Abstract
Weak interactions have been an important part of nuclear astrophysics ever since hydrogen burning in the sun was elucidated. In type II supernovae, ß ± decay and electron capture are extremely important because they determine the electron fraction per nucleon (Ye) of the iron core. The mass of the iron core and the Lagrangian position of shock formation both vary as Y 2e [l],[2]. Also, these reactions create neutrinos which, before core collapse, are able to carry core energy off to infinity. These rates are thus crucial ingredients of the stellar evolution calculation which is the initial model for a type II supernova simulation.
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© 1991 Springer-Verlag New York, Inc.
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Aufderheide, M.B. (1991). Is There Life After Fuller, Fowler & Newman?. In: Woosley, S.E. (eds) Supernovae. Santa Cruz Summer Workshops in Astronomy and Astrophysics. Springer, New York, NY. https://doi.org/10.1007/978-1-4612-2988-9_54
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DOI: https://doi.org/10.1007/978-1-4612-2988-9_54
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