No abstract

Reference [15] should read as follows:[15] S. M. Bilenky and B.

The first results of the solar neutrino flux measurement from Super-Kamiokande are presented. The results shown here are obtained from data taken between 31 May 1996, and 23 June 1997. Using our measurement of recoil electrons with energies above 6.5 MeV, we infer the total flux of 8 B solar neutrinos to be 2.42 6 0.06͑stat͒ 10.10 20.07 ͑syst͒ 3 10 6 cm 22 s 21 . This result is consistent with the Kamiokande measurement and is 36% of the flux predicted by the BP95 solar model. The flux is also measured in 1.5 month subsets and shown to be consistent with a constant rate. [S0031-9007(98)06804-5] PACS numbers: 26.65. + t, 95.85.Ry, 96.40.Tv

The flavor ratio of the atmospheric neutrino flux and its zenith angle dependence have been studied in the multi-GeV energy range using an exposure of 25.5 kiloton-years of the Super-Kamiokande detector. By comparing the data to a detailed Monte Carlo simulation, the ratio (µ/e) DAT A /(µ/e) MC was measured to be 0.66 ± 0.06(stat.) ± 0.08(sys.). In addition, a strong distortion in the shape of the µ-like event zenith angle distribution was observed. The ratio of the number of upward to downward µ-like events was found to be 0.52 +0.07 −0.06 (stat.) ± 0.01(sys.), with an expected value of 0.98 ± 0.03(stat.) ± 0.02(sys.), while the same ratio for the e-like events was consistent with unity.

From an exposure of 25.5 kiloton-years of the Super-Kamiokande detector, 900 muon-like and 983 electronlike single-ring atmospheric neutrino interactions were detected with momentum p e > 100 MeV/c, p µ > 200 MeV/c, and with visible energy less than 1.33 GeV. Using a detailed Monte Carlo simulation, the ratio (µ/e) DAT A /(µ/e) MC was measured to be 0.61 ± 0.03(stat.) ± 0.05(sys.), consistent with previous results from the Kamiokande, IMB and Soudan-2 experiments, and smaller than expected from theoretical models of atmospheric neutrino production.