Abstract
Evolving stars pass through consecutive nuclear burning stages. The nuclear ashes, produced by a given nuclear fusion stage, can serve as nuclear fuel for a next burning phase if the temperature is high enough. The maximum temperature that can be attained in the stellar interior depends largely on the total mass of the star. It depends also on this temperature whether or not the produced ‘ashes’ will be ignited for a subsequent nuclear fusion phase.
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Literature
Salpeter, E.E., “Stellar Evolution Leading up to White Dwarfs and Neutron Stars”, in Relativity Theory and Stellar Structure, Lectures in Applied Mathematics, Vol. 10, American Mathematical Socirty, 1967
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Woosley, S.E., 1986,in “Nucleosynthesis and Chemical Evolution”, 16th Advanced Course,Swiss Society of Astrophysics and Astronomy, Saas-Fee, eds. B. Hauck, A. Maeder and G.Meynet
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© 1992 Springer Science+Business Media New York
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De Loore, C.W.H., Doom, C. (1992). Final Stages of Single Star Evolution. In: Structure and Evolution of Single and Binary Stars. Astrophysics and Space Science Library, vol 179. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-2502-4_14
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DOI: https://doi.org/10.1007/978-94-011-2502-4_14
Publisher Name: Springer, Dordrecht
Print ISBN: 978-0-7923-1844-6
Online ISBN: 978-94-011-2502-4
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