Reinvestigation of the irregularities in the 3H decay |
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| Institution: | 1. Institució Catalana de Recerca i Etudes Avançats (ICREA), Spain;2. Departament d’Estructura i Constituents de la Matèria and Institut de Ciencies del Cosmos, Universitat de Barcelona, Diagonal 647, E-08028 Barcelona, Spain;3. C.N. Yang Institute for Theoretical Physics, and Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794-3840, USA;4. Wisconsin IceCube Particle Astrophysics Center and Department of Physics, University of Wisconsin, Madison, WI 53706, USA;1. High Energy Accelerator Research Organization, 1-1 Oho, Tsukuba, Ibaraki 305-0801, Japan;2. RCNP, Osaka University, 10-1 Mihogaoka, Ibaraki, Osaka 567-0047, Japan;3. Graduate School of Science, Osaka University, 1-1 Machikaneyama, Toyonaka, Osaka 560-0043, Japan;1. Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China;2. National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China;3. Faculty of Engineering, Yokohama National University, Yokohama 240-8501, Japan;4. Department of Physics, Shandong University, Jinan 250100, China;5. Institute of Modern Physics, Southwest Jiaotong University, Chengdu 610031, China;6. Physics Department of Science School, Tibet University, Lhasa 850000, China;7. Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582, Japan;1. Department of Physics and Astronomy, Michigan State University, BioMedical Physical Sciences Building, East Lansing, MI 48824, United States;2. Department of Physics and Astronomy, University of California, Irvine, CA 92697, United States;3. Santa Cruz Institute for Particle Physics, University of California, 1156 High Street, Santa Cruz, CA 95064, United States;4. Department of Physics, University of Maryland, College Park, MD 20742, United States;5. Department of Physics, New York University, 4 Washington Place, New York, NY 10003, United States;6. Department of Physics, Pennsylvania State University, University Park, PA 16802, United States;7. Group P-23, Los Alamos National Laboratory, P.O. Box 1663, Los Alamos, NM 87545, United States;8. Department of Physics and Astronomy, George Mason University, 4400 University Drive, Fairfax, VA 22030, United States;9. Instituto de Astronomía, Universidad Nacional Autónoma de México, D.F., México 04510, Mexico;10. NASA Goddard Space Flight Center, Greenbelt, MD 20771, United States;11. Department of Physics, Michigan Technological University, Houghton, MI 49931, United States;12. Department of Physics, University of New Hampshire, Morse Hall, Durham, NH 03824, United States;13. University of California Santa Cruz, Natural Science 2, 1156 High Street, Santa Cruz, CA 95064, United States;14. Ohio State University, Lima, OH 45804, United States;15. Department of Physics, The University of Hong Kong, Pokfulam Road, Hong Kong, China |
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| Abstract: | Having in mind the potential impact of the results presented by Veprev and Muromtsev (2012) 13] on our knowledge of the universe, we reinvestigated the liquid scintillation measurement of the count rate variations of 3H. Making use of the sophisticated Quantulus liquid scintillation spectrometer, we found that the measurement of the high-energy tail of 3H spectrum may be significantly influenced by instrumental instability. Thus, the possible explanation for the relatively high count rate variations of Veprev and Muromtsev (2012) 13] can be attributed mainly to the walk of the cut-off in the integrated spectrum, although weak variations of different origin could be masked by such cut-off drifts. In our experiment we have also registered the oscillatory behavior of measured high-energy tail of 3H spectrum, but with very small amplitude (less than 0.5%), which cannot be easily explained only by instrumental instability. When the total 3H spectrum was measured, no significant variations in the count rate were found. |
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| Keywords: | Liquid scintillation counting Cosmic rays |
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