Abstract
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
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© 2002 Springer-Verlag Berlin Heidelberg
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Bisnovatyi-Kogan, G.S. (2002). Dynamic Stability. In: Stellar Physics. Astronomy and Astrophysics Library. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-22639-1_6
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DOI: https://doi.org/10.1007/978-3-662-22639-1_6
Publisher Name: Springer, Berlin, Heidelberg
Print ISBN: 978-3-642-08633-5
Online ISBN: 978-3-662-22639-1
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