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Dynamic Stability

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Abstract

Processes underlying the stellar evolution are characterized by a wide variety of time scales, such as hydrodynamical (τh), thermal (τth), and nuclear (τn) times, and a time characterizing the weak interaction rate (τβ). Throughout most of the evolution, from the phase of the young contracting star to the late evolutionary phases, τh remains the smallest of all the time scales.

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Notes

  1. 1.

    Equation (10.1) implies m = m 0 since only the rest mass is gravitating in Newtonian theory.

  2. 2.

    When S ≠ 0, the phase transitions are assumed to occur at S = const. The validity of this assumption is not obvious, it is only a rough method for describing a phase transition.

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Authors and Affiliations

  1. Space Research Institute, Russian Academy of Sciences, Profsoyuznaya Str. 84/32, 117997, Moskva, Russia

    Dr. Gennady S. Bisnovatyi-Kogan

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  1. Dr. Gennady S. Bisnovatyi-Kogan
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Correspondence to Gennady S. Bisnovatyi-Kogan .

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Bisnovatyi-Kogan, G.S. (2010). Dynamic Stability. In: Stellar Physics. Astronomy and Astrophysics Library. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-14734-0_6

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  • DOI: https://doi.org/10.1007/978-3-642-14734-0_6

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