Supernova Neutrino Process and its Impact on the Galactic Chemical Evolution of the Light Elements

Abstract

In order to resolve the overproduction problem of 11B in supernova explosions during Galactic chemical evolution, the dependence of the ejected masses of the light elements produced through the nu-process in supernova explosions on supernova neutrino parameters is investigated and constraints on the supernova neutrinos are evaluated. Detailed nucleosynthesis in a supernova explosion model corresponding to SN 1987A is calculated by postprocessing. The ejected masses of 11B and 7Li depend strongly on the temperature of mu- and tau-neutrinos and their antiparticles and are roughly proportional to the total neutrino energy. The range of temperature of mu- and -tau neutrinos and their antiparticles appropriate for the amount of 11B necessary for Galactic chemical evolution and the total neutrino energy deduced from the gravitational energy of a typical neutron star is between 4.8 MeV and 6.6 MeV. In the case of neutrino energy spectra with non-zero chemical potential, this range decreases by about 10%.

arXiv comment4 pages, 2 figures, contribution to Nuclei in the Cosmos VIII, to appear in Nucl. Phys. A

References in corpus (5)

• Neutron Star Structure and the Equation of State
• Monte Carlo Study of Supernova Neutrino Spectra Formation
• Nucleosynthesis of Light Elements and Heavy r-Process Elements through the nu-Process in Supernova Explosion
• Testing Spallation Processes With Beryllium and Boron
• Galactic Cosmic Rays from Superbubbles and the Abundances of Lithium, Beryllium, and Boron

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• (Non)-supersymmetric Marginal Deformations from Twistor String Theory