Nuclear response of water Cherenkov detectors to supernova and solar neutrinos

Details Nuclear response of water Cherenkov detectors to supernova and solar neutrinos Nuclear response of water Cherenkov detectors to supernova and solar neutrinos

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987phrvd..36.2283h&link_type=abstract

Physical Review D (Particles and Fields), Volume 36, Issue 8, 15 October 1987, pp.2283-2292

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123

Supernovae

Scientific paper

I present a careful examination of the nuclear cross sections of low-energy neutrinos and antineutrinos in water Cherenkov detectors, and consider the implications for neutrinos from SN1987A. For thermal sources with T>~4-5 MeV (depending on the detector threshold) the reaction O(νe,e-)F becomes the dominant mechanism for νe interactions, and at T>~7-9 MeV its rate exceeds that for (νe,e) elastic scattering by at least an order of magnitude. This has important implications for proposed mechanisms for prompt emission of energetic νe's following neutronization. The O(ν¯e,e+)N contribution remains a small correction to the dominant ν¯e+p-->e++n rate, accounting for less than 10% of the events even at T=10 MeV. Thus delayed β- emission by 16(τ1/2=7.1 sec) cannot distort event timing. Observable neutral-current nuclear excitations are absent in water, but can be strongly excited in carbon-bearing liquid-scintillation detectors. Arguments are given that a burst poor in electron neutrinos and antineutrinos, but otherwise similar to those derived from standard supernovae theory, might produce comparable signals in the Mt. Blanc, Kamioka, and Irvine-Michigan-Brookhaven detectors. For solar neutrinos generated by 8B β decay, reactions with trace quantities of 18O (two atoms per 104 electrons in natural water) account for approximately 10% of electron events. If it proves feasible to enhance the 18O content of a water Cherenkov detector, the hard spectrum of produced electrons would make an attractive charged-current signal.

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