GNO solar neutrino observations: results for GNO I

By M. Altmann, M. Balata, P. Belli, E. Bellotti, R. Bernabei, E. Burkert, C. Cattadori, G. Cerichelli, Marco Chiarini, M. Cribier and 20 more. 2000

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Abstract We report the first GNO solar neutrino results for the measuring period GNO I, solar exposure time May 20, 1998 till January 12, 2000. In the present analysis, counting results for solar runs SR1–SR19 were used till April 4, 2000. With counting completed for all but the last 3 runs (SR17–SR19), the GNO I result is [65.8 ± 10.2 9.6 (stat.) ± 3.4 3.6 (syst.)] SNU (1 σ ) or [65.8 ± 10.7 10.2 (incl. syst.)] SNU (1 σ ) with errors combined. This may be compared to the result for Gallex (I–IV), which is [77.5 ± 7.6 7.8 (incl. syst.)] SNU (1 σ ). A combined result from both GNO I and Gallex (I–IV) together is [74.1 ± 6.7 6.8 (incl. syst.)] SNU (1 σ ).

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1932c98a882e17c3732cf78cd8fd663463e5484d

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In Nuclear and High Energy Physics

Citations in the corpus

Solar neutrinos: Global analysis and implications for SNO (2001, background): “Theanalysis revealsat99:7% C.L.eightcurrently-allowed discrete regionsin two-neutrino oscillation space, ve regionscorresponding to active neutrinosand threecorresponding to sterileneutrinos.”
Nuclear weak-interaction processes in stars (2002, background): “…for example, for 37Cl (Aufderheide et al., 1994a), 40Ar (Ormand et al., 1995) and 71Ga (Haxton, 1998), the detector material in the Homestake (Cleveland et al., 1998), ICARUS4, and GALLEX/SAGE/GNO detectors (Abdurashitov et al., 1999; Altmann et al., 2000; Hampel et al., 1999), respectively.”
Dark energy from mass varying neutrinos (2003, neutral): “1.1 Coincidences and Damn Coincidences 2”