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The nu-process
Woosley, S. E.; Hartmann, D. H.; Hoffman, R. D.; Haxton, W. C.
AA(Lick Observatory, Santa Cruz; Lawrence Livermore National Laboratory, Livermore, CA), AB(Lick Observatory, Santa Cruz; Lawrence Livermore National Laboratory, Livermore, CA), AC(San Francisco State University, CA), AD(Washington, University, Seattle)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 356, June 10, 1990, p. 272-301. Research supported by the Los Alamos National Laboratory and University of California. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Neutrinos, Neutron Stars, Nuclear Astrophysics, Nuclear Fusion, Supernovae, Cosmic Rays, Heavy Elements, Stellar Envelopes, Stellar Interiors, Stellar Mass
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As the core of a massive star collapses to form a neutron star, the flux of neutrinos in the overlying shells of heavy elements becomes so great that, despite the small cross section, substantial nuclear transmutation is induced. Neutrinos excite heavy elements and even helium to particle unbound levels. The evaporation of a single neutron or proton, and the back reaction of these nucleons on other species present, significantly alters the outcome of traditional nucleosynthesis calculations leading to a new process: nu-nucleosynthesis. Modifications to traditional hydrostatic and explosive varieties of helium, carbon, neon, oxygen, and silicon burning are considered. The results show that a large number of rare isotopes, including many of the odd-Z nuclei from boron through copper, owe much of their present abundance in nature to this process.

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