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Non-Linear Instability of Stars With M > 100 M⊙

Published online by Cambridge University Press:  07 February 2017

J. C. B. Papaloizou  and
R. J. Tayler
J. C. B. Papaloizou*
Affiliation:
Astronomy Centre, University of Sussex, England
R. J. Tayler
Affiliation:
Astronomy Centre, University of Sussex, England
*
Present address: Department of Astrophysics, Oxford, England.

Abstract

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Massive main sequence stars are vibrationally unstable to small perturbations excited in the region of nuclear energy generation. This instability may, however, be limited at finite amplitude. Only the fundamental radial mode is unstable with an e-folding time of 105 to 106 pulsation periods; in contrast the overtones have damping times short compared with the growth time of the fundamental. Non-linear effects couple the linear modes. At very low amplitude the energy transfer time between modes is long compared with both growth and damping times and, as the overtones decay, a pure fundamental should result. However, as the amplitude increases, the transfer time becomes less than the growth and damping times. Energy can then be transferred from the fundamental to the overtones and damping can lead to a limitation of amplitude.

Type
Part III Large Mass Stars, Stability in Supergiants, Critical Masses
Information
Symposium - International Astronomical Union , Volume 59: Stellar Instability and Evolution , 1974 , pp. 77 - 79
Copyright
Copyright © Reidel 1974 

References

Papaloizou, J. C. B.: 1973a, Monthly Notices Roy. Astron. Soc. 162, 143.Google Scholar
Papaloizou, J. C. B.: 1973b, Monthly Notices Roy. Astron. Soc. 162, 169.Google Scholar