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Are There Different Types of Variability Among B Stars?

Published online by Cambridge University Press:  12 April 2016

J.-P. Sareyan ,
J.-M. Le Contel ,
J.-C. Valtier  and
D. Ducatel
J.-P. Sareyan
Affiliation:
Nice Observatory, B.P.n° 252, 06007 Nice Cedex, France
J.-M. Le Contel
Affiliation:
Nice Observatory, B.P.n° 252, 06007 Nice Cedex, France
J.-C. Valtier
Affiliation:
Nice Observatory, B.P.n° 252, 06007 Nice Cedex, France
D. Ducatel
Affiliation:
Nice Observatory, B.P.n° 252, 06007 Nice Cedex, France

Extract

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Almost every survey for β Cephei detection has been restricted to the small area of the HR diagram that contained the 15-20 first discovered. (Table 1). Of course, every new short period pulsating star found in such an a priori limited region has strengthened the impression that an instability box could be derived from the study of the statistics of β Cep variables. That conclusion could have led to the discovery of a β Cep pulsation mechanism related to a particular mass - age internal structure status. On the contrary if the phenomenon is due to a mechanism acting in a wider extension of the HR diagram (and so probably better related to envelope properties) one still has to explain why its detection seems to be easier in the B0-B1 zone. Moreover, even within the “instability box” some classical β Cep could be either in core hydrogen burning phase or others in shell hydrogen burning phase, i.e. with quite different internal structures.

Type
III. β-Cephei and 53 Persei Variables
Information
International Astronomical Union Colloquium , Volume 58: Stellar Hydrodynamics , August 1980 , pp. 353 - 359
Copyright
Copyright © Reidel 1980

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