Stellar Pulsations and Stability
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.
KeywordsMassive Star Oscillation Cycle Stellar Mass Radial Oscillation Phase Core
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