Neutrino Reactions on [TSUP]4[/TSUP]H[CLC]e[/CLC] and the [CLC][ITAL]r[/ITAL][/CLC]-Process

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Abstract
Neutrinos from a Kelvin-Helmholtz-cooling neutron star drive the winds in which the r-process of nucleosynthesis possibly occurs. The neutrinos establish the matter expansion rate, the entropy per baryon, and the neutron richness in the wind material. Some models of the nucleosynthesis in neutrino-driven winds have successfully reproduced the solar r-process isotopic patterns and yields. An effect not previously included in these models, however, is the interaction of neutrinos with the abundant 4He nuclei. Such interactions tend to inhibit the r-process by allowing the assembly of too many seed nuclei, thereby destroying the good agreement between model yields and solar system abundances. In order to restore that good agreement, it is necessary to postulate some modification or modifications to current models.

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