2010/01/31 by Basudeb Dasgupta, Georg G. Raffelt, Irene Tamborra
Chemistry · Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Chemistry #Flavor #Mixing (physics) #Neutrino #Neutrino Physics Research #Neutrino oscillation #Particle physics #Particle physics theoretical and experimental studies #Physics #Quantum mechanics #Radiative transfer #Supernova #astro-ph.SR #hep-ex #hep-ph
paper · pdf · doi:10.1103/physrevd.81.073004
published as Phys.Rev.D81:073004,2010 · 6 pages, including 3 figures (slightly modified to match the published version). Accepted for publication in PRD.
arxiv created 2010/04/15 · openalex publication_date 2010/04/15 · arxiv updated 2010/04/29 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Collective flavor transformations in supernovae, caused by neutrino-neutrino interactions, are essentially a two-flavor phenomenon driven by the atmospheric mass difference and the small mixing angle \ensuremathθ13. In the two-flavor approximation, the initial evolution depends logarithmically on \ensuremathθ13 and the system remains trapped in an unstable fixed point for \ensuremathθ13=0. However, any effect breaking exact \ensuremathν_\ensuremathμ\ensuremath-\ensuremathν_\ensuremathτ equivalence triggers the conversion. Such three-flavor perturbations include radiative corrections to weak interactions, small differences between the \ensuremathν_\ensuremathμ and \ensuremathν_\ensuremathτ fluxes, or nonstandard interactions. Therefore, extremely small values of \ensuremathθ13 are in practice equivalent, the fate of the system depending only on the neutrino spectra and their mass ordering.