A road map to solar neutrino fluxes, neutrino oscillation parameters, and tests for new physics

We analyze all available solar and related reactor neutrino experiments, as well as simulated future 7Be, p− p, and pep solar neutrino experiments. We treat all solar neutrino fluxes as free parameters subject to the condition that the total luminosity represented by the neutrinos equals the observed solar luminosity (the ‘luminosity constraint’). Existing experiments plus the luminosity constraint show that the p−p solar neutrino flux is 1.02 ± 0.02 (1σ) times the flux predicted by the BP00 standard solar model; the 7Be neutrino flux is 0.93 −0.63 the predicted flux; and the 8B flux is 1.01 ± 0.04 the predicted flux. The CNO fluxes are very poorly determined. The neutrino oscillation parameters are: ∆m2 = 7.3 −0.6 × 10−5 eV2 and tan2 θ12 = 0.41 ± 0.04. We evaluate how accurate future experiments must be to determine more precisely neutrino oscillation parameters and solar neutrino fluxes, and to elucidate the transition from vacuum-dominated to matterdominated oscillations at low energies. A future 7Be ν − e scattering experiment accurate to ±10% can reduce the uncertainty in the experimentally determined 7Be neutrino flux by a factor of four and the uncertainty in the p − p neutrino flux by a factor of 2.5 (to ±0.8%). A future p − p experiment must be accurate to better than ±3% to shrink the uncertainty in tan2 θ12 by more than 15%. The idea that the Sun shines because of nuclear fusion reactions can be tested accurately by comparing the observed photon luminosity of the Sun with the luminosity inferred from measurements of solar neutrino fluxes. Based upon quantitative analyses of present and simulated future experiments, we answer the question: Why perform low-energy solar neutrino experiments?