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Difference between Be stars and shell stars from Hα emission

Published online by Cambridge University Press:  26 May 2016

H. Chen  and
A. R. Taylor
H. Chen
Affiliation:
Department of Physics and Astronomy University of Calgary, Canada
A. R. Taylor
Affiliation:
Department of Physics and Astronomy University of Calgary, Canada

Abstract

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We examine Hα equivalent widths versus spectral-types for 41 Be stars. Although the Wα value is scattered for a given spectral-type, a well-defined upper limit exists. Most shell stars are located in the upper limit region. The shell stars all have v sin i/vcri larger than the normal Be stars in the upper limit region. This strongly suggests that the distinction between shell stars and normal Be stars of high equivalent width is a result of variation in inclination angle i. Polarization data also support this hypothesis.

Type
6. Be Stars: Circumstellar Environment
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 354 - 355
Copyright
Copyright © Kluwer 1994 

References

The References

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