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Measurement of the rate of nu(e) + d --> p + p + e(-) interactions produced by (8)B solar neutrinos at the Sudbury Neutrino Observatory |
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| Authors: | Ahmad Q R Allen R C Andersen T C Anglin J D Bühler G Barton J C Beier E W Bercovitch M Bigu J Biller S Black R A Blevis I Boardman R J Boger J Bonvin E Boulay M G Bowler M G Bowles T J Brice S J Browne M C Bullard T V Burritt T H Cameron K Cameron J Chan Y D Chen M Chen H H Chen X Chon M C Cleveland B T Clifford E T Cowan J H Cowen D F Cox G A Dai Y Dai X Dalnoki-Veress F Davidson W F Doe P J Doucas G Dragowsky M R Duba C A Duncan F A Dunmore J Earle E D Elliott S R Evans H C Ewan G T Farine J Fergani H Ferraris A P Ford R J Fowler M M Frame K Frank E D Frati W Germani J V Gil S Goldschmidt A |
| Affiliation: | Center for Experimental Nuclear Physics and Astrophysics, and Department of Physics, University of Washington, Seattle, Washington 98195, USA. |
| 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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