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Theory of Pulsational Instabilities of Hot Stars

Published online by Cambridge University Press:  12 April 2016

Alexei A. Pamyatnykh
Alexei A. Pamyatnykh*
Affiliation:
Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland Institute of Astronomy, Pyatnitskaya 48, 109017 Moscow, Russia

Abstract

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Basic physical mechanism of the pulsational instability in OB stars is shortly reviewed. Similarities and differences in the driving effect acting in these objects and in the classical pulsating variables are emphasized. Updated theoretical instability domains in the H-R diagram, in the log g – log Teff and in the Period – log Teff diagrams are presented and compared with the observational data on β Cephei, SPB and some other types of hot variables.

Type
Section V Pulsation
Information
International Astronomical Union Colloquium , Volume 169: Variable and Non-spherical Stellar Winds in Luminous Hot Stars , 1999 , pp. 320 - 328
Copyright
Copyright © Springer-Verlag 1999

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