We perform a global analysis in the framework of two active neutrino oscillations of all solar neutrino data, including the recent SNO day and night spectra (comprised of the charged current (CC), elastic scattering (ES) and neutral current (NC) events), the Super-Kamiokande (SK) day and night spectra (from 1496 days) and the updated SAGE results. We find that the Large Mixing Angle (LMA) solution is selected at the 99% C.L.; the best-fit parameters are ∆m 2 = 5.6×10 −5 eV 2 and θ = 32 • . No solutions with θ ≥ π/4 are allowed at the 5σ C.L. Oscillations to a pure sterile state are excluded at 5.3σ, but a sizeable sterile neutrino component could still be present in the solar flux.Typeset using REVT E X 1

We study how well KamLAND, the first terrestrial neutrino experiment capable of addressing the solar neutrino problem, will perform in ascertaining whether or not the large mixing angle MSW solution (with 10 −5 < ∼ ∆m 2 21 < ∼ 10 −4 eV 2 and oscillation amplitude sin 2 2 θ 12 > 0.3) is correct. We find that in a year of operation KamLAND will provide unequivocal evidence for or against this solution. Furthermore, its sensitivity to the three-neutrino oscillation parameters in this region is sufficiently acute as to determine ∆m 2 21 to approximately ±10% (for sin 2 2 θ 12 > 0.7) and to fix sin 2 2 θ 12 to within ±0.1 (at the 2σ level) with three years of accumulated data, independent of the value of θ 13 .

We analyze the 1258-day Super-Kamiokande day and night solar neutrino energy spectra with various χ 2 definitions. The best-fit lies in the LMA region at (∆m 2 , tan 2 θ) = (5.01 × 10 −5 eV 2 , 0.60), independently of whether systematic errors are included in the χ 2 -definition. We compare the exclusion and allowed regions from the different definitions and choose the most suitable definition to predict the regions from SNO at the end of three years of data accumulation. We first work under the assumption that Super-Kamiokande sees a flux-suppressed flat energy spectrum. Then, we consider the possibility of each one of the three MSW regions being the solution to the solar neutrino problem. We find that the exclusion and allowed regions for the flat spectrum hypothesis and the LMA and LOW solutions are alike. In three years, we expect SNO to find very similar regions to that obtained by Super-Kamiokande. We evaluate whether the zenith angle distribution at SNO with optimum binning will add anything to the analysis of the day and night spectra; for comparison, we show the results of our analysis of the 1258-day zenith angle distribution from Super-Kamiokande, for which the best-fit parameters are (∆m 2 , tan 2 θ) = (5.01 × 10 −5 eV 2 , 0.56).

We show that the temperatures of the emergent non-electron neutrinos and the binding energy released by a galactic Type II supernova are determinable, assuming the Large Mixing Angle (LMA) solution is correct, from observations at the Sudbury Neutrino Observatory (SNO) and at Super-Kamiokande (SK). If the neutrino mass hierarchy is inverted, either a lower or upper bound can be placed on the neutrino mixing angle θ13, and the hierarchy can be deduced for adiabatic transitions. For the normal hierarchy, neither can θ13 be constrained nor can the hierarchy be determined. Our conclusions are qualitatively unchanged for the proposed Hyper-Kamiokande detector.

We perform a detailed analysis of the capabilities of the MINOS, ICARUS and OPERA experiments to measure neutrino oscillation parameters at the atmospheric scale with their data taken separately and in combination. MI-NOS will determine ∆m 2 32 and sin 2 2θ 23 to within 10% at the 99% C.L. with 10 kton-years of data. While no one experiment will determine sin 2 2θ 13 with much precision, if its value lies in the combined sensitivity region of the three experiments, it will be possible to place a lower bound of O(0.01) at the 95% C.L. on this parameter by combining the data from the three experiments. The same bound can be placed with a combination of MINOS and ICARUS data alone.