Flavor-dependent neutrino angular distribution in core-collapse supernovae

TY - JOUR

T1 - Flavor-dependent neutrino angular distribution in core-collapse supernovae

AU - Tamborra, Irene

AU - Huedepohl, Lorenz

AU - Raffelt, Georg

AU - Janka, Hans-Thomas

N1 - 10 pages, including 8 figures. Minor changes in the text, matches version accepted for publication in ApJ. Data and animated visualization available at: http://wwwmpa.mpa-garching.mpg.de/ccsnarchive/data/Tamborra2017/

PY - 2017/4/20

Y1 - 2017/4/20

N2 - According to recent studies, the collective flavor evolution of neutrinos in core-collapse supernovae depends strongly on the flavor-dependent angular distribution of the local neutrino radiation field, notably on the angular intensity of the electron lepton number carried by neutrinos. To facilitate further investigations of this subject, we study the energy and angle distributions of the neutrino radiation field computed with the Vertex neutrino-transport code for several spherically symmetric (1D) supernova simulations (of progenitor masses 11.2, 15, and 25 M⊙) and explain how to extract this information from additional models of the Garching group. Beginning in the decoupling region ("neutrino sphere"), the distributions are more and more forward peaked in the radial direction with an angular spread that is largest for νe, smaller for , and smallest for νx, where x = μ or τ. While the energy-integrated νe minus angle distribution has a dip in the forward direction, it does not turn negative in any of our investigated cases.

AB - According to recent studies, the collective flavor evolution of neutrinos in core-collapse supernovae depends strongly on the flavor-dependent angular distribution of the local neutrino radiation field, notably on the angular intensity of the electron lepton number carried by neutrinos. To facilitate further investigations of this subject, we study the energy and angle distributions of the neutrino radiation field computed with the Vertex neutrino-transport code for several spherically symmetric (1D) supernova simulations (of progenitor masses 11.2, 15, and 25 M⊙) and explain how to extract this information from additional models of the Garching group. Beginning in the decoupling region ("neutrino sphere"), the distributions are more and more forward peaked in the radial direction with an angular spread that is largest for νe, smaller for , and smallest for νx, where x = μ or τ. While the energy-integrated νe minus angle distribution has a dip in the forward direction, it does not turn negative in any of our investigated cases.

KW - astro-ph.HE

KW - hep-ph

U2 - 10.3847/1538-4357/aa6a18

DO - 10.3847/1538-4357/aa6a18

M3 - Journal article

SN - 0004-637X

VL - 839

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 132

ER -