[en] In the past decade non-accelerator experiments have discovered neutrino oscillations and made precise measurements of neutrino mixing parameters. I will review the phenomenon of neutrino oscillation and describe what non-accelerator experiments have revealed about neutrino masses and mixings. (author)

[en] The Sudbury Neutrino Observatory is a 1000 T D₂O Cerenkov detector that is sensitive to ⁸B solar neutrinos. The energy, radius, and direction with respect to the sun is measured for each neutrino event; these distributions are used to separately determine the rates of the charged current, neutral current and electron scattering reactions of neutrinos on deuterium. Assuming an undistorted ⁸B spectrum, the ν_e component of the ⁸B solar flux is phi_e = 1.76^+0.05_-0.05(stat.)^+0.09_-0.09 (syst.) x 10⁶ cm^-2s^-1 based on events with a measured kinetic energy above 5 MeV. The non-ν_e component is phi_μτ 3.41^+0.45_-0.45(stat.)^+0.48_-0.45 (syst.) x 10⁶ cm^-2s^-1, 5.3σ greater than zero, providing strong evidence for solar ν_e flavor transformation. The total flux measured with the NC reaction is phi_NC = 5.09^+0.044_-0.43(stat.)^+0.46_-0.43 (sy st.) x 10⁶ cm^-2s^-1, consistent with solar models. The night minus day rate is 14.0% ± 6.3%^+1.5_-1.4% of the average rate. If the total flux of active neutrinos is additionally constrained to have no asymmetry, the ν_e asymmetry is found to be 7.0% ± 4.9%^+1.3_-1.2%. A global solar neutrino analysis is terms of matter-enhanced oscillations of two active flavors strongly favors the Large Mixing Angle (LMA) solution

[en] A search has been made for neutrinos from the hep reaction in the Sun and from the diffuse supernova neutrino background (DSNB)using data collected during the first operational phase of the Sudbury Neutrino Observatory, with an exposure of 0.65 kilotons-years. For the hep neutrino search, two events are observed in the effective electron energy range of 14.3 MeV< T_eff<20 MeV where 3.1 background events are expected. After accounting for neutrino oscillations, an upper limit of 2.3 x 104 cm-2s-1 at the 90 percent confidence level is inferred on the integral total flux of hep neutrinos. For DSNB neutrinos, no events are observed in the effective electron energy range of 21 MeV< T_eff<35 MeV and, consequently, an upper limit on the nu e component of the DSNB flux in the neutrino energy range of 22.9 MeV< E nu<36.9 MeV of 70 cm-2-1 is inferred at the 90 percent confidence level. This is an improvement by a factor of 6.5 on the previous best upper limit on the hep neutrino flux and by two orders of magnitude on the previous upper limit on the nu e component of the DSNB flux

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[en] The Sudbury Neutrino Observatory (SNO) has precisely determined the total active (v_x)⁸B solar neutrino flux without assumptions about the energy dependence of the v_e survival probability. The measurements were made with dissolved NaCl in the heavy water to enhance the sensitivity and signature for neutral-current interactions. The flux is found to be 5.21+-0.27 (stat)+-0.38(syst)x10^-6 cm^-2s^-1, in agreement with previous measurements and standard solar models. A global analysis of these and other solar and reactor neutrino results yields Δm² = 7.1^+1.2_-0.6 x 10^-5 eV² and θ 32.5^+2.4_-2.3 degrees. Maximal mixing is rejected at the equivalent of 5.4 standard deviations

[en] The Sudbury Neutrino Observatory (SNO) is a water imaging Cherenkov detector. Its usage of 1000 metric tons of D₂O as target allows the SNO detector to make a solar-model independent test of the neutrino oscillation hypothesis by simultaneously measuring the solar ν_e flux and the total flux of all active neutrino species. Solar neutrinos from the decay of ⁸B have been detected at SNO by the charged-current (CC) interaction on the deuteron and by the elastic scattering (ES) of electrons. While the CC reaction is sensitive exclusively to ν_e, the ES reaction also has a small sensitivity to ν_μ and ν_τ. In this paper, recent solar neutrino results from the SNO experiment are presented. It is demonstrated that the solar flux from ⁸B decay as measured from the ES reaction rate under the no-oscillation assumption is consistent with the high precision ES measurement by the Super-Kamiokande experiment. The ν_e flux deduced from the CC reaction rate in SNO differs from the Super-Kamiokande ES results by 3.3σ. This is evidence for an active neutrino component, in additional to ν_e, in the solar neutrino flux. These results also allow the first experimental determination of the total active ⁸B neutrino flux from the Sun, and is found to be in good agreement with solar model predictions