The nu-process

Details The nu-process The nu-process

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...356..272w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 356, June 10, 1990, p. 272-301. Research supported by the Los Alamos Nation

Astronomy and Astrophysics

Astrophysics

405

Neutrinos, Neutron Stars, Nuclear Astrophysics, Nuclear Fusion, Supernovae, Cosmic Rays, Heavy Elements, Stellar Envelopes, Stellar Interiors, Stellar Mass

Scientific paper

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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