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Ahmed SN, Anthony AE, Beier EW, Bellerive A, Biller SD, Boger J, Boulay MG, Bowler MG, Bowles TJ, Brice SJ, Bullard TV, Chan YD, Chen M, Chen X, Cleveland BT, Cox GA, Dai X, Dalnoki-Veress F, Doe PJ, Dosanjh RS, Doucas G, Dragowsky MR, Duba CA, Duncan FA, Dunford M, Dunmore JA, Earle ED, Elliott SR, Evans HC, Ewan GT, Farine J, Fergani H, Fleurot F, Formaggio JA, Fowler MM, Frame K, Fulsom BG, Gagnon N, Graham K, Grant DR, Hahn RL, Hall JC, Hallin AL, Hallman ED, Hamer AS, Handler WB, Hargrove CK, Harvey PJ, Hazama R, Heeger KM, Heintzelman WJ, Heise J, Helmer RL, Hemingway RJ, Hime A, Howe MA, Jagam P, Jelley NA, Klein JR, Kos MS, Krumins AV, Kutter T, Kyba CCM, Labranche H, Lange R, Law J, Lawson IT, Lesko KT, Leslie JR, Levine I, Luoma S, MacLellan R, Majerus S, Mak HB, Maneira J, Marino AD, McCauley N, McDonald AB, McGee S, McGregor G, Mifflin C, Miknaitis KKS, Miller GG, Moffat BA, Nally CW, Nickel BG, Noble AJ, Norman EB, Oblath NS, Okada CE, Ollerhead RW, Orrell JL, Oser SM, Ouellet C, Peeters SJM, Poon AWP, Robertson BC, Robertson RGH, Rollin E, Rosendahl SSE, Rusu VL, Schwendener MH, Simard O, Simpson JJ, Sims CJ, Sinclair D, Skensved P, Smith MWE, Starinsky N, Stokstad RG, Stonehill LC, Tafirout R, Takeuchi Y, Tesić G, Thomson M, Thorman M, Van Berg R, Van de Water RG, Virtue CJ, Wall BL, Waller D, Waltham CE, Tseung HWC, Wark DL, West N, Wilhelmy JB, Wilkerson JF, Wilson JR, Wouters JM, Yeh M, Zuber K. Measurement of the total active 8B solar neutrino flux at the Sudbury Neutrino Observatory with enhanced neutral current sensitivity. Phys Rev Lett 2004; 92:181301. [PMID: 15169480 DOI: 10.1103/physrevlett.92.181301] [Citation(s) in RCA: 54] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/06/2003] [Indexed: 05/24/2023]
Abstract
The Sudbury Neutrino Observatory has precisely determined the total active (nu(x)) 8B solar neutrino flux without assumptions about the energy dependence of the nu(e) survival probability. The measurements were made with dissolved NaCl in 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) x 10(6) cm(-2) s(-1), in agreement with previous measurements and standard solar models. A global analysis of these and other solar and reactor neutrino results yields Deltam(2)=7.1(+1.2)(-0.6) x 10(-5) eV(2) and theta=32.5(+2.4)(-2.3) degrees. Maximal mixing is rejected at the equivalent of 5.4 standard deviations.
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Affiliation(s)
- S N Ahmed
- Department of Physics, Queen's University, Kingston, Ontario K7L 3N6 Canada
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Ahmed SN, Anthony AE, Beier EW, Bellerive A, Biller SD, Boger J, Boulay MG, Bowler MG, Bowles TJ, Brice SJ, Bullard TV, Chan YD, Chen M, Chen X, Cleveland BT, Cox GA, Dai X, Dalnoki-Veress F, Doe PJ, Dosanjh RS, Doucas G, Dragowsky MR, Duba CA, Duncan FA, Dunford M, Dunmore JA, Earle ED, Elliott SR, Evans HC, Ewan GT, Farine J, Fergani H, Fleurot F, Formaggio JA, Fowler MM, Frame K, Frati W, Fulsom BG, Gagnon N, Graham K, Grant DR, Hahn RL, Hall JC, Hallin AL, Hallman ED, Hamer AS, Handler WB, Hargrove CK, Harvey PJ, Hazama R, Heeger KM, Heintzelman WJ, Heise J, Helmer RL, Hemingway RJ, Hime A, Howe MA, Jagam P, Jelley NA, Klein JR, Kos MS, Krumins AV, Kutter T, Kyba CCM, Labranche H, Lange R, Law J, Lawson IT, Lesko KT, Leslie JR, Levine I, Luoma S, MacLellan R, Majerus S, Mak HB, Maneira J, Marino AD, McCauley N, McDonald AB, McGee S, McGregor G, Mifflin C, Miknaitis KKS, Miller GG, Moffat BA, Nally CW, Neubauer MS, Nickel BG, Noble AJ, Norman EB, Oblath NS, Okada CE, Ollerhead RW, Orrell JL, Oser SM, Ouellet C, Peeters SJM, Poon AWP, Robertson BC, Robertson RGH, Rollin E, Rosendahl SSE, Rusu VL, Schwendener MH, Simard O, Simpson JJ, Sims CJ, Sinclair D, Skensved P, Smith MWE, Starinsky N, Stokstad RG, Stonehill LC, Tafirout R, Takeuchi Y, Tesić G, Thomson M, Thorman M, Van Berg R, Van de Water RG, Virtue CJ, Wall BL, Waller D, Waltham CE, Tseung HWC, Wark DL, West N, Wilhelmy JB, Wilkerson JF, Wilson JR, Wittich P, Wouters JM, Yeh M, Zuber K. Constraints on nucleon decay via invisible modes from the Sudbury Neutrino Observatory. Phys Rev Lett 2004; 92:102004. [PMID: 15089201 DOI: 10.1103/physrevlett.92.102004] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/14/2003] [Indexed: 05/24/2023]
Abstract
Data from the Sudbury Neutrino Observatory have been used to constrain the lifetime for nucleon decay to "invisible" modes, such as n-->3nu. The analysis was based on a search for gamma rays from the deexcitation of the residual nucleus that would result from the disappearance of either a proton or neutron from 16O. A limit of tau(inv)>2 x 10(29) yr is obtained at 90% confidence for either neutron- or proton-decay modes. This is about an order of magnitude more stringent than previous constraints on invisible proton-decay modes and 400 times more stringent than similar neutron modes.
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Affiliation(s)
- S N Ahmed
- Department of Physics, Queen's University, Kingston, Ontario, Canada K7L 3N6
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Ahmad QR, Allen RC, Andersen TC, Anglin JD, Barton JC, Beier EW, Bercovitch M, Bigu J, Biller SD, Black RA, Blevis I, Boardman RJ, Boger J, Bonvin E, Boulay MG, Bowler MG, Bowles TJ, Brice SJ, Browne MC, Bullard TV, Bühler G, Cameron J, Chan YD, Chen HH, Chen M, Chen X, Cleveland BT, Clifford ETH, Cowan JHM, Cowen DF, Cox GA, Dai X, Dalnoki-Veress F, Davidson WF, Doe PJ, Doucas G, Dragowsky MR, Duba CA, Duncan FA, Dunford M, Dunmore JA, Earle ED, Elliott SR, Evans HC, Ewan GT, Farine J, Fergani H, Ferraris AP, Ford RJ, Formaggio JA, Fowler MM, Frame K, Frank ED, Frati W, Gagnon N, Germani JV, Gil S, Graham K, Grant DR, Hahn RL, Hallin AL, Hallman ED, Hamer AS, Hamian AA, Handler WB, Haq RU, Hargrove CK, Harvey PJ, Hazama R, Heeger KM, Heintzelman WJ, Heise J, Helmer RL, Hepburn JD, Heron H, Hewett J, Hime A, Howe M, Hykawy JG, Isaac MCP, Jagam P, Jelley NA, Jillings C, Jonkmans G, Kazkaz K, Keener PT, Klein JR, Knox AB, Komar RJ, Kouzes R, Kutter T, Kyba CCM, Law J, Lawson IT, Lay M, Lee HW, Lesko KT, Leslie JR, Levine I, Locke W, Luoma S, Lyon J, Majerus S, Mak HB, Maneira J, Manor J, Marino AD, McCauley N, McDonald AB, McDonald DS, McFarlane K, McGregor G, Meijer Drees R, Mifflin C, Miller GG, Milton G, Moffat BA, Moorhead M, Nally CW, Neubauer MS, Newcomer FM, Ng HS, Noble AJ, Norman EB, Novikov VM, O'Neill M, Okada CE, Ollerhead RW, Omori M, Orrell JL, Oser SM, Poon AWP, Radcliffe TJ, Roberge A, Robertson BC, Robertson RGH, Rosendahl SSE, Rowley JK, Rusu VL, Saettler E, Schaffer KK, Schwendener MH, Schülke A, Seifert H, Shatkay M, Simpson JJ, Sims CJ, Sinclair D, Skensved P, Smith AR, Smith MWE, Spreitzer T, Starinsky N, Steiger TD, Stokstad RG, Stonehill LC, Storey RS, Sur B, Tafirout R, Tagg N, Tanner NW, Taplin RK, Thorman M, Thornewell PM, Trent PT, Tserkovnyak YI, Van Berg R, Van de Water RG, Virtue CJ, Waltham CE, Wang JX, Wark DL, West N, Wilhelmy JB, Wilkerson JF, Wilson JR, Wittich P, Wouters JM, Yeh M. Measurement of day and night neutrino energy spectra at SNO and constraints on neutrino mixing parameters. Phys Rev Lett 2002; 89:011302. [PMID: 12097026 DOI: 10.1103/physrevlett.89.011302] [Citation(s) in RCA: 66] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/19/2002] [Indexed: 05/23/2023]
Abstract
The Sudbury Neutrino Observatory (SNO) has measured day and night solar neutrino energy spectra and rates. For charged current events, assuming an undistorted 8B spectrum, 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 nu(e) asymmetry is found to be 7.0%+/-4.9%(+1.3%)(-1.2%). A global solar neutrino analysis in terms of matter-enhanced oscillations of two active flavors strongly favors the large mixing angle solution.
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Affiliation(s)
- Q R Ahmad
- Center for Experimental Nuclear Physics and Astrophysics, and Department of Physics, University of Washington, Seattle, Washington 98195, USA
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Ahmad QR, Allen RC, Andersen TC, D Anglin J, Barton JC, Beier EW, Bercovitch M, Bigu J, Biller SD, Black RA, Blevis I, Boardman RJ, Boger J, Bonvin E, Boulay MG, Bowler MG, Bowles TJ, Brice SJ, Browne MC, Bullard TV, Bühler G, Cameron J, Chan YD, Chen HH, Chen M, Chen X, Cleveland BT, Clifford ETH, Cowan JHM, Cowen DF, Cox GA, Dai X, Dalnoki-Veress F, Davidson WF, Doe PJ, Doucas G, Dragowsky MR, Duba CA, Duncan FA, Dunford M, Dunmore JA, Earle ED, Elliott SR, Evans HC, Ewan GT, Farine J, Fergani H, Ferraris AP, Ford RJ, Formaggio JA, Fowler MM, Frame K, Frank ED, Frati W, Gagnon N, Germani JV, Gil S, Graham K, Grant DR, Hahn RL, Hallin AL, Hallman ED, Hamer AS, Hamian AA, Handler WB, Haq RU, Hargrove CK, Harvey PJ, Hazama R, Heeger KM, Heintzelman WJ, Heise J, Helmer RL, Hepburn JD, Heron H, Hewett J, Hime A, Howe M, Hykawy JG, Isaac MCP, Jagam P, Jelley NA, Jillings C, Jonkmans G, Kazkaz K, Keener PT, Klein JR, Knox AB, Komar RJ, Kouzes R, Kutter T, Kyba CCM, Law J, Lawson IT, Lay M, Lee HW, Lesko KT, Leslie JR, Levine I, Locke W, Luoma S, Lyon J, Majerus S, Mak HB, Maneira J, Manor J, Marino AD, McCauley N, McDonald AB, McDonald DS, McFarlane K, McGregor G, Meijer Drees R, Mifflin C, Miller GG, Milton G, Moffat BA, Moorhead M, Nally CW, Neubauer MS, Newcomer FM, Ng HS, Noble AJ, Norman EB, Novikov VM, O'Neill M, Okada CE, Ollerhead RW, Omori M, Orrell JL, Oser SM, Poon AWP, Radcliffe TJ, Roberge A, Robertson BC, Robertson RGH, Rosendahl SSE, Rowley JK, Rusu VL, Saettler E, Schaffer KK, Schwendener MH, Schülke A, Seifert H, Shatkay M, Simpson JJ, Sims CJ, Sinclair D, Skensved P, Smith AR, Smith MWE, Spreitzer T, Starinsky N, Steiger TD, Stokstad RG, Stonehill LC, Storey RS, Sur B, Tafirout R, Tagg N, Tanner NW, Taplin RK, Thorman M, Thornewell PM, Trent PT, Tserkovnyak YI, Van Berg R, Van de Water RG, Virtue CJ, Waltham CE, Wang JX, Wark DL, West N, Wilhelmy JB, Wilkerson JF, Wilson JR, Wittich P, Wouters JM, Yeh M. Direct evidence for neutrino flavor transformation from neutral-current interactions in the Sudbury Neutrino Observatory. Phys Rev Lett 2002; 89:011301. [PMID: 12097025 DOI: 10.1103/physrevlett.89.011301] [Citation(s) in RCA: 170] [Impact Index Per Article: 7.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/19/2002] [Indexed: 05/23/2023]
Abstract
Observations of neutral-current nu interactions on deuterium in the Sudbury Neutrino Observatory are reported. Using the neutral current (NC), elastic scattering, and charged current reactions and assuming the standard 8B shape, the nu(e) component of the 8B solar flux is phis(e) = 1.76(+0.05)(-0.05)(stat)(+0.09)(-0.09)(syst) x 10(6) cm(-2) s(-1) for a kinetic energy threshold of 5 MeV. The non-nu(e) component is phi(mu)(tau) = 3.41(+0.45)(-0.45)(stat)(+0.48)(-0.45)(syst) x 10(6) cm(-2) s(-1), 5.3sigma greater than zero, providing strong evidence for solar nu(e) flavor transformation. The total flux measured with the NC reaction is phi(NC) = 5.09(+0.44)(-0.43)(stat)(+0.46)(-0.43)(syst) x 10(6) cm(-2) s(-1), consistent with solar models.
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Affiliation(s)
- Q R Ahmad
- Center for Experimental Nuclear Physics and Astrophysics, and Department of Physics, University of Washington, Seattle, Washington 98195, USA
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Ahmad QR, Allen RC, Andersen TC, Anglin JD, Bühler G, Barton JC, Beier EW, Bercovitch M, Bigu J, Biller S, Black RA, Blevis I, Boardman RJ, Boger J, Bonvin E, Boulay MG, Bowler MG, Bowles TJ, Brice SJ, Browne MC, Bullard TV, Burritt TH, Cameron K, Cameron J, Chan YD, Chen M, Chen HH, Chen X, Chon MC, Cleveland BT, Clifford ET, Cowan JH, Cowen DF, Cox GA, Dai Y, Dai X, Dalnoki-Veress F, Davidson WF, Doe PJ, Doucas G, Dragowsky MR, Duba CA, Duncan FA, Dunmore J, Earle ED, Elliott SR, Evans HC, Ewan GT, Farine J, Fergani H, Ferraris AP, Ford RJ, Fowler MM, Frame K, Frank ED, Frati W, Germani JV, Gil S, Goldschmidt A, Grant DR, Hahn RL, Hallin AL, Hallman ED, Hamer A, Hamian AA, Haq RU, Hargrove CK, Harvey PJ, Hazama R, Heaton R, Heeger KM, Heintzelman WJ, Heise J, Helmer RL, Hepburn JD, Heron H, Hewett J, Hime A, Howe M, Hykawy JG, Isaac MC, Jagam P, Jelley NA, Jillings C, Jonkmans G, Karn J, Keener PT, Kirch K, Klein JR, Knox AB, Komar RJ, Kouzes R, Kutter T, Kyba CC, Law J, Lawson IT, Lay M, Lee HW, Lesko KT, Leslie JR, Levine I, Locke W, Lowry MM, Luoma S, Lyon J, Majerus S, Mak HB, Marino AD, McCauley N, McDonald AB, McDonald DS, McFarlane K, McGregor G, McLatchie W, Meijer Drees R, Mes H, Mifflin C, Miller GG, Milton G, Moffat BA, Moorhead M, Nally CW, Neubauer MS, Newcomer FM, Ng HS, Noble AJ, Norman EB, Novikov VM, O'Neill M, Okada CE, Ollerhead RW, Omori M, Orrell JL, Oser SM, Poon AW, Radcliffe TJ, Roberge A, Robertson BC, Robertson RG, Rowley JK, Rusu VL, Saettler E, Schaffer KK, Schuelke A, Schwendener MH, Seifert H, Shatkay M, Simpson JJ, Sinclair D, Skensved P, Smith AR, Smith MW, Starinsky N, Steiger TD, Stokstad RG, Storey RS, Sur B, Tafirout R, Tagg N, Tanner NW, Taplin RK, Thorman M, Thornewell P, Trent PT, Tserkovnyak YI, Van Berg R, Van de Water RG, Virtue CJ, Waltham CE, Wang JX, Wark DL, West N, Wilhelmy JB, Wilkerson JF, Wilson J, Wittich P, Wouters JM, Yeh M. Measurement of the rate of nu(e) + d --> p + p + e(-) interactions produced by (8)B solar neutrinos at the Sudbury Neutrino Observatory. Phys Rev Lett 2001; 87:071301. [PMID: 11497878 DOI: 10.1103/physrevlett.87.071301] [Citation(s) in RCA: 169] [Impact Index Per Article: 7.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/18/2001] [Indexed: 05/23/2023]
Abstract
Solar neutrinos from (8)B decay have been detected at the Sudbury Neutrino Observatory via the charged current (CC) reaction on deuterium and the elastic scattering (ES) of electrons. The flux of nu(e)'s is measured by the CC reaction rate to be straight phi(CC)(nu(e)) = 1.75 +/- 0.07(stat)(+0.12)(-0.11)(syst) +/- 0.05(theor) x 10(6) cm(-2) s(-1). Comparison of straight phi(CC)(nu(e)) to the Super-Kamiokande Collaboration's precision value of the flux inferred from the ES reaction yields a 3.3 sigma difference, assuming the systematic uncertainties are normally distributed, providing evidence of an active non- nu(e) component in the solar flux. The total flux of active 8B neutrinos is determined to be 5.44+/-0.99 x 10(6) cm(-2) s(-1).
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Affiliation(s)
- Q R Ahmad
- Center for Experimental Nuclear Physics and Astrophysics, and Department of Physics, University of Washington, Seattle, Washington 98195, USA
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