2016/10/31 by Ignacio Izaguirre, Georg G. Raffelt, Georg Raffelt +1 · 1 citation
Mathematics · Physics and Astronomy · #Astrophysics #Astrophysics and Cosmic Phenomena #Computer science #Data mining #Dispersion (optics) #Dispersion relation #Mathematics #Neutrino #Neutrino Physics Research #Nuclear physics #Optics #Pairwise comparison #Particle physics theoretical and experimental studies #Physics #Relation (database) #Statistics #Supernova #astro-ph.SR #hep-ph
paper · pdf · doi:10.1103/physrevlett.118.021101
published as Phys. Rev. Lett. 118, 021101 (2017) · 6 pages, 3 figures. Minor changes in the text, references added and discussion of figure 3 extended. Matches published PRL version
openalex publication_date 2017/01/10 · arxiv created 2017/01/11 · arxiv updated 2017/01/12 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Collective pair conversion \ensuremathνe\ensuremathνe\ensuremath↔\ensuremathνx\ensuremathνx by forward scattering, where x=\ensuremathμ or \ensuremathτ, may be generic for supernova neutrino transport. Depending on the local angular intensity of the electron lepton number carried by neutrinos, the conversion rate can be ``fast,'' i.e., of the order of √(2)GF(n_\ensuremathνe\ensuremath-n_\ensuremathνe)\ensuremath≫\mathrm\ensuremathΔmatm2/2E. We present a novel approach to understand these phenomena: a dispersion relation for the frequency and wave number (\mathrm\ensuremathΩ,K) of disturbances in the mean field of \ensuremathνe\ensuremathνx flavor coherence. Runaway solutions occur in ``dispersion gaps,'' i.e., in ``forbidden'' intervals of \mathrm\ensuremathΩ and/or K where propagating plane waves do not exist. We stress that the actual solutions also depend on the initial and/or boundary conditions, which need to be further investigated.