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作者机构:Solar Terrestrial Environment Laboratory Nagoya University Nagoya Aichi 464-8602 Japan Kamioka Observatory Institute for Cosmic Ray Research University of Tokyo Kamioka Gifu 506-1205 Japan Kavli Institute for the Physics and Mathematics of the Universe (WPI) Todai Institutes for Advanced Study University of Tokyo Kashiwa Chiba 277-8582 Japan Research Center for Cosmic Neutrinos Institute for Cosmic Ray Research University of Tokyo Kashiwa Chiba 277-8582 Japan Department of Theoretical Physics University Autonoma Madrid 28049 Madrid Spain Department of Physics Boston University Boston Massachusetts 02215 USA Department of Physics and Astronomy University of British Columbia Vancouver British Columbia V6T1Z4 Canada Physics Department Brookhaven National Laboratory Upton New York 11973 USA Department of Physics and Astronomy University of California Irvine Irvine California 92697-4575 USA Department of Physics California State University Dominguez Hills Carson California 90747 USA Department of Physics Chonnam National University Kwangju 500-757 Korea Department of Physics Duke University Durham North Carolina 27708 USA Junior College Fukuoka Institute of Technology Fukuoka Fukuoka 811-0295 Japan Department of Physics Gifu University Gifu Gifu 501-1193 Japan GIST College Gwangju Institute of Science and Technology Gwangju 500-712 Korea Department of Physics and Astronomy University of Hawaii Honolulu Hawaii 96822 USA High Energy Accelerator Research Organization (KEK) Tsukuba Ibaraki 305-0801 Japan Department of Physics Kobe University Kobe Hyogo 657-8501 Japan Department of Physics Kyoto University Kyoto Kyoto 606-8502 Japan Department of Physics Miyagi University of Education Sendai Miyagi 980-0845 Japan National Centre For Nuclear Research 00-681 Warsaw Poland Department of Physics and Astronomy State University of New York at Stony Brook Stony Brook New York 11794-3800 USA Department of Physics Okayama University Okayama Okayama 700-8530 Japan Department of Physics Osaka University Toyonaka Osaka 560-0043 Japan Department of Physics University of Regina 3737 Wascana Parkway Regina Saskatchewan S4SOA2 Canada TRIUMF 4004 Wesbrook Mall Vancouver British Columbia V6T2A3 Canada Department of Physics Seoul National University Seoul 151-742 Korea Department of Informatics in Social Welfare Shizuoka University of Welfare Yaizu Shizuoka 425-8611 Japan Department of Physics Sungkyunkwan University Suwon 440-746 Korea Department of Physics Tokai University Hiratsuka Kanagawa 259-1292 Japan The University of Tokyo Bunkyo Tokyo 113-0033 Japan Department of Physics University of Toronto 60 Street Toronto Ontario M5S1A7 Canada Department of Engineering Physics Tsinghua University Beijing 100084 China Department of Physics University of Washington Seattle Washington 98195-1560 USA
出 版 物:《Physical Review Letters》 (Phys Rev Lett)
年 卷 期:2015年第114卷第14期
页 面:141301-141301页
核心收录:
基 金:Japan Society for the Promotion of Science, JSPS, (23340062) Japan Society for the Promotion of Science, JSPS
主 题:NEUTRINOS LEPTONS (Nuclear physics) DARK matter (Astronomy) INTERSTELLAR matter COSMOLOGY
摘 要:Super-Kamiokande (SK) can search for weakly interacting massive particles (WIMPs) by detecting neutrinos produced from WIMP annihilations occurring inside the Sun. In this analysis, we include neutrino events with interaction vertices in the detector in addition to upward-going muons produced in the surrounding rock. Compared to the previous result, which used the upward-going muons only, the signal acceptances for light (few−GeV/c2−200−GeV/c2) WIMPs are significantly increased. We fit 3903 days of SK data to search for the contribution of neutrinos from WIMP annihilation in the Sun. We found no significant excess over expected atmospheric-neutrino background and the result is interpreted in terms of upper limits on WIMP-nucleon elastic scattering cross sections under different assumptions about the annihilation channel. We set the current best limits on the spin-dependent WIMP-proton cross section for WIMP masses below 200 GeV/c2 (at 10 GeV/c2, 1.49×10−39 cm2 for χχ→bb¯ and 1.31×10−40 cm2 for χχ→τ+τ− annihilation channels), also ruling out some fraction of WIMP candidates with spin-independent coupling in the few−GeV/c2 mass range.