Stellar Pulsations and Stability

  • G. S. Bisnovatyi-Kogan
Part of the Astronomy and Astrophysics Library book series (AAL)


Being a dynamical system, the star has diverse oscillatory eigenmodes. When account is taken of thermal processes, some of these appear to be unstable. The increment of such an instability γ, equal to the inverse time scale of the amplitude increase by a factor of e, is usually well below the pulsational frequency ω. Other modes can be unstable in the adiabatic approximation as well, as in the case of convective instability (9.1.2b), for dS/dr < 0.


Massive Star Oscillation Cycle Stellar Mass Radial Oscillation Phase Core 
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Copyright information

© Springer-Verlag Berlin Heidelberg 2002

Authors and Affiliations

  • G. S. Bisnovatyi-Kogan
    • 1
  1. 1.Space Research InstituteRussian Academy of SciencesMoscowRussia

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