The solution to the solar neutrino problem was

THE SOLUTION TO THE SOLAR NEUTRINO PROBLEM WAS FREE

10 -5 eV 2, corresponds to the first oscillation maximum, f eff ~ p (maximum of the survival probability). (ii) The second allowed region, D m 2 = (5 - 10). (i) The lowest ''island' allowed by KamLAND with D m 2 17%, is still consistent with data. L eff corresponds to the distance between KamLAND and the closest set of reactors which provides the large fraction of the antineutrino flux. The pattern can be described in terms of oscillations with certain effective distance, L eff, and effective oscillation phase f eff: The contours manifest an oscillatory pattern in D m 2 in spite of a strong averaging effect which originates from large spread in distances from different reactors. 1 the contours of constant confidence level with respect to the best fit point (7) in the ( D m 2 - tan 2 q) plane using relation: c 2 = + Dc 2, where Dc 2 = 1, 3.84 and 6.63 for 1 s, 95% and 99% C.L. Notice that in contrast with the KamLAND result our best fit mixing deviates from the maximal mixing. We find that for E p > 2.6 MeV the minimum of is achieved forДЄnd in this point c 2/ d.o.f. Where the ln term is absent in bins with no events (5 last bins). The KamLAND data are analyzed through a Poisson statistics, using the following c 2: Where N = ГҐ a N a, N a is given in (4) and N 0 is the total number of events in the absence of oscillations (following KamLAND we will call N and N 0 the rates).ДЎ). The suppression factor of the total number of (reactor neutrino) events above certain threshold is defined as: We sum over all reactors contributing appreciable to the flux at KamLAND. Is the vacuum oscillation survival probability for i reactor situated at the distance L ifrom KamLAND, F i is the flux from i reactor, s is the cross-section of В® e + n reaction, E p is the observed prompt energy, E p' is the true prompt energy, f( E p, E p') is the energy resolution function, A is the factor which takes into account the fiducial volume, the time of observation, etc. 13) the signal at KamLAND is determined by It consists of a very large volume scintilator detector, that can detect the anti-neutrinos from the inverse beta-decay reaction: The KamLAND (Kamioka Liquid scintillator Anti-Neutrino Detector) experiment detects anti-neutrinos created in ~ 26 nuclear reactors situated around the detector site, tipically at distances between 80 and 200 Km. This work is based in our recent paper where the KamLAND data were analysed, as well as the combination of this analysis with solar neutrinos data. As a result, the allowed ''island' in the D m 2 - sin 2 2 q plane with the best fit KamLAND point covers the best fit point from the solar neutrino analysis. The spectral data (although not yet precise) reproduce well the features described above. The first KamLAND results, both the total number of events and spectrum shape, are in a very good agreement with predictions: No distortion of the spectrum is expected for the other solutions. In the best fit point we predict for SNO: CC/NC = and = 3.0 В± 0.8% (68% C.L.), and (4 - 5) MeV. The best fit values of neutrino parameters are D m 2 = 7.1.10 -5 eV 2, tan 2 q = 0.40 and f B = 1.04 with the 1 s intervals: D m 2 = (6.4 - 8.4).

THE SOLUTION TO THE SOLAR NEUTRINO PROBLEM WAS FREE

We perform a combined analysis of the KamLAND (rate, spectrum) and the solar neutrino data with a free boron neutrino flux f B. The first KamLAND results are in a very good agreement with the predictions made on the basis of the solar neutrino data and the LMA realization of the MSW mechanism. IIThe Abdus Salam International Centre for Theoretical Physics, I-34100 Trieste, Italy, Institute for Nuclear Research of Russian Academy of Sciences, Moscow 117312, Russia IInstituto de FГ sica Gleb Wataghin - UNICAMP, 13083-970 Campinas SP, Brazil KamLAND data and the solution to the solar neutrino problem

The solution to the solar neutrino problem was