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Title: Simple picture for neutrino flavor transformation in supernovae

Abstract

We can understand many recently discovered features of flavor evolution in dense, self-coupled supernova neutrino and antineutrino systems with a simple, physical scheme consisting of two quasistatic solutions. One solution closely resembles the conventional, adiabatic single-neutrino Mikheyev-Smirnov-Wolfenstein (MSW) mechanism, in that neutrinos and antineutrinos remain in mass eigenstates as they evolve in flavor space. The other solution is analogous to the regular precession of a gyroscopic pendulum in flavor space, and has been discussed extensively in recent works. Results of recent numerical studies are best explained with combinations of these solutions in the following general scenario: (1) Near the neutrino sphere, the MSW-like many-body solution obtains. (2) Depending on neutrino vacuum mixing parameters, luminosities, energy spectra, and the matter density profile, collective flavor transformation in the nutation mode develops and drives neutrinos away from the MSW-like evolution and toward regular precession. (3) Neutrino and antineutrino flavors roughly evolve according to the regular precession solution until neutrino densities are low. In the late stage of the precession solution, a stepwise swapping develops in the energy spectra of {nu}{sub e} and {nu}{sub {mu}}/{nu}{sub {tau}}. We also discuss some subtle points regarding adiabaticity in flavor transformation in dense-neutrino systems.

Authors:
; ;  [1]
  1. Department of Physics, University of California, San Diego, La Jolla, California 92093-0319 (United States)
Publication Date:
OSTI Identifier:
21032499
Resource Type:
Journal Article
Journal Name:
Physical Review. D, Particles Fields
Additional Journal Information:
Journal Volume: 76; Journal Issue: 8; Other Information: DOI: 10.1103/PhysRevD.76.085013; (c) 2007 The American Physical Society; Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0556-2821
Country of Publication:
United States
Language:
English
Subject:
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; ANTINEUTRINOS; EIGENSTATES; ELECTRON NEUTRINOS; ENERGY SPECTRA; FLAVOR MODEL; MANY-BODY PROBLEM; MATHEMATICAL SOLUTIONS; MUON NEUTRINOS; NUMERICAL ANALYSIS; REST MASS; SPACE; SUPERNOVAE; TAU NEUTRINOS; TRANSFORMATIONS

Citation Formats

Huaiyu, Duan, Fuller, George M, Yongzhong, Qian, and School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455. Simple picture for neutrino flavor transformation in supernovae. United States: N. p., 2007. Web. doi:10.1103/PHYSREVD.76.085013.
Huaiyu, Duan, Fuller, George M, Yongzhong, Qian, & School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455. Simple picture for neutrino flavor transformation in supernovae. United States. doi:10.1103/PHYSREVD.76.085013.
Huaiyu, Duan, Fuller, George M, Yongzhong, Qian, and School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455. Mon . "Simple picture for neutrino flavor transformation in supernovae". United States. doi:10.1103/PHYSREVD.76.085013.
@article{osti_21032499,
title = {Simple picture for neutrino flavor transformation in supernovae},
author = {Huaiyu, Duan and Fuller, George M and Yongzhong, Qian and School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455},
abstractNote = {We can understand many recently discovered features of flavor evolution in dense, self-coupled supernova neutrino and antineutrino systems with a simple, physical scheme consisting of two quasistatic solutions. One solution closely resembles the conventional, adiabatic single-neutrino Mikheyev-Smirnov-Wolfenstein (MSW) mechanism, in that neutrinos and antineutrinos remain in mass eigenstates as they evolve in flavor space. The other solution is analogous to the regular precession of a gyroscopic pendulum in flavor space, and has been discussed extensively in recent works. Results of recent numerical studies are best explained with combinations of these solutions in the following general scenario: (1) Near the neutrino sphere, the MSW-like many-body solution obtains. (2) Depending on neutrino vacuum mixing parameters, luminosities, energy spectra, and the matter density profile, collective flavor transformation in the nutation mode develops and drives neutrinos away from the MSW-like evolution and toward regular precession. (3) Neutrino and antineutrino flavors roughly evolve according to the regular precession solution until neutrino densities are low. In the late stage of the precession solution, a stepwise swapping develops in the energy spectra of {nu}{sub e} and {nu}{sub {mu}}/{nu}{sub {tau}}. We also discuss some subtle points regarding adiabaticity in flavor transformation in dense-neutrino systems.},
doi = {10.1103/PHYSREVD.76.085013},
journal = {Physical Review. D, Particles Fields},
issn = {0556-2821},
number = 8,
volume = 76,
place = {United States},
year = {2007},
month = {10}
}