Solar neutrino results in Super-Kamiokande-III

Published

Journal Article

The results of the third phase of the Super-Kamiokande solar neutrino measurement are presented and compared to the first and second phase results. With improved detector calibrations, a full detector simulation, and improved analysis methods, the systematic uncertainty on the total neutrino flux is estimated to be ±2.1%, which is about two thirds of the systematic uncertainty for the first phase of Super-Kamiokande. The observed B8 solar flux in the 5.0 to 20 MeV total electron energy region is 2.32±0.04(stat) ±0.05(sys)×106cm - 2sec - 1 under the assumption of pure electron-flavor content, in agreement with previous measurements. A combined oscillation analysis is carried out using SK-I, II, and III data, and the results are also combined with the results of other solar neutrino experiments. The best-fit oscillation parameters are obtained to be sin 2θ 12 =0.30-0.01+0.02( tan 2θ 12 =0.42-0.02+0.04) and Δm212=6.2-1.9+1.1×10 - 5eV2. Combined with KamLAND results, the best-fit oscillation parameters are found to be sin 2θ 12 =0.31±0. 01( tan 2θ 12 =0.44±0.03) and Δm212=7.6±0.2×10 - 5eV2. The B8 neutrino flux obtained from global solar neutrino experiments is 5.3±0.2(stat+sys) ×106cm - 2s - 1, while the B8 flux becomes 5.1±0.1(stat+sys)×106cm - 2s - 1 by adding KamLAND results. In a three-flavor analysis combining all solar neutrino experiments, the upper limit of sin 2θ 13 is 0.060 at 95% C.L.. After combination with KamLAND results, the upper limit of sin 2θ 13 is found to be 0.059 at 95% C.L. © 2011 American Physical Society.

Full Text

Duke Authors

Cited Authors

  • Abe, K; Hayato, Y; Iida, T; Ikeda, M; Ishihara, C; Iyogi, K; Kameda, J; Kobayashi, K; Koshio, Y; Kozuma, Y; Miura, M; Moriyama, S; Nakahata, M; Nakayama, S; Obayashi, Y; Ogawa, H; Sekiya, H; Shiozawa, M; Suzuki, Y; Takeda, A; Takenaga, Y; Ueno, K; Ueshima, K; Watanabe, H; Yamada, S; Yokozawa, T; Hazama, S; Kaji, H; Kajita, T; Kaneyuki, K; McLachlan, T; Okumura, K; Shimizu, Y; Tanimoto, N; Vagins, MR; Labarga, L; Magro, LM; Dufour, F; Kearns, E; Litos, M; Raaf, JL; Stone, JL; Sulak, LR; Wang, W; Goldhaber, M; Bays, K; Casper, D; Cravens, JP; Kropp, WR; Mine, S; Regis, C; Renshaw, A; Smy, MB; Sobel, HW; Ganezer, KS; Hill, J; Keig, WE; Jang, JS; Kim, JY; Lim, IT; Albert, J; Wendell, R; Wongjirad, T; Scholberg, K; Walter, CW; Ishizuka, T; Tasaka, S; Learned, JG; Matsuno, S; Watanabe, Y; Hasegawa, T; Ishida, T; Ishii, T; Kobayashi, T; Nakadaira, T; Nakamura, K; Nishikawa, K; Nishino, H; Oyama, Y; Sakashita, K; Sekiguchi, T; Tsukamoto, T; Suzuki, AT; Takeuchi, Y; Minamino, A; Nakaya, T; Fukuda, Y; Itow, Y; Mitsuka, G; Tanaka, T; Jung, CK; Lopez, G; McGrew, C; Terri, R; Yanagisawa, C; Tamura, N; Ishino, H; Kibayashi, A; Mino, S; Mori, T

Published Date

  • March 24, 2011

Published In

Volume / Issue

  • 83 / 5

Electronic International Standard Serial Number (EISSN)

  • 1550-2368

International Standard Serial Number (ISSN)

  • 1550-7998

Digital Object Identifier (DOI)

  • 10.1103/PhysRevD.83.052010

Citation Source

  • Scopus