Stability analysis of collective neutrino oscillations in the supernova accretion phase with realistic energy and angle distributions

Details Stability analysis of collective neutrino oscillations in the supernova accretion phase with realistic energy and angle distributions Stability analysis of collective neutrino oscillations in the supernova accretion phase with realistic energy and angle distributions

2012-03-07

arxiv.org/abs/1203.1484v1

Physics

High Energy Physics

High Energy Physics - Phenomenology

(8 pages, 3 eps figures)

Scientific paper

We revisit our previous results on the matter suppression of self-induced neutrino flavor conversions during a supernova (SN) accretion phase, performing a linearized stability analysis of the neutrino equations of motion, in the presence of realistic SN density profiles. In our previous numerical study, we used a simplified model based on an isotropic neutrino emission with a single typical energy. Here, we take into account realistic neutrino energy and angle distributions. We find that multi-energy effects have a sub-leading impact in the flavor stability of the SN neutrino fluxes with respect to our previous single-energy results. Conversely, realistic forward-peaked neutrino angular distributions would enhance the matter suppression of the self-induced oscillations with respect to an isotropic neutrino emission. As a result, in our models for iron-core SNe, collective flavor conversions have a negligible impact on the characterization of the observable neutrino signal during the accretion phase. Instead, for a low-mass O-Ne-Mg core SN model, with lower matter density profile and less forward-peaked angular distributions, collective conversions are possible also at early times.

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