Dynamic Stability

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


Processes underlying the stellar evolution are characterized by a wide variety of time scales, such as hydrodynamical (т h ), thermal (т th ) and nuclear (т n ) times and a time characterizing the weak interaction rate (т β ). Throughout most of the evolution, from the phase of the young contracting star to the late evolutionary phases, T h remains the smallest of all the time scales. In massive presupernova models, under conditions of nuclear equilibrium, the time scale T n is the smallest one (see Sect. 10.1). In an ordinary star there is a rough equilibrium with respect to rapid processes (static equilibrium, for example), while the evolutionary lifetime is determined by one of the slower processes, as follows


Variational Principle Dynamic Stability White Dwarf Trial Function Thermal Time 
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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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