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Periodic Variability of Be Stars: Nonradial Pulsation or Rotational Modulation?

Published online by Cambridge University Press:  26 May 2016

D. Baade  and
L.A. Balona
D. Baade
Affiliation:
European Southern Observatory Karl-Schwarzschild-Str. 2, D-85748 Garching bei München, Germany
L.A. Balona
Affiliation:
South African Astronomical Observatory P.O. Box 9, Observatory 7935, Cape Town, South Africa

Abstract

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A large fraction of Be stars show periodic light and line profile variations with a timescale of about one day. The mechanism which causes these periodic variations has been attributed to nonradial pulsation (NRP) or rotational modulation (RM). The authors present arguments supporting the two opposing points of view with the purpose of stimulating subsequent discussion by the Symposium participants.

Type
5. Be Stars: Spectroscopy and Photometry
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 311 - 324
Copyright
Copyright © Kluwer 1994 

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