Supernova neutrino detection in Borexino

Abstract

We calculated the expected neutrino signal in Borexino from a typical Type II supernova at a distance of 10 kpc. A burst of around 110 events would appear in Borexino within a time interval of about 10 s. Most of these events would come from the reaction channelν e + p → e + + n, while about 30 events would be induced by the interaction of the supernova neutrino flux on 12 C in the liquid scintillator. Borexino can clearly distinguish between the neutral-current excitations 12 C(ν, ν ′ ) 12 C * (15.11 MeV) and the charged-current reactions 12 C(ν e , e − ) 12 N and 12 C(ν e , e + ) 12 B, via their distinctive event signatures. The ratio of the chargedcurrent to neutral-current neutrino event rates and their time profiles with respect to each other can provide a handle on supernova and non-standard neutrino physics (mass and flavor oscillations).

New results from RENO & prospects with RENO-50

“…The background in the RENO-50 detector in a 10 second period is low enough for an observation of the neutrino signals from supernova burst. The RENO-50 detector would observe ~6000 events from a supernova at 8 kpc [14,15].…”

Science and technology of Borexino: a real-time detector for low energy solar neutrinos

“…Two factors make its detection in Borexino interesting. 74 As the first major detector with liquid scintillator operating at low energies, Borexino may be unique despite the relatively low detector mass because: (i) low energies in the Fermi-Dirac spectrum of the supernova ν's can be probed; (ii) e can be detected with high sensitivity and (iii) Supernova neutrino interactions with 12 C in the liquid scintillator offer a unique tool for a CC/NC analysis of the ν flux by combining the results from the reactions 12 C( e ,e -) 12 N, 12 C( e ,e + ) 12 The signals are estimated to be ≈80 e -events and ≈30 events from reactions on 12 C for a 3×10 53 erg burst at a distance of 10kpc. The principal results of interest to the supernova mechanism as well as to ν physics are:…”

Determining neutrino and supernova parameters with a galactic supernova

“…If another oil will be used the carbon to proton ratio may change and thus the results will change slightly. A discussion on SN neutrinos and scintillator detectors can be found in [49,50], although without an explicit calculation of the accuracy of the determination of the parameters.…”