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Title: Flavor-mixing effects of cosmologically significant neutrinos on supernova dynamics and nucleosynthesis

Abstract

Massive neutrinos are interesting in cosmology, astrophysics, and particle physics. The current experimental upper limits on neutrino masses are very loose (m[sub [nu]e] < 7.2 eV, m[sub [nu][mu]] < 250 keV, and M[sub [nu][tau]] < 31 MeV). The existence of cosmologically significant neutrinos (m[sub [nu]] = 1-100 eV) has to be tested by other means. Once neutrinos have mass, mixing between different neutrino flavors occurs. In particular, this mixing can be greatly enhanced by the Mikheyev-Smirnov-Wolfenstein (MSW) mechanism when neutrinos are propagating through matter with appropriate densities. The MSW mechanism can be operating for cosmologically significant neutrinos in core-collapse driven supernovae, where the central part of a massive star evolves into a protoneutron star, releasing about 10[sup 53] erg in all three flavors of neutrinos and anti-neutrinos. Because of their different interactions with matter, [nu][sub [mu]], [nu][sub [tau]] and their anti-neutrinos decouple deeper in the core and therefore have higher average energies than [nu][sub e] and [bar [nu]][sub e]. For the late time supernova mechanism, which depends on the energy deposit by [nu][sub e] and [bar [nu]][sub e] absorption of free nucleons above the proto-neutron star to revive the stalled shock, mixing between a cosmologically significant [nu][sub [mu]] or [nu][submore » [tau]] and [nu][sub e] will increase the energy deposit rate, and may help bridge the gap between the simulated and the observed explosion energy. After the stalled shock gets outgoing again, a high-entropy, evacuated region above the proto-neutron star is created by the previous and still on-going neutrino heating. Later, the expansion of this region develops into a neutrino-driven wind. And this wind is a promising site for the r-process nucleosynthesis of heavy elements.« less

Authors:
Publication Date:
Research Org.:
California Univ., San Diego, La Jolla, CA (United States)
OSTI Identifier:
7006022
Resource Type:
Miscellaneous
Resource Relation:
Other Information: Thesis (Ph.D.)
Country of Publication:
United States
Language:
English
Subject:
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; NEUTRINOS; MASS; SUPERNOVAE; NUCLEOSYNTHESIS; R PROCESS; ELECTRON NEUTRINOS; MUON NEUTRINOS; NEUTRINO-NEUTRINO INTERACTIONS; QUANTUM FLAVORDYNAMICS; TAU NEUTRINOS; ELEMENTARY PARTICLES; ERUPTIVE VARIABLE STARS; FERMIONS; FIELD THEORIES; HEAVY LEPTONS; INTERACTIONS; LEPTON-LEPTON INTERACTIONS; LEPTONS; MASSLESS PARTICLES; PARTICLE INTERACTIONS; POSTULATED PARTICLES; QUANTUM FIELD THEORY; STAR EVOLUTION; STARS; SYNTHESIS; VARIABLE STARS; 662430* - Properties of Leptons- (1992-)

Citation Formats

Qian, Yongzhong. Flavor-mixing effects of cosmologically significant neutrinos on supernova dynamics and nucleosynthesis. United States: N. p., 1993. Web.
Qian, Yongzhong. Flavor-mixing effects of cosmologically significant neutrinos on supernova dynamics and nucleosynthesis. United States.
Qian, Yongzhong. Fri . "Flavor-mixing effects of cosmologically significant neutrinos on supernova dynamics and nucleosynthesis". United States.
@article{osti_7006022,
title = {Flavor-mixing effects of cosmologically significant neutrinos on supernova dynamics and nucleosynthesis},
author = {Qian, Yongzhong},
abstractNote = {Massive neutrinos are interesting in cosmology, astrophysics, and particle physics. The current experimental upper limits on neutrino masses are very loose (m[sub [nu]e] < 7.2 eV, m[sub [nu][mu]] < 250 keV, and M[sub [nu][tau]] < 31 MeV). The existence of cosmologically significant neutrinos (m[sub [nu]] = 1-100 eV) has to be tested by other means. Once neutrinos have mass, mixing between different neutrino flavors occurs. In particular, this mixing can be greatly enhanced by the Mikheyev-Smirnov-Wolfenstein (MSW) mechanism when neutrinos are propagating through matter with appropriate densities. The MSW mechanism can be operating for cosmologically significant neutrinos in core-collapse driven supernovae, where the central part of a massive star evolves into a protoneutron star, releasing about 10[sup 53] erg in all three flavors of neutrinos and anti-neutrinos. Because of their different interactions with matter, [nu][sub [mu]], [nu][sub [tau]] and their anti-neutrinos decouple deeper in the core and therefore have higher average energies than [nu][sub e] and [bar [nu]][sub e]. For the late time supernova mechanism, which depends on the energy deposit by [nu][sub e] and [bar [nu]][sub e] absorption of free nucleons above the proto-neutron star to revive the stalled shock, mixing between a cosmologically significant [nu][sub [mu]] or [nu][sub [tau]] and [nu][sub e] will increase the energy deposit rate, and may help bridge the gap between the simulated and the observed explosion energy. After the stalled shock gets outgoing again, a high-entropy, evacuated region above the proto-neutron star is created by the previous and still on-going neutrino heating. Later, the expansion of this region develops into a neutrino-driven wind. And this wind is a promising site for the r-process nucleosynthesis of heavy elements.},
doi = {},
journal = {},
number = ,
volume = ,
place = {United States},
year = {1993},
month = {1}
}

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