Supernova Neutrinos and Their Influence on Nucleosynthesis:. Light Elements and R-Process Elements

Details Supernova Neutrinos and Their Influence on Nucleosynthesis:. Light Elements and R-Process Elements Supernova Neutrinos and Their Influence on Nucleosynthesis:. Light Elements and R-Process Elements

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005omeg.conf..456y&link_type=abstract

ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2003. Held 17-19 November 2003 in RIKEN, Wako, Saitama, Japan. Edited by M Terasawa,

Astronomy and Astrophysics

Astronomy

Scientific paper

The influence of the neutrino luminosity on the nucleosynthesis of the light elements 7Li and 11B and the r-process heavy elements in Type II Supernovae is investigated. Common models of the neutrino luminosity, which are parameterized by the total energy Eν and decay time τν, are adopted to understand both processes. The supernova explosion of a 16.2 M&sun; star, which corresponds to SN 1987A, is calculated and the light element synthesis is pursued by postprocessing. The ejected masses of 7Li and 11B are roughly proportional to Eν but are insensitive to τν. As for the r-process, the same models of neutrino luminosity are adopted in the neutrino-driven wind models of a 1.4 &sun; neutron star. The r-process is affected through the peak neutrino luminosity, which relates to Eν/τν. An unsolved problem of the overproduction of 11B in the galactic chemical evolution is discussed. The total neutrino energy should be smaller than 1.2 × 1053 ergs to avoid the overproduction of 11B, which is too small to accept compared to 3.0 × 1053 ergs deduced from the observation of SN 1987A. We here propose to reduce the temperature of νμ,τ and bar ν {μ ,τ } to 6.0 MeV/k in a model with Eν 3 × 1053 ergs and τν = 9.0 s. This modification is shown to resolve the overproduction problem of 11B while still preserving a successful r-process abundance pattern.

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