1999/01/13 by J. F. Beacom, Beacom, J. F.
Physics and Astronomy · #Astrophysics (astro-ph) #Astrophysics and Cosmic Phenomena #FOS: Physical sciences #High Energy Physics - Experiment (hep-ex) #High Energy Physics - Phenomenology (hep-ph) #Neutrino Physics Research #Nuclear Experiment (nucl-ex) #Nuclear Theory (nucl-th) #Particle physics theoretical and experimental studies #astro-ph #hep-ex #hep-ph #nucl-ex #nucl-th
paper · pdf · doi:10.48550/arxiv.hep-ph/9901300
8 pages including two figures. Invited talk at the 22nd Symposium on Nuclear Physics, Oaxtepec, Morelos, Mexico, 5-8 Jan. 1999
arxiv created 1999/01/13 · openalex publication_date 1999/01/13 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Core-collapse supernovae emit of order 1058 neutrinos and antineutrinos of all flavors over several seconds, with average energies of 10--25 MeV. In the Sudbury Neutrino Observatory (SNO), a future Galactic supernova at a distance of 10 kpc would cause several hundred events. The νμ and ντ neutrinos and antineutrinos are of particular interest, as a test of the supernova mechanism. In addition, it is possible to measure or limit their masses by their delay (determined from neutral-current events) relative to the νe neutrinos (determined from charged-current events). Numerical results are presented for such a future supernova as seen in SNO. Under reasonable assumptions, and in the presence of the expected counting statistics, a νμ or ντ mass down to about 30 eV can be simply and robustly determined. This seems to be the best technique for direct measurement of these masses.