Neutrino-Nucleus Reactions

Abstract

This is a review of the current status of theoretical treatments of neutrino-nucleus reactions that are relevant to the detection of astrophysical neutrinos. Various nuclear physics aspects involved in the evaluation of the neutrino-nucleus reaction cross-sections are critically surveyed.

Dynamics of low-energy nuclear forces for electromagnetic and weak reactions with the deuteron in the Nambu-Jona-Lasinio model of light nuclei

“…Since our result is valid for much lower neutrino energies, we give the numerical values of the cross section only for the energies from the region 4 MeV ≤ E νe ≤ 10 MeV: The data in parentheses are taken from Table 1 of Ref. [46]. Thus, on the average the cross section σ νeD→e − pp (E νe ) calculated in the NNJL model by a factor of 1.6 is larger compared with the PMA ones.…”

“…Recently the calculation of the cross section for the reaction ν e + D → e − + p + p has been carried in Ref. [46] within the PMA and tabulated for the neutrino energies ranging over the region from threshold up to 170 MeV. Since our result is valid for much lower neutrino energies, we give the numerical values of the cross section only for the energies from the region 4 MeV ≤ E νe ≤ 10 MeV: The data in parentheses are taken from Table 1 of Ref.…”

The simplest resonant spin-flavour solution to the solar neutrino problem

“…[34] and the preliminary SNO collaboration estimates for the energy resolution, absolute energy scale and detection efficiencies. For definiteness we adopt the most optimistic threshold energy of 5 MeV which should be reached by the collaboration [35].…”

SNO: Predictions for ten measurable quantities

“…We calculate the quantities X that will be measured by SNO using the standard 8 B spectrum and the effective 3σ different spectra and determine from the following formula the associated uncertainty due to the shape of the 8 B spectrum. Thus [29], by Kubodera and Nozawa (KN) [28], and by Bahcall and Lisi (BL) [11]; the YHH and KN calculations use potential models and BL used an effective range treatment. For the neutral current cross sections, only the YHH and KN cross sections are available.…”

“…(18) result from (cf. Table III): (a) the difference between the Ying, Haxton, and Henley [29] and Kubodera-Nozawa cross sections [28] neutrino cross sections, (b) the shape of the 8 B neutrino energy spectrum [27], (c) the The most important question concerning the CC rate in SNO is the following: Is the reduced CC rate less than the reduced neutrino-electron scattering rate? If the reduced CC rate is measured to be less than the reduced ν-e scattering rate, then this will be evidence for neutral currents produced by ν µ or ν τ which appear as a result of neutrino oscillations.…”