Neutrinos and the Supernova Origin of the Elements
arXiv:astro-ph/0008494 · doi:10.1016/S0920-5632(00)00961-0
Abstract
Intense fluxes of neutrinos are emitted by the hot neutron star produced in a supernova. The electron neutrino and antineutrino capture reactions on neutrons and protons, respectively, provide heating to drive a wind from the hot neutron star. The same reactions also determine the neutron-richness of the wind material. Nucleosynthesis via rapid neutron capture, the r-process, may occur in the wind material as it expands away from the neutron star. The neutron-richness of the wind material, and hence, the r-process nucleosynthesis therein, are sensitive to mixing between the muon (or tauon) neutrino/antineutrino and the electron (or sterile) neutrino/antineutrino. Indirect arguments and direct tests for the supernova origin of the r-process elements are discussed with a goal to establish supernova r-process nucleosynthesis as an important probe for neutrino mixing.
6 pages including 2 figures, to appear in the Proceedings of Neutrino 2000
References in corpus (5)
- Supernovae versus Neutron Star Mergers as the Major r-Process Sources
- Sterile neutrinos and supernova nucleosynthesis
- Prompt Iron Enrichment, Two r-Process Components, and Abundances in Very Metal-Poor Stars
- Stellar Abundances in the Early Galaxy and Two r-Process Components
- Probing r-Process Production of Nuclei Beyond Bi209 with Gamma Rays