983, Publ.Astron.Soc.Japan, 15, 343.Google Scholar
Ando, H. 1986, Astron.Astrophys., 163, 97.Google Scholar
Baade, D. 1987, in IAU Coll. No.92, Physics of Be stars, ed. Slettebak, A., Cambridge Univ. Press. Google Scholar
Struve, O. 1931, Astrophys. J., 73, 94.Google Scholar
Willson, L.A. 1986, Publ.Astron.Soc.Pacific, 98, 35.Google Scholar