Supernova Neutrinos and the Neutrino Masses
| dc.creator | Beacom, J. F. | |
| dc.date | 1999-01-13 | |
| dc.date.accessioned | 2026-07-07T04:06:13Z | |
| dc.date.available | 2026-07-07T04:06:13Z | |
| dc.description | Core-collapse supernovae emit of order $10^{58}$ 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 $ν_μ$ and $ν_τ$ 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 $\barν_e$ 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 $ν_μ$ or $ν_τ$ 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. | |
| dc.description | 8 pages including two figures. Invited talk at the 22nd Symposium on Nuclear Physics, Oaxtepec, Morelos, Mexico, 5-8 Jan. 1999 | |
| dc.identifier | https://arxiv.org/abs/hep-ph/9901300 | |
| dc.identifier | http://arxiv.org/abs/hep-ph/9901300 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/48685 | |
| dc.subject | High Energy Physics - Phenomenology | |
| dc.subject | Astrophysics | |
| dc.subject | High Energy Physics - Experiment | |
| dc.subject | Nuclear Experiment | |
| dc.subject | Nuclear Theory | |
| dc.title | Supernova Neutrinos and the Neutrino Masses | |
| dc.type | text |