2014/06/30 by Irene Tamborra, Georg G. Raffelt, Georg Raffelt +5 · 1 citation
Physics and Astronomy · #Accretion (finance) #Astrophysics #Astrophysics and Cosmic Phenomena #Asymmetry #Instability #Lepton #Mechanics #Neutrino #Neutrino Physics Research #Neutrino detector #Neutrino oscillation #Nuclear physics #Particle physics #Particle physics theoretical and experimental studies #Physics #Supernova #astro-ph.SR #hep-ex #hep-ph
paper · pdf · doi:10.1103/physrevd.90.045032
published as Phys. Rev. D 90, 045032 (2014) · 18 pages, including 18 figures. One section and new figures added; conclusions unchanged. Matches published version in PRD
openalex publication_date 2014/08/25 · arxiv created 2014/08/26 · arxiv updated 2014/09/05 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The neutrino emission characteristics of the first full-scale three-dimensional supernova simulations with sophisticated three-flavor neutrino transport for three models with masses 11.2, 20, and 27M_\ensuremath\bigodot are evaluated in detail. All the studied progenitors show the expected hydrodynamical instabilities in the form of large-scale convective overturn. In addition, the recently identified lepton-number emission self-sustained asymmetry (LESA) phenomenon is generic for all our cases. Standing accretion-shock instability (SASI) activity appears in the 20 and 27M_\ensuremath\bigodot cases, partly in the form of a spiral mode, inducing large but direction- and flavor-dependent modulations of neutrino emission. These modulations can be clearly identified in the existing IceCube and future Hyper-Kamiokande detectors, depending on the distance and detector location relative to the main standing accretion-shock instability sloshing direction.