2003/06/30 by Enrico Nardi, Jorge I. Zuluaga · 16 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Cosmic neutrino background #Measurements of neutrino speed #Neutrino #Neutrino Physics Research #Neutrino astronomy #Neutrino detector #Neutrino oscillation #Nuclear physics #Particle physics #Particle physics theoretical and experimental studies #Physics #Range (aeronautics) #Solar neutrino #Solar neutrino problem #Supernova #astro-ph #hep-ph
paper · pdf · doi:10.1103/physrevd.69.103002
published in Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields 69(10) (American Physical Society) · Included analysis with numerical neutrino energy spectrum and oscillations effects. 7 pages, 6 figures
arxiv created 2004/01/30 · openalex publication_date 2004/05/12 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
A new method to study the effects of neutrino masses on a supernova neutrino signal is proposed. The method relies exclusively on the analysis of the full statistics of neutrino events, it is independent of astrophysical assumptions, and does not require the observation of any additional phenomenon to trace possible delays in the neutrino arrival times. The sensitivity of the method to the sub-eV neutrino mass range, defined as the capability of disentangling at 95% C.L. the case m_\ensuremathν=1eV from m_\ensuremathν=0, is tested by analyzing a set of synthetic neutrino samples modeled according to the signal that could be detected at SuperKamiokande. For a supernova at the Galactic center success is achieved in more than 50% of the cases. It is argued that a future Galactic supernova yielding several thousands of inverse \ensuremathβ decays might provide enough information to explore a neutrino mass range somewhat below 1 eV.