2003/06/06 by Keitaro Takahashi, Katsuhiko Sato, Adam Burrows +1
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Gamma-ray bursts and supernovae #Neutrino Physics Research #hep-ph
paper · pdf · doi:10.1103/physrevd.68.113009
published as Phys.Rev. D68 (2003) 113009 · 8 pages, 15 figures
arxiv created 2003/06/06 · openalex publication_date 2003/12/30 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We investigate the initial progenitor mass dependence of the early-phase neutrino signal from supernovae taking neutrino oscillations into account. The early-phase analysis has advantages in that it is not affected by the time evolution of the density structure of the star due to shock propagation or whether the remnant is a neutron star or a black hole. The initial mass affects the evolution of the massive star and its presupernova structure, which is important for two reasons when considering the neutrino signal. First, the density profile of the mantle affects the dynamics of neutrino oscillation in supernova. Second, the final iron core structure determines the features of the neutrino burst, i.e., the luminosity and the average energy. We find that both effects are rather small. This is desirable when we try to extract information on neutrino parameters from future supernova-neutrino observations. Although the uncertainty due to the progenitor mass is not small for intermediate \ensuremathθ13 (10^\ensuremath-5\ensuremath\lesssimsin22\ensuremathθ13\ensuremath\lesssim10^\ensuremath-3), we can, nevertheless, extract information on the character of the mass hierarchy and whether \ensuremathθ13 is very large or very small.