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R Coronae Borealis Pulsations

Published online by Cambridge University Press:  12 April 2016

David S. King
David S. King*
Affiliation:
The University of New Mexico, Albuquerque, New Mexico 87131

Abstract

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The Cepheid-like pulsations of some of the R CrB stars should in principle make it possible to determine their masses and hence to place constraints on possible evolution scenarios. We briefly review the evidence for these pulsations and discuss the problem of how these low-mass, hydrogen-deficient carbon stars could have evolved to their present position in the H-R diagram. Linear and nonlinear pulsation calculations are reviewed. It is found that for these large luminosity to mass ratio (L/M) stars a region of pulsation instability extends considerably hotter than for normal high luminosity Cepheids. The envelopes of these models are so nonadiabatic that the identification of modes becomes very difficult since there is frequently no clearly defined nodal structure. For the most extreme L/M cases it is found that the models are unstable in the sense that they appear on the verge of ejecting the outer layers.

Type
VIII. R Coronae Borealis Pulsations
Information
International Astronomical Union Colloquium , Volume 58: Stellar Hydrodynamics , August 1980 , pp. 519 - 527
Copyright
Copyright © Reidel 1980

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