Supernovae and Neutrinos

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dc.creatorBeacom, John F.
dc.date2002-09-08
dc.date.accessioned2026-07-07T11:28:58Z
dc.date.available2026-07-07T11:28:58Z
dc.descriptionA long-standing problem in supernova physics is how to measure the total energy and temperature of $ν_μ$, $ν_τ$, $\barν_μ$, and $\barν_τ$. While of the highest importance, this is very difficult because these flavors only have neutral-current detector interactions. We propose that neutrino-proton elastic scattering, $ν+ p \to ν+ p$, can be used for the detection of supernova neutrinos in scintillator detectors. It should be emphasized immediately that the dominant signal is on {\it free} protons. Though the proton recoil kinetic energy spectrum is soft, with $T_p \simeq 2 E_ν^2/M_p$, and the scintillation light output from slow, heavily ionizing protons is quenched, the yield above a realistic threshold is nearly as large as that from $\barν_e + p \to e^+ + n$. In addition, the measured proton spectrum is related to the incident neutrino spectrum. The ability to detect this signal would give detectors like KamLAND and Borexino a crucial and unique role in the quest to detect supernova neutrinos. These results are now published: J. F. Beacom, W. M. Farr and P. Vogel, Phys. Rev. D {\bf 66}, 033001 (2002) [arXiv:hep-ph/0205220]; the details are given there.
dc.descriptionInvited talk at the XXth International Conference on Neutrino Physics and Astrophysics (Neutrino 2002), Munich, Germany, May 25-30, 2002
dc.identifierhttps://arxiv.org/abs/astro-ph/0209136
dc.identifierhttp://arxiv.org/abs/astro-ph/0209136
dc.identifierNucl.Phys.Proc.Suppl.118:307-314,2003
dc.identifierdoi:10.1016/S0920-5632(03)01323-9
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/196569
dc.subjectAstrophysics
dc.subjectHigh Energy Physics - Phenomenology
dc.subjectNuclear Theory
dc.titleSupernovae and Neutrinos
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