KamLAND and solar antineutrino spectrum |
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Authors: | B. C. Chauhan J. Pulido E. Torrente-Lujan |
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Affiliation: | (1) Centro de Ciências Exatas, Ambientais e de Tecnologias, Pontifícia Universidade Católica de Campinas, Caixa Postal 317, 13020-970 Campinas, SP, Brasil;(2) Instituto de Física Gleb Wataghin, Universidade Estadual de Campinas - UNICAMP, 13083-970 Campinas, SP, Brasil |
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Abstract: | We use the recent KamLAND observations to predict the solar antineutrino spectrum at some confidence limits. We find a scaling of the antineutrino probability with respect to the magnetic field profile—in the sense that the same probability function can be reproduced by any profile with a suitable peak field value—that can be utilized to obtain the general shape ofthe solar antineutrino spectrum. This scaling and the upper bound on the solar antineutrino event rate, which can be derived from the data, lead to: 1) an upper bound on the solar antineutrino flux and 2) the prediction of their energy spectrum. We get (phi _{bar nu } < 3.8 times 10^{ - 3} phi (^8 B)) or (phi _{bar nu } < 5.5 times 10^{ - 3} phi (^8 B)) at 95% C.L., assuming Gaussian or Poissonian statistics, respectively. For 90% C.L., these become (phi _{bar nu } < 3.4 times 10^{ - 3} phi (^8 B)) and (phi _{bar nu } < 4.9 times 10^{ - 3} phi (^8 B)). This provides an improvement by a factor of 3–5 with respect to the existing bounds. These limits are quite general and independent of the detailed structure of the magnetic field in the solar interior. |
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