E-viri
-
Hallin, A.L.; Beier, E.W.; Biller, S.D.; Boulay, M.G.; Bowler, M.G.; Bowles, T.J.; Brice, S.J.; Bullard, T.V.; Cameron, J.; Chan, Y.D.; Chen, X.; Chen, M.; Cleveland, B.T.; Cox, G.A.; Dai, X.; Dalnoki-Veress, F.; Doe, P.J.; Doucas, G.; Duba, C.A.; Duncan, F.A.; Dunmore, J.A.; Elliott, S.R.; Evans, H.C.; Ewan, G.T.; Farine, J.; Fergani, H.; Formaggio, J.A.; Fowler, M.M.; Frame, K.; Frati, W.; Gagnon, N.; Graham, K.; Grant, D.R.; Hahn, R.L.; Hallman, E.D.; Hamer, A.S.; Handler, W.B.; Hargrove, C.K.; Harvey, P.J.; Hazama, R.; Heeger, K.M.; Heintzelman, W.J.; Heise, J.; Helmer, R.L.; Hime, A.; Howe, M.; Jelley, N.A.; Kazkaz, K.; Keener, P.T.; Klein, J.R.; Kutter, T.; Kyba, C.C.M.; Law, J.; Lawson, I.T.; Leslie, J.R.; Levine, I.; Luoma, S.; Majerus, S.; Mak, H.B.; Maneira, J.; Manor, J.; McCauley, N.; McDonald, A.B.; McGregor, G.; Miller, G.G.; Nally, C.W.; Noble, A.J.; Norman, E.B.; Okada, C.E.; Orrell, J.L.; Oser, S.M.; Poon, A.W.P.; Robertson, B.C.; Robertson, R.G.H.; Rosendahl, S.S.E.; Rusu, V.L.; Schaffer, K.K.; Schwendener, M.H.; Simpson, J.J.; Sims, C.J.; Sinclair, D.; Skensved, P.; Smith, M.W.E.; Spreitzer, T.; Starinsky, N.; Stonehill, L.C.; Tafirout, R.; Tagg, N.; Van Berg, R.; Van de Water, R.G.; Virtue, C.J.; Waltham, C.E.; Wark, D.L.; West, N.; Wilhelmy, J.B.; Wilkerson, J.F.; Wilson, J.R.; Wittich, P.; Wouters, J.M.; Yeh, M.
Nuclear physics. Section B, Proceedings supplement, 2003, Letnik: 118Journal Article
The Sudbury Neutrino Observatory is a 1000 T D 2O 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 φ e = 1.76 +0.05 −0.05(stat.) +0.09 −0.09 (syst.) × 10 6 cm −2s −1 based on events with a measured kinetic enegy above 5 MeV. The non- ν e component is φ μτ = 3.41 +0.45 −0.45(stat.) +0.48 −0.45 (syst.) × 10 6 cm −2s −1, 5.3 σ greater than zero, providing strong evidence for solar ν e flavor transformation. The total flux measured with the NC reaction is φ NC = 5.09 +0.044 −0.43(stat.) +0.46 −0.43 (syst.) × 10 6 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.
