Neutrino capture by nuclei and the neutrino pulse from a supernova

Details Neutrino capture by nuclei and the neutrino pulse from a supernova Neutrino capture by nuclei and the neutrino pulse from a supernova

May 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...328..691s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 328, May 15, 1988, p. 691-698.

Statistics

Computation

6

Gravitational Collapse, Neutrinos, Neutron Stars, Nuclear Capture, Stellar Interiors, Computational Astrophysics, Cross Sections, Energy Dissipation, Exothermic Reactions, Mean Free Path, Nuclear Astrophysics

Scientific paper

The absorption of electron neutrinos in hot nuclei embedded in a dense medium typical of the outer regions of a neutron star, the regions which comprise the neutrino 'photosphere' in the first seconds after collapse is calculated. The model used for the nuclear transition strength is a generalization of that used by Bethe et al. (1979), whose model basically counts the states as in a Fermi gas but concentrates the transition strength in a state (or a cluster of states) at a particular energy. The generalization is to the case of nonzero temperature and allows the transition strength to be distributed over a range in energies. The resulting neutrino opacities are large in comparison to those resulting from other processes in matter at the same densities. Of note is the fact that the opacities are non-vanishing in the limit of zero neutrino energy. The implications of the new results for the calculation of the spectrum of the neutrinos emitted in the first few seconds after the stellar collapse are discussed. Some general considerations relating to the calculation of the neutrino pulse and to the results of other authors are also discussed.

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