ABE, S.; ENOMOTO, S.; FURUNO, K.; GANDO, Y.; IKEDA, H.; INOUE, K.; KIBE, Y.; KISHIMOTO, Y.; KOGA, M.; MINEKAWA, Y.; MITSUI, T.; NAKAJIMA, K.; NAKAMURA, K.; NAKAMURA, M.; SHIMIZU, I.; SHIMIZU, Y.; SHIRAI, J.; SUEKANE, F.; SUZUKI, A.; TAKEMOTO, Y.; TAMAE, K.; TERASHIMA, A.; WATANABE, H.; YONEZAWA, E.; YOSHIDA, S.; KOZLOV, A.; MURAYAMA, H.; BUSENITZ, J.; CLASSEN, T.; GRANT, C.; KEEFER, G.; S. LEONARD, D.; MCKEE, D.; PIEPKE, A.; I. BANKS, T.; BLOXHAM, T.; A. DETWILER, J.; J. FREEDMAN, S.; K. FUJIKAWA, B.; GRAY, F.; GUARDINCERRI, E.; HSU, L.; ICHIMURA, K.; KADEL, R.; LENDVAI, C.; LUK, K.-B.; O'DONNELL, T.; M. STEINER, H.; A. WINSLOW, L.; DWYER, D.A.; JILLINGS, C.; MAUGER, C.; D. MCKEOWN, R.; VOGEL, P.; ZHANG, C.; E. BERGER, B.; E. LANE, C.; MARICIC, J.; MILETIC, T.; BATYGOV, M.; G. LEARNED, J.; MATSUNO, S.; PAKVASA, S.; FOSTER, J.; A. HORTON-SMITH, G.; TANG, A.; DAZELEY, S.; E. DOWNUM, K.; GRATTA, G.; TOLICH, K.; BUGG, W.; EFREMENKO, Y.; KAMYSHKOV, Y.; PEREVOZCHIKOV, O.; J. KARWOWSKI, H.; M. MARKOFF, D.; TORNOW, W.; M. HEEGER, K.; PIQUEMAL, F.; RICOL, J.S.; P. DECOWSKI, M.

doi:10.1103/PhysRevC.81.025807

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ABE, S.

ENOMOTO, S.

FURUNO, K.

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Physical Review C. 2010-02, vol. 81, p. 025807

American Physical Society

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Radioactive isotopes produced through cosmic muon spallation are a background for rare-event detection in ν detectors, double-β-decay experiments, and dark-matter searches. Understanding the nature of cosmogenic backgrounds is particularly important for future experiments aiming to determine the pep and CNOsolar neutrino fluxes, for which the background is dominated by the spallation production of 11C. Data from the Kamioka liquid-scintillator antineutrino detector (KamLAND) provides valuable information for better understanding these backgrounds, especially in liquid scintillators, and for checking estimates from current simulations based upon MUSIC, FLUKA, and GEANT4. Using the time correlation between detected muons and neutron captures, the neutron production yield in the KamLAND liquid scintillator is measured to be Yn = (2.8 ± 0.3) × 10−4 μ −1 g−1 cm2. For other isotopes, the production yield is determined from the observed time correlation related to known isotope lifetimes.We find some yields are inconsistent with extrapolations based on an accelerator muon beam experiment.< Réduire

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Production of radioactive isotopes through cosmic muon spallation in KamLAND

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