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51. Cosmic-ray muon fluxes deep underground: Intensity vs depth, and the neutrino-induced component

Author

M. Crouch, J. Lathrop, H. Coxell, Frederick Reines, J.P.F. Sellschop, W. G. Sandie, P. B. Landecker, and Henry W. Sobel

Subjects
Angular distribution, Muon, Computer science, Cosmic ray, Atomic physics, Neutrino, Intensity (heat transfer)
Abstract

The angular distribution of muons observed deep underground (10788 ft, or 8.89 \ifmmode\times\else\texttimes\fi{} ${10}^{5}$ g ${\mathrm{cm}}^{\ensuremath{-}2}$ standard rock) has been measured with a ${174\ensuremath{-}\mathrm{m}}^{2}$ liquid scintillation detector in conjunction with 48 384 neon flash tubes. The data are fitted by a curve giving the vertical intensity of muons vs vertical depth ${h}_{0}$ as ${I}_{v\ensuremath{\mu}}({h}_{0})=A \mathrm{exp}(\frac{\ensuremath{-}{h}_{0}}{\ensuremath{\lambda}})+{I}_{v\ensuremath{\mu}}^{(\ensuremath{\nu})}$, where $A=(2.26\ifmmode\pm\else\textpm\fi{}0.16)\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}6}$ ${\mathrm{cm}}^{\ensuremath{-}2}$ ${\mathrm{sec}}^{\ensuremath{-}1}$ ${\mathrm{sr}}^{\ensuremath{-}1}$, and $\ensuremath{\gamma}=(7.58\ifmmode\pm\else\textpm\fi{}0.09)\ifmmode\times\else\texttimes\fi{}{10}^{4}$ g ${\mathrm{cm}}^{\ensuremath{-}2}$. The constant term, representing the measured depth-independent flux of muons produced in the surrounding rock by interactions of cosmic-ray neutrinos generated in the earth's atmosphere, has the value ${I}_{v\ensuremath{\mu}}^{(\ensuremath{\nu})}=(2.23\ifmmode\pm\else\textpm\fi{}0.20)\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}13}$ ${\mathrm{cm}}^{\ensuremath{-}2}$ ${\mathrm{sec}}^{\ensuremath{-}1}$ ${\mathrm{sr}}^{\ensuremath{-}1}$. This observed flux is in fair agreement with that predicted assuming a cosmic-ray neutrino flux which is a composite of several theoretical estimates. Thus the flux of muons from extraterrestrial neutrinos is ${10}^{\ensuremath{-}13}$ ${\mathrm{cm}}^{\ensuremath{-}2}$ ${\mathrm{sec}}^{\ensuremath{-}1}$ ${\mathrm{sr}}^{\ensuremath{-}1}$.

Published
1991

52. Stability of the Neutrino

Author

Frederick Reines, Henry W. Sobel, and H. S. Gurr

Subjects
Physics, Particle physics, Solar neutrino, High Energy Physics::Phenomenology, Decay length, High Energy Physics::Experiment, Fission reactor, Neutrino, Electron neutrino
Abstract

Limits of g ${10}^{5}$ astronomical units are set on the decay length of an electron antineutrino ${\overline{\ensuremath{\nu}}}_{e}$ via the process ${\overline{\ensuremath{\nu}}}_{e}\ensuremath{\rightarrow}{\ensuremath{\nu}}^{\ensuremath{'}}+\ensuremath{\gamma}$ for ${E}_{\ensuremath{\gamma}}$ in the range 0.1-0.5 MeV using the results from a well-shielded detector in the vicinity of a fission reactor. This mode of decay is therefore ruled out as a possible explanation for the paucity of solar neutrinos revealed by the experiment of Davis.

Published
1991

53. Yoji Totsuka (1942–2008)

Author

Henry W. Sobel and Yoshihiro Suzuki

Subjects
Multidisciplinary, media_common.quotation_subject, Art history, Art, Obituary, media_common
Published
2008

54. Search for Nucleon Decay via Modes Favored by Supersymmetric Grand Unification Models in Super-Kamiokande-I

Author

Masatoshi Koshiba, Shoei Nakayama, Yuichi Oyama, A. Kibayashi, J. Ishii, K. Kaneyuki, J. Hill, Y. Gando, S. Matsuno, Yasunari Suzuki, Makoto Sakuda, Y. Takeuchi, Shinya Yamada, Toshio Namba, Y. Totsuka, Yusuke Koshio, R. Nambu, Mark R. Vagins, T. Ishizuka, H. Maesaka, M. Goldhaber, Taichi Morita, R. W. Ellsworth, A. Suzuki, M. Earl, Masashi Yokoyama, J. A. Goodman, R. Svoboda, Magdalena Malek, J. Zalipska, T. Harada, Tsuyoshi Nakaya, T. Ishida, C. McGrew, M. Ishitsuka, C. W. Walter, Y. Hayato, S. B. Kim, J. Y. Kim, J. Yoo, Shantanu Desai, Masato Shiozawa, Y. Choi, N. Tamura, T. Sasaki, J. L. Stone, L. R. Sulak, Henry W. Sobel, K. Nitta, Shoji Yamamoto, Koji Nakamura, A. Minamino, Kyoshi Nishijima, Michael B. Smy, T. Ooyabu, Masayuki Nakahata, Takaaki Kajita, H. Seo, Shigetaka Moriyama, Y. Fukuda, A. L. Stachyra, T. J. Haines, A. Sarrat, David William Casper, C. Mitsuda, J. Hosaka, A. K. Ichikawa, M. D. Messier, K. K. Shiraishi, D. W. Liu, C. Mauger, D. Takemori, K. Taki, A. Okada, H. G. Berns, J. Kameda, C. W. Sterner, D. Turcan, Y. Nakajima, K. Ishihara, T. Kobayashi, K. Hayashi, S. Ueda, T. Maruyama, Ko Okumura, John G. Learned, Y. Ashie, G. W. Sullivan, Katsuhiro Kobayashi, Kunio Inoue, J. S. Jang, K. Nishikawa, Y. Watanabe, S. Mine, T. Toshito, J. P. Cravens, W. R. Kropp, G. Guillian, T. Iwashita, S. Likhoded, Yoshitaka Itow, Y. Kuno, T. Kato, C. K. Jung, Minoru Yoshida, D. Kielczewska, Kazumasa Miyano, K. S. Ganezer, I. Kato, Y. Obayashi, W. E. Keig, Y. Takenaga, Masaya Hasegawa, M. Miura, K. Washburn, S. Hatakeyama, R. Gran, E. Blaufuss, C. Yanagisawa, Atsumu Suzuki, E. Kearns, T. Nakadaira, Takehisa Hasegawa, C. Saji, Hirokazu Ishino, W. Wang, H. Okazawa, Alec Habig, J. Shirai, Shigeki Tasaka, E. Sharkey, S. Dazeley, W. Gajewski, Kate Scholberg, T. Ishii, R. J. Wilkes, and I. T. Lim

Subjects
Physics, Nuclear and High Energy Physics, Particle physics, High Energy Physics::Phenomenology, Supersymmetry, High Energy Physics - Experiment, Particle decay, TheoryofComputation_ANALYSISOFALGORITHMSANDPROBLEMCOMPLEXITY, Mass spectrum, Grand Unified Theory, High Energy Physics::Experiment, Neutron, Neutrino, Nucleon, Super-Kamiokande
Abstract

We report the results for nucleon decay searches via modes favored by supersymmetric grand unified models in Super-Kamiokande. Using 1489 days of full Super-Kamiokande-I data, we searched for $p \to \bar{\nu} K^+$, $n \to \bar{\nu} K^0$, $p \to \mu^+ K^0$ and $p \to e^+ K^0$ modes. We found no evidence for nucleon decay in any of these modes. We set lower limits of partial nucleon lifetime 2.3$\times10^{33}$, 1.3$\times10^{32}$, 1.3$\times10^{33}$ and 1.0$\times10^{33}$ years at 90% confidence level for $p \to \bar{\nu} K^+$, $n \to \bar{\nu} K^0$, $p \to \mu^+ K^0$ and $p \to e^+ K^0$ modes, respectively. These results give a strong constraint on supersymmetric grand unification models., Comment: 14 pages, 13 figures

Published
2005

55. Evidence for Neutrino Instability

Author

Henry W. Sobel, Frederick Reines, and E. Pasierb

Subjects
Physics, Particle physics, Antiparticle, Neutral current, Antimatter, General Physics and Astronomy, Elementary particle, Fermion, Neutrino, Neutrino oscillation, Lepton
Abstract

We report evidence for neutrino instability obtained from the analysis of data taken on the charged and neutral current branches of the reaction $$ \overline {v_e } + d\left( {\begin{array}{*{20}c} { \nearrow \;n + n + e^ + \;c.c.} \\ { \searrow \;n + p + \overline {v_e } \;n.c.} \\ \end{array} } \right) $$ at 11.2 meters from a 2000 MW Savannah River reactor. Tests of the results show them to be consistent with data on \( \overline {\nu _e } + p \to n + e^ + \) also taken at 11.2 meters and 6.0 meters.

Published
1980

56. Calculation of Atmospheric Neutrino-Induced Backgrounds in a Nucleon-Decay Search

Author

Lawrence Sulak, J. Schultz, T. J. Haines, M. Goldhaber, D. Sinclair, R. Svoboda, J. L. Stone, Geoffrey Blewitt, Sally Seidel, L. R. Price, Henry W. Sobel, T. W. Jones, E. Shumard, W. Gajewski, S. Errede, E. Lehmann, J. C. van der Velde, H.-S. Park, J. M. LoSecco, Craig R. Wuest, Frederick Reines, John Matthews, David William Casper, R. Claus, John G. Learned, C. B. Bratton, B. G. Cortez, R. M. Bionta, K. S. Ganezer, W. R. Kropp, G. W. Foster, and D. Kielczewska

Subjects
Nuclear physics, Physics, Massless particle, Particle physics, Muon, Pion, Meson, General Physics and Astronomy, High Energy Physics::Experiment, Neutrino, Nucleon, Radioactive decay, Lepton
Abstract

We have developed an extensive model of atmospheric ..nu.. interactions which provide the backgrounds to nucleon-decay experiments. We report results from a 417-live-day exposure of the Irvine-Michigan-Brookhaven detector. During this time 401 contained events were observed at a rate and with characteristics consistent with atmospheric ..nu.. interactions. We have calculated the expected backgrounds to a variety of two- and three-body decay modes and have set lower limits on many nucleon partial lifetimes.

Published
1986

57. Cosmic-ray muon fluxes deep underground: Intensity vs depth, and the neutrino-induced component

Author

J. Lathrop, H. Coxell, Frederick Reines, J.P.F. Sellschop, P. B. Landecker, M. Crouch, Henry W. Sobel, and W. G. Sandie

Subjects
Physics, Massless particle, Particle physics, Muon, Elementary particle, Cosmic ray, Fermion, Neutrino, Intensity (heat transfer), Lepton
Abstract

The angular distribution of muons observed deep underground (10788 ft, or 8.89 \ifmmode\times\else\texttimes\fi{} ${10}^{5}$ g ${\mathrm{cm}}^{\ensuremath{-}2}$ standard rock) has been measured with a ${174\ensuremath{-}\mathrm{m}}^{2}$ liquid scintillation detector in conjunction with 48 384 neon flash tubes. The data are fitted by a curve giving the vertical intensity of muons vs vertical depth ${h}_{0}$ as ${I}_{v\ensuremath{\mu}}({h}_{0})=A \mathrm{exp}(\frac{\ensuremath{-}{h}_{0}}{\ensuremath{\lambda}})+{I}_{v\ensuremath{\mu}}^{(\ensuremath{\nu})}$, where $A=(2.26\ifmmode\pm\else\textpm\fi{}0.16)\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}6}$ ${\mathrm{cm}}^{\ensuremath{-}2}$ ${\mathrm{sec}}^{\ensuremath{-}1}$ ${\mathrm{sr}}^{\ensuremath{-}1}$, and $\ensuremath{\gamma}=(7.58\ifmmode\pm\else\textpm\fi{}0.09)\ifmmode\times\else\texttimes\fi{}{10}^{4}$ g ${\mathrm{cm}}^{\ensuremath{-}2}$. The constant term, representing the measured depth-independent flux of muons produced in the surrounding rock by interactions of cosmic-ray neutrinos generated in the earth's atmosphere, has the value ${I}_{v\ensuremath{\mu}}^{(\ensuremath{\nu})}=(2.23\ifmmode\pm\else\textpm\fi{}0.20)\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}13}$ ${\mathrm{cm}}^{\ensuremath{-}2}$ ${\mathrm{sec}}^{\ensuremath{-}1}$ ${\mathrm{sr}}^{\ensuremath{-}1}$. This observed flux is in fair agreement with that predicted assuming a cosmic-ray neutrino flux which is a composite of several theoretical estimates. Thus the flux of muons from extraterrestrial neutrinos is ${10}^{\ensuremath{-}13}$ ${\mathrm{cm}}^{\ensuremath{-}2}$ ${\mathrm{sec}}^{\ensuremath{-}1}$ ${\mathrm{sr}}^{\ensuremath{-}1}$.

Published
1978

58. Muons Produced By Atmospheric Neutrinos: Experiment

Author

H. S. Gurr, W. R. Kropp, Frederick Reines, Henry W. Sobel, J.P.F. Sellschop, M. Crouch, B. S. Meyer, and J. Lathrop

Subjects
Nuclear physics, Physics, Particle physics, Muon, Hodoscope, Physics::Instrumentation and Detectors, Muon flux, Theoretical models, High Energy Physics::Experiment, Cosmic ray, Production (computer science), Neutrino, Energy (signal processing)
Abstract

The interaction of high-energy muon neutrinos produced in the atmosphere by primary cosmic rays has been observed deep underground (8.74\ifmmode\times\else\texttimes\fi{}${10}^{5}$ g ${\mathrm{cm}}^{\ensuremath{-}2}$ std. rock) in the rock surrounding a large-area (160 ${\mathrm{m}}^{2}$) liquid-scintillation-detector hodoscope. A series of arguments is given to separate the residual atmospheric muons which reached the detector from those produced by neutrino interactions in the surrounding rock. These arguments are based on the widely differing angular distributions and mean energies of the two sources. The observation of four events arising from the decay of muons stopping in the detector suggests that the energy of neutrino-induced muons is \ensuremath{\sim}\textonehalf{} GeV. Operation of the system over a three-year period yielded a total of 39 which we identify as neutrino-produced muons. Of these, 35 were in the aperture chosen for the observation of neutrino-induced muons, yielding a total rate of (6.5\ifmmode\pm\else\textpm\fi{}1.1)\ifmmode\times\else\texttimes\fi{}${10}^{\ensuremath{-}7}$ ${\mathrm{sec}}^{\ensuremath{-}1}$. In a companion paper, this result is compared with rates predicted using various theoretical models of the neutrino-nucleon interaction. This comparison selects the most appropriate model and leads to an underground neutrino-induced muon flux. In the present paper the simplifying approximation of an isotropic neutrino distribution leads directly to a flux of (3.7\ifmmode\pm\else\textpm\fi{}0.6)\ifmmode\times\else\texttimes\fi{}${10}^{\ensuremath{-}13}$ ${\mathrm{cm}}^{\ensuremath{-}2}$ ${\mathrm{sec}}^{\ensuremath{-}1}$ ${\mathrm{sr}}^{\ensuremath{-}1}$.

Published
1971

59. Cosmic-Ray Muon Intensity Deep Underground versus Depth

Author

M. Crouch, J. Lathrop, Henry W. Sobel, W. R. Kropp, H. S. Gurr, J.P.F. Sellschop, Frederick Reines, and B. S. Meyer

Subjects
Nuclear physics, Physics, Muon, Scintillation counter, Cosmic ray, Spectral line, Intensity (physics)
Published
1970

60. Search forν¯e+e−Scattering

Author

Frederick Reines, Henry W. Sobel, and H. S. Gurr

Subjects
Physics, Nuclear physics, Elastic scattering, Fission, Scattering, Scintillation counter, General Physics and Astronomy, Neutrino, Scintillator, Electron neutrino, Lepton
Abstract

An improved cross-section upper limit of 1.9 times that of V−A theory is determined for the reaction ν¯e+e−→ν¯e+e−. The target, a 7.84-kg plastic scintillator, was enclosed by a composite 330-kg NaI and 2200-liter liquid anticoincidence detector, and was operated in a fission ν¯e flux of 2.2×1013 cm−2 sec−1. We note some constraints which this limit imposes on theoretical conjectures.

Published
1972

61. Observation of a neutrino burst in coincidence with supernova 1987A in the Large Magellanic Cloud

Author

M. Crouch, Lawrence Sulak, Todd Haines, John G. Learned, L. R. Price, J. C. van der Velde, R. M. Bionta, M. Goldhaber, Stephen T. Dye, Sally Seidel, Robert Svoboda, D. Casper, John M. LoSecco, J. Schultz, D. Sinclair, W. R. Kropp, Frederick Reines, John Matthews, Richard Miller, C. Wuest, J. L. Stone, B. G. Cortez, K. S. Ganezer, C. B. Bratton, Geoff Thornton, Henry W. Sobel, Geoffrey Blewitt, G. W. Foster, R. Claus, S. Errede, D. Kielczewska, Alessandra Ciocio, E. Shumard, W. Gajewski, H. S. Park, T. W. Jones, and M. S. Mudan

Subjects
Physics, Physics::Instrumentation and Detectors, Cherenkov detector, Astrophysics::High Energy Astrophysical Phenomena, General Physics and Astronomy, Astronomy, Astrophysics, Coincidence, Particle detector, law.invention, Supernova, Neutrino detector, law, High Energy Physics::Experiment, Neutrino, Large Magellanic Cloud, Astrophysics::Galaxy Astrophysics, Cherenkov radiation
Abstract

A burst of eight neutrino events a preceding the optical detection of the supernova in the Large Magellanic Cloud has been observed in a large underground water Cherenkov detector. The events span an interval of 6 s and have visible energies in the range 20-40 MeV.

Published
1987

62. Test of neutrino oscillations using atmospheric neutrinos

Author

Lawrence Sulak, K. S. Ganezer, B. G. Cortez, David William Casper, J. Schultz, van der Velde Jc, E. Shumard, W. Gajewski, John G. Learned, J. L. Stone, Henry W. Sobel, S. Errede, T. J. Haines, D. Kielczewska, R. M. Bionta, G. W. Foster, R. Claus, Sally Seidel, P. Chrysicopoulou, W. R. Kropp, H.-S. Park, M. Goldhaber, John M. LoSecco, E. Lehmann, Biewitt G, Craig R. Wuest, D. Sinclair, R. Svoboda, T. W. Jones, Frederick Reines, and C. B. Bratton

Subjects
Nuclear physics, Physics, Muon, Energy distribution, Solar neutrino, General Physics and Astronomy, Measurements of neutrino speed, Solar neutrino problem, Neutrino, Space radiation, Neutrino oscillation
Abstract

On a etudie la distribution de 135 evenements de neutrinos collectes durant 420 jours sous terre. Leurs longueurs des parcours etaient de quelques kilometres a 10 4 km. Leur energie moyenne: 920 MeV. On n'observe pas d'oscillations

Published
1985

63. Neutrino instability

Author

Henry W. Sobel, Frederick Reines, and Elaine Pasierb

Published
1981

64. Low Energy Neutrino Interactions

Author

Frederick Reines, Henry W. Sobel, and Elaine Pasierb

Subjects
Physics, Nuclear reaction, Particle physics, Physics::Instrumentation and Detectors, High Energy Physics::Phenomenology, Nuclear Theory, Elementary particle, Fermion, Massless particle, Pion, High Energy Physics::Experiment, Neutrino, Nuclear Experiment, Neutrino oscillation, Lepton
Abstract

This paper was intended to be a review of low energy neutrino interactions. However, in view of our. recently reported deuteron results, we have been requested to concentrate on them. To this end, we comment briefly on pion factory neutrino experiments and then discuss reactor neutrino work and, at greater length, the deuteron experiment.

Published
1982

65. Underground search for muons correlated with Cygnus X-3

Author

D. Kielczewska, D. Sinclair, D. Casper, L. R. Price, J. Schulz, Todd Haines, Stephen T. Dye, M. Goldhaber, Geoffrey Blewitt, R. Svoboda, R. Claus, Alessandra Ciocio, J. L. Stone, J. C. van der Velde, Henry W. Sobel, Sally Seidel, Geoff Thornton, R. M. Bionta, W. R. Kropp, C. B. Bratton, G. W. Foster, Lawrence Sulak, Frederick Reines, John Matthews, C. Wuest, E. Shumard, W. Gajewski, T. W. Jones, M. Crouch, S. Errede, John G. Learned, John M. LoSecco, H. S. Park, and K. S. Ganezer

Subjects
Physics, Radiation flux, Muon, Detector, Phase (waves), Flux, Cosmic ray, Astrophysics, Particle detector, Lepton
Abstract

We have examined muon data collected with the IMB (Irvine-Michigan-Brookhaven) proton-decay detector in search of a muon flux associated with the x-ray binary Cygnus X-3. A sample of 3.6 x 10/sup 4/ muons from the direction of Cygnus X-3 during the period September 1982 until April 1984 shows no evidence of its characteristic 4.8-h periodicity. In the phase interval 0.65 to 0.90 where a signal has been reported by other workers at a similar depth we obtain a 90%-confidence-level limit to the flux of 6.9 x 10/sup -11/ cm/sup -2/sec/sup -1/ for a depth of 1800 m water equivalent. This limit does not conflict with the reported signal. Three subsets of the data taken during Cygnus X-3 radio bursts have been separately analyzed. We find some evidence for an excess in the phase interval 0.50--0.60 at the time of the October 1983 outburst. We examine this excess in detail.

Published
1987

66. Physics Potentials with the Second Hyper-Kamiokande Detector in Korea

Author

Seong Chan Park, D.H. Moon, V. Paolone, W. Y. Ma, H. J. Kim, A. Mitra, M. Vagins, F. d. M. Blaszczyk, B. Quilain, A. Korzenev, Tracey Berry, A. Konaka, Hiromasa Tanaka, Carsten Rott, C. Mariani, T. Ovsiannikova, Kohta Murase, L. Berns, Y. Seiya, M. Posiadala-Zezula, A. Aimi, H.A. Tanaka, S. Molina Sedgwick, P. Ko, Jan T. Sobczyk, Monojit Ghosh, N. W. Prouse, Kimihiro Okumura, Y. Oh, H. K. Tanaka, A. Longhin, B. Richards, M. G. Catanesi, M. Buizza Avanzini, B. Jamieson, S. Nakayama, W. R. Kropp, Y. Suda, R. A. Wendell, Vincenzo Berardi, Etam Noah, J. Lagoda, B. G. Cheon, C. Kachulis, L. L. Kormos, Masaki Ishitsuka, A. Takenaka, J. F. Martin, M. Tzanov, C. J. Metelko, T. Yoshida, Hang Bae Kim, S. W. Kim, James R. Wilson, J. D. Perkin, Y. Fukuda, S. Parsa, S. Hirota, M. Mezzetto, M. M. Khabibullin, K. S. Ganezer, S. Short, P. Beltrame, Alexander Finch, K. Choi, A. Cole, M. Yu, J. M. Poutissou, C. Bronner, S. Jeon, Alan Cosimo Ruggeri, T. Dealtry, T. Xin, C. Simpson, Myung-Ki Cheoun, Dongsu Ryu, T. Feusels, S.H. Seo, W. Kim, J. C. Park, J. G. Learned, Myeong-Gu Park, Yoshinari Hayato, Giovanni Fiorentini, E. Mazzucato, Makoto Sakuda, C. H. Lee, A. Minamino, M. McCarthy, Hiroyuki Sekiya, Patrick Dunne, D. Sgalaberna, T. Yano, M. Taani, R. Terri, K. Zaremba, R. Shah, Oleg Mineev, J. S. Jang, C. Yanagisawa, R. Akutsu, R. Tacik, D. Fukuda, J. Yoo, K. Frankiewicz, S.Y. Kim, D. R. Hadley, T. Ishida, Jocelyn Monroe, G. Vasseur, M. Thiesse, K. Iwamoto, O. Drapier, M. Bergevin, S. D. Rountree, Jung-Hyun Kim, Atsushi Takeda, C. Riccio, F. Retiere, M. Malek, Francesco Muto, G. De Rosa, R. A. Owen, M. Ziembicki, E. Rondio, N. McCauley, C. M. Nantais, V. Palladino, L. O'Sullivan, H. Seo, Kyujin Kwak, S. C. Kim, Intae Yu, Gareth J. Barker, S. B. Kim, J. H. Choi, J. L. Palomino, G. Fiorillo, D. C. Son, J. Zalipska, J. Insler, S. V. Cao, Masahiro Kuze, Kendall Mahn, F. Nova, J. Y. Kim, Y. Takeuchi, M. Ikeda, A. C. Kaboth, S. B. Boyd, S. C. Yoon, T. Towstego, Y. Ashida, C. S. Moon, L. Labarga, J. Kameda, A. Evangelisti, L. H. V. Anthony, S. W. K. Emery, Yutaka Nakajima, K. Y. Choi, V. Aushev, Mcd Sanchez, P. Przewlocki, P. Lasorak, S. Berkman, D. N. Yeum, M. Miura, T. Nicholls, Michael Thorpe, A. Shaikhiev, R. G. Calland, I. M. Anghel, G. A. Cowan, Philippe Mermod, Ara Ioannisian, Yoshihiro Suzuki, H. S. Park, B. A. Popov, E. J. Chun, Brandon L. Hartfiel, J. P. Coleman, C. Checchia, Weonjong Lee, Hyper-Kamiokande proto-collaboration, K. K. Joo, Akimichi Taketa, A. Esmaili, S. Zsoldos, E. Won, Yuichi Oyama, S. L. Cartwright, S. Matsuno, Lester D.R. Thompson, R. A. Intonti, A. Izmaylov, Hiroshi Nunokawa, T. Lou, M. Lawe, Z. Chen-Wishart, R. P. Litchfield, M. Gonin, Y. Kataoka, Shih-Chang Lee, Masayuki Nakahata, C. Pidcott, R. B. Vogelaar, Enrique Fernandez-Martinez, L. Maret, P. Gumplinger, Hiroaki Aihara, P. N. Ratoff, Toru Iijima, J. L. Stone, M. Quinto, S. Yen, Ke. Abe, Yusuke Koshio, Y. Uchida, K. Abe, Kunio Inoue, R. J. Wilkes, K. S. Jeong, T. Kutter, E. H. Kwon, K. Kowalik, Y. Okajima, Teppei Katori, A. Pritchard, Roberto Spina, Koji Nakamura, A. N. Khotjantsev, C. Vilela, C. S. Kim, Takaaki Kajita, V. Takhistov, W. Parker, D. Dewhurst, J. Imber, S. Moriyama, Y. Fujii, S. Bolognesi, F. Cafagna, M. Friend, Janusz Marzec, J. Dumarchez, Marco Laveder, M. B. Smy, L. Cremonesi, Masato Shiozawa, Martin Ward, K. Kayrapetyan, H. J. Rose, M. Antonova, Ll. Marti, Henry W. Sobel, M. Fitton, D. Bravo-Bergu no, S. Bhadra, Y. Nishimura, T. S. Yoon, T. Mochizuki, H. D. Yoo, I. T. Lim, S. H. Ahn, A. Suzuki, Masashi Yokoyama, R. Svoboda, Gus Sinnis, Erin O'Sullivan, J. Walker, A. Mefodiev, L. Ludovici, Tsuyoshi Nakaya, C. Touramanis, M. Jiang, A. K. Ichikawa, J. Walding, E. S. Pinzon Guerra, Th. A. Mueller, P. Mijakowski, Kalen Martens, M. Needham, N. Yershov, H. M. O'Keeffe, M. O. Wascko, D. Payne, Kevin Scott McFarland, E. Kearns, Takashi Kobayashi, E. Drakopoulou, M. Barbi, Osamu Yasuda, M. Hartz, I. Shimizu, Yu. Onishchuk, R. Sacco, A. C. Weber, Hirokazu Ishino, J.-S. Kim, C. McGrew, T. Lindner, C. Andreopoulos, Michal Dziewiecki, K. Cho, Kazuhiro Yamamoto, S. Playfer, G.D. Barr, Y. Obayashi, C. Densham, S. King, S. W. Snow, S. Tobayama, N. Grant, F. Di Lodovico, G. Collazuol, Mark Scott, F. Muheim, Yu. G. Kudenko, A. Rychter, S. Mine, Todd D. Stewart, L. Magaletti, C. Giganti, M. J. Wilking, J. A. Nowak, M. Zito, K. M. Tsui, Hisakazu Minakata, Sin Kyu Kang, K. Hayrapetyan, T. Tsukamoto, T. Sekiguchi, H. I. Jang, M. Koga, Shunsaku Horiuchi, P. F. Loverre, E. Scantamburlo, R.P. Kurjata, J. Migenda, Y. Sonoda, A. Bravar, T. J. Kim, Yoshitaka Itow, P. Jonsson, G. Pronost, E. Radicioni, Y. Shitov, Yudai Suwa, John Hill, D. L. Wark, M. Y. Pac, A. Blondel, Yuji Kishimoto, Y. D. Oh, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Hyper-Kamiokande, Science and Technology Facilities Council (STFC), Blondel, Alain, Bravar, Alessandro, Korzenev, Alexander, Maret, Lucie, Mermod, Philippe, Noah Messomo, Etam Albert, Parsa, Saba, Scantamburlo, Enrico, Sgalaberna, Davide, Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Abe, K., Abe, Ke, Ahn, S. H., Aihara, H., Aimi, A., Akutsu, R., Andreopoulos, C., Anghel, I., Anthony, L. H. V., Antonova, M., Ashida, Y., Aushev, V., Barbi, M., Barker, G. J., Barr, G., Beltrame, P., Berardi, V., Bergevin, M., Berkman, S., Berns, L., Berry, T., Bhadra, S., Blaszczyk, F. D. M., Blondel, A., Bolognesi, S., Boyd, S. B., Bravar, A., Bronner, C., Buizza Avanzini, M., Cafagna, F. S., Calland, R., Cao, S., Cartwright, S. L., Catanesi, M. G., Checchia, C., Chen-Wishart, Z., Cheon, B. G., Cheoun, M. K., Cho, K., Choi, J. H., Choi, K., Choi, K. Y., Chun, E. J., Cole, A., Coleman, J., Collazuol, G., Cowan, G., Cremonesi, Cristina, Dealtry, T., De Rosa, G., Densham, C., Dewhurst, D., Drakopoulou, E., Di Lodovico, F., Drapier, O., Dumarchez, J., Dunne, P., Dziewiecki, M., Di Cicco, Emery, Esmaili, A., Evangelisti, A., Fernández-Martinez, E., Feusels, T., Finch, A., Fiorentini, G. A., Fiorillo, G., Fitton, M., Frankiewicz, K., Friend, M., Fujii, Y., Fukuda, Y., Fukuda, D., Ganezer, K., Ghosh, M., Giganti, C., Gonin, M., Grant, N., Gumplinger, P., Hadley, D. R., Hartfiel, B., Hartz, M., Hayato, Y., Hayrapetyan, K., Hill, J., Hirota, S., Horiuchi, S., Ichikawa, A. K., Iijima, T., Ikeda, M., Imber, J., Inoue, K., Insler, J., Intonti, R. A., Ioannisian, A., Ishida, T., Ishino, H., Ishitsuka, M., Itow, Y., Iwamoto, K., Izmaylov, A., Jamieson, B., Jang, H. I., Jang, J. S., Jeon, S. H., Jeong, K. S., Jiang, M., Jonsson, P., Joo, K. K., Kaboth, A., Kachulis, C., Kajita, T., Kang, S. K., Kameda, J., Kataoka, Y., Katori, T., Kayrapetyan, K., Kearns, E., Khabibullin, M., Khotjantsev, A., Kim, C. S., Kim, H. B., Kim, H. J., Kim, J. H., Kim, J. -S., Kim, J. Y., Kim, S. B., Kim, S. C., Kim, S. -W., Kim, S. Y., Kim, T. J., Kim, W., King, S., Kishimoto, Y., Ko, P., Kobayashi, T., Koga, M., Konaka, A., Kormos, L. L., Koshio, Y., Korzenev, A., Kowalik, K. L., Kropp, W. R., Kudenko, Y., Kurjata, R., Kutter, T., Kuze, M., Kwak, K., Kwon, E. H., Labarga, L., Lagoda, J., Lasorak, P. J. J., Laveder, M., Lawe, M., Learned, J. G., Lee, C. H., Lee, S. J., Lee, W. J., Lim, I. T., Lindner, T., Litchfield, R. P., Longhin, A., Loverre, P., Lou, T., Ludovici, L., Ma, W., Magaletti, L., Mahn, K., Malek, M., Maret, L., Mariani, C., Martens, K., Marti, L., Martin, J. F., Marzec, J., Matsuno, S., Mazzucato, E., Mccarthy, M., Mccauley, N., Mcfarland, K. S., Mcgrew, C., Mefodiev, A., Mermod, P., Metelko, C., Mezzetto, M., Migenda, J., Mijakowski, P., Minakata, H., Minamino, A., Mine, S., Mineev, O., Mitra, A., Miura, M., Mochizuki, T., Monroe, J., Moon, C. S., Moon, D. H., Moriyama, S., Mueller, T., Muheim, F., Murase, K., Muto, F., Nakahata, M., Nakajima, Y., Nakamura, K., Nakaya, T., Nakayama, S., Nantais, C., Needham, M., Nicholls, T., Nishimura, Y., Noah, E., Nova, F., Nowak, J., Nunokawa, H., Obayashi, Y., Oh, Y. D., Oh, Y., O'Keeffe, H. M., Okajima, Y., Okumura, K., Onishchuk, Yu., O'Sullivan, E., O'Sullivan, L., Ovsiannikova, T., Owen, R. A., Oyama, Y., Pérez, J., Pac, M. Y., Palladino, V., Palomino, J. L., Paolone, V., Park, H. S., Park, J. C., Park, M. G., Parker, W., Park, S. C., Parsa, S., Payne, D., Perkin, J. D., Pidcott, C., Pinzon Guerra, E., Playfer, S., Popov, B., Posiadala-Zezula, M., Poutissou, J. -M., Pritchard, A., Prouse, N. W., Pronost, G., Przewlocki, P., Quilain, B., Quinto, M., Radicioni, E., Ratoff, P. N., Retiere, F., Riccio, C., Richards, B., Rondio, E., Rose, H. J., Rott, C., Rountree, S. D., Ruggeri, A. C., Rychter, A., Ryu, D., Sacco, R., Sakuda, M., Sanchez, M. C., Scantamburlo, E., Scott, M., Molina Sedgwick, S., Seiya, Y., Sekiguchi, T., Sekiya, H., Seo, H., Seo, S. H., Sgalaberna, D., Shah, R., Shaikhiev, A., Shimizu, I., Shiozawa, M., Shitov, Y., Short, S., Simpson, C., Sinnis, G., Smy, M. B., Snow, S., Sobczyk, J., Sobel, H. W., Son, D. C., Sonoda, Y., Spina, R., Stewart, T., Stone, J. L., Suda, Y., Suwa, Y., Suzuki, Y., Suzuki, A. T., Svoboda, R., Taani, M., Tacik, R., Takeda, A., Takenaka, A., Taketa, A., Takeuchi, Y., Takhistov, V., Tanaka, H. A., Tanaka, H. K. M., Tanaka, H., Terri, R., Thiesse, M., Thompson, L. F., Thorpe, M., Tobayama, S., Touramanis, C., Towstego, T., Tsukamoto, T., Tsui, K. M., Tzanov, M., Uchida, Y., Vagins, M. R., Vasseur, G., Vilela, C., Vogelaar, R. B., Walding, J., Walker, J., Ward, M., Wark, D., Wascko, M. O., Weber, A., Wendell, R., Wilkes, R. J., Wilking, M. J., Wilson, J. R., Won, E., Xin, T., Yamamoto, K., Yanagisawa, C., Yano, T., Yasuda, O., Yen, S., Yershov, N., Yeum, D. N., Yokoyama, M., Yoo, H. D., Yoo, J., Yoon, S. C., Yoon, T. S., Yoshida, T., Yu, I., Yu, M., Zalipska, J., Zaremba, K., Ziembicki, M., Zito, M., Zsoldos, S., and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics - Instrumentation and Detectors, neutrino: solar, Physics::Instrumentation and Detectors, General Physics and Astronomy, KAMIOKANDE, 01 natural sciences, 7. Clean energy, C03, C04, C12, C32, C43, Physics and Astronomy (all), High Energy Physics - Experiment, Physics, Particles & Fields, MUSIC, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), site, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], neutrino: supernova, neutrino: mass, physics.ins-det, neutrino: interaction, energy: low, Physics, SPECTROSCOPY, J-PARC Lab, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, hep-ph, Computer Science::Computation and Language (Computational Linguistics and Natural Language and Speech Processing), Instrumentation and Detectors (physics.ins-det), LINE-EXPERIMENT-SIMULATOR, High Energy Physics - Phenomenology, Supernova, C04 Neutrino masses, Physical Sciences, SIMULATION, CP violation, CP VIOLATION, Neutrino, C03 CP violation, Physics::Physics and Society, Particle physics, and oscillations, Astrophysics::High Energy Astrophysical Phenomena, Physics, Multidisciplinary, NEUTRINO OSCILLATION EXPERIMENTS, CODE, FOS: Physical sciences, ddc:500.2, Neutrino beam, Computer Science::Digital Libraries, C12 Grand unified theories, dark matter, 0103 physical sciences, CP: violation, EARTH, mixing, Sensitivity (control systems), [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Neutrino oscillation, Science & Technology, hep-ex, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, sensitivity, C32 Experiments using neutrino beams, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Physics::Accelerator Physics, High Energy Physics::Experiment, C43 Underground experiments, MATTER, experimental results
Abstract

Hyper-Kamiokande consists of two identical water-Cherenkov detectors of total 520~kt with the first one in Japan at 295~km from the J-PARC neutrino beam with 2.5$^{\textrm{o}}$ Off-Axis Angles (OAAs), and the second one possibly in Korea in a later stage. Having the second detector in Korea would benefit almost all areas of neutrino oscillation physics mainly due to longer baselines. There are several candidate sites in Korea with baselines of 1,000$\sim$1,300~km and OAAs of 1$^{\textrm{o}}$$\sim$3$^{\textrm{o}}$. We conducted sensitivity studies on neutrino oscillation physics for a second detector, either in Japan (JD $\times$ 2) or Korea (JD + KD) and compared the results with a single detector in Japan. Leptonic CP violation sensitivity is improved especially when the CP is non-maximally violated. The larger matter effect at Korean candidate sites significantly enhances sensitivities to non-standard interactions of neutrinos and mass ordering determination. Current studies indicate the best sensitivity is obtained at Mt. Bisul (1,088~km baseline, $1.3^\circ$ OAA). Thanks to a larger (1,000~m) overburden than the first detector site, clear improvements to sensitivities for solar and supernova relic neutrino searches are expected., Comment: 102 pages, 49 figures. Accepted by PTEP

67. Stability of the Neutrino

Author

Henry W. Sobel, H. S. Gurr, and Frederick Reines

Subjects
Physics, Particle physics, Solar neutrino, High Energy Physics::Phenomenology, General Physics and Astronomy, Solar neutrino problem, Lower limit, Nuclear physics, Decay length, High Energy Physics::Experiment, Neutrino, Fission reactor, Neutrino oscillation, Electron neutrino
Abstract

Limits of g ${10}^{5}$ astronomical units are set on the decay length of an electron antineutrino ${\overline{\ensuremath{\nu}}}_{e}$ via the process ${\overline{\ensuremath{\nu}}}_{e}\ensuremath{\rightarrow}{\ensuremath{\nu}}^{\ensuremath{'}}+\ensuremath{\gamma}$ for ${E}_{\ensuremath{\gamma}}$ in the range 0.1-0.5 MeV using the results from a well-shielded detector in the vicinity of a fission reactor. This mode of decay is therefore ruled out as a possible explanation for the paucity of solar neutrinos revealed by the experiment of Davis.

Published
1974

68. An upper limit on the flux of extraterrestrial neutrinos

Author

D. Kielczewska, T. W. Jones, Lawrence Sulak, W. R. Kropp, G. W. Foster, Geoff Thornton, P. Chrysicopoulou, D. Sinclair, J. L. Stone, R. Svoboda, Henry W. Sobel, C. B. Bratton, H. S. Park, Geoffrey Blewitt, Sally Seidel, M. Goldhaber, J. C. van der Velde, Alessandra Ciocio, R. Claus, John M. LoSecco, John G. Learned, Stephen T. Dye, Frederick Reines, John Matthews, B. G. Cortez, C. Wuest, R. M. Bionta, K. S. Ganezer, D. Casper, Todd Haines, S. Errede, E. Shumard, W. Gajewski, and J. Schultz

Subjects
Physics, Massless particle, Cosmic neutrino background, Radiation flux, Neutrino detector, Space and Planetary Science, Extraterrestrial life, Flux, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Neutrino
Published
1987

69. Search for Neutrinos in Super-Kamiokande Associated with the GW170817 Neutron-star Merger

Author

C. W. Walter, Masaki Ishitsuka, T. Hasegawa, S. Mine, T. Towstego, T. Nakadaira, K. S. Ganezer, A. Ali, R. A. Intonti, Hiroyuki Sekiya, H. Okazawa, S. Nakayama, Soo-Bong Kim, Yoshitaka Itow, A. Pritchard, S. Tobayama, M. Elnimr, Y. Okajima, J. G. Learned, A. Takenaka, K. Nakamura, Mark R. Vagins, P. Fernandez, K. M. Tsui, S. Molina Sedgwick, Ken Sakashita, W. R. Kropp, M. J. Wilking, K. Abe, J. F. Martin, G. Pronost, M. G. Catanesi, S. V. Cao, M. Gonin, C. Bronner, Y. Takeuchi, Y. Sonoda, E. Radicioni, E. Kearns, Yoshitaka Kuno, A. Minamino, E. O’Sullivan, J. Y. Kim, M. Miura, T. Sekiguchi, S. Hirota, M. O. Wascko, John Hill, Y. Fukuda, D. L. Wark, Makoto Hasegawa, L. Wan, Takashi Yoshida, Jl Stone, Y. Nakajima, M. Jiang, M. Murdoch, Yasuhiro Kishimoto, Ryosuke Akutsu, R. Tacik, D. Fukuda, C. Simpson, T. Ishida, J. L. Raaf, Takashi Kobayashi, Makoto Sakuda, F. Di Lodovico, Xiaoning Li, K. Ito, T. Yano, F. d. M. Blaszczyk, Volodymyr Takhistov, C. K. Jung, D. Hamabe, C. Kachulis, S. Tasaka, M. Mori, P. Weatherly, Y. Oyama, N. McCauley, C. M. Nantais, C. Viela, Kimihiro Okumura, B. Richards, K. E. Nakamura, Z. Li, J. L. Palomino, Y. Suda, J. Kameda, Yasuhiro Nishimura, Y. Kato, Lester D.R. Thompson, J. Amey, Yuuki Nakano, I. T. Lim, Henry W. Sobel, Kyoshi Nishijima, A. Kibayashi, C. Xu, A. Takeda, Shintaro Ito, T. Hayashino, Takaaki Kajita, Shigetaka Moriyama, M. Ikeda, H. A. Tanaka, B. Quilain, Luis Labarga, M. Koshiba, P. Mijakowski, A. Konaka, Hiromasa Tanaka, A. Cole, J. Imber, T. Tsukamoto, H. Nagata, K. Choi, T. Nakamura, Francesco Muto, G. De Rosa, R. G. Park, M. B. Smy, R. P. Litchfield, S. Locke, M. Friend, Masato Shiozawa, Y. Choi, Ll. Marti, K. Martens, K. Iyogi, W. Y. Ma, Th. A. Mueller, L. H. V. Anthony, J. S. Jang, J. Bian, Masahiro Kuze, S. Berkman, R. G. Calland, Yoshihiro Suzuki, R. A. Wendell, S. Chen, L. Ludovici, A. Suzuki, Masashi Yokoyama, S. Matsuno, T. Ishizuka, Tsuyoshi Nakaya, Yoshinari Hayato, T. Ishii, C. Yanagisawa, Kate Scholberg, M. Hartz, Hirokazu Ishino, G. Collazuol, M. Murase, K. Frankiewicz, A. Orii, Lawrence Sulak, Yusuke Koshio, G. Santucci, Masayuki Nakahata, Y. Uchida, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Super-Kamiokande, Abe, K., Bronner, C., Hayato, Y., Ikeda, M., Iyogi, K., Kameda, J., Kato, Y., Kishimoto, Y., Marti, Ll., Miura, M., Moriyama, S., Nakahata, M., Nakajima, Y., Nakano, Y., Nakayama, S., Orii, A., Pronost, G., Sekiya, H., Shiozawa, M., Sonoda, Y., Takeda, A., Takenaka, A., Tanaka, H., Tasaka, S., Yano, T., Akutsu, R., Kajita, T., Nishimura, Y., Okumura, K., Tsui, K. M., Labarga, L., Fernandez, P., Blaszczyk, F. D. M., Kachulis, C., Kearns, E., Raaf, J. L., Stone, J. L., Sulak, L. R., Berkman, S., Tobayama, S., Bian, J., Elnimr, M., Kropp, W. R., Locke, S., Mine, S., Weatherly, P., Smy, M. B., Sobel, H. W., Takhistov, V., Ganezer, K. S., Hill, J., Kim, J. Y., Lim, I. T., Park, R. G., Li, Z., O'Sullivan, E., Scholberg, K., Walter, C. W., Gonin, M., Imber, J., Mueller, Th. A., Ishizuka, T., Nakamura, T., Jang, J. S., Choi, K., Learned, J. G., Matsuno, S., Amey, J., Litchfield, R. P., Ma, W. Y., Uchida, Y., Wascko, M. O., Catanesi, M. G., Intonti, R. A., Radicioni, E., De Rosa, Gianfranca, Ali, A., Collazuol, G., Ludovici, L., Cao, S., Friend, M., Hasegawa, T., Ishida, T., Ishii, T., Kobayashi, T., Nakadaira, T., Nakamura, K., Oyama, Y., Sakashita, K., Sekiguchi, T., Tsukamoto, T., Abe, K. E., Hasegawa, M., Suzuki, A. T., Takeuchi, Y., Hayashino, T., Hirota, S., Jiang, M., Mori, M., Nakamura, K. E., Nakaya, T., Wendell, R. A., Anthony, L. H. V., Mccauley, N., Pritchard, A., Fukuda, Y., Itow, Y., Murase, M., Muto, F., Mijakowski, P., Frankiewicz, K., Jung, C. K., Li, X., Palomino, J. L., Santucci, G., Viela, C., Wilking, M. J., Yanagisawa, C., Fukuda, D., Ishino, H., Ito, S., Kibayashi, A., Koshio, Y., Nagata, H., Sakuda, M., Xu, C., Kuno, Y., Wark, D., Lodovico, F. Di, Richards, B., Sedgwick, S. Molina, Tacik, R., Kim, S. B., Cole, A., Thompson, L., Okazawa, H., Choi, Y., Ito, K., Nishijima, K., Koshiba, M., Suda, Y., Yokoyama, M., Calland, R. G., Hartz, M., Martens, K., Murdoch, M., Quilain, B., Simpson, C., Suzuki, Y., Vagins, M. R., Hamabe, D., Kuze, M., Okajima, Y., Yoshida, T., Ishitsuka, M., Martin, J. F., Nantais, C. M., Tanaka, H. A., Towstego, T., Konaka, A., Chen, S., Wan, L., Minamino, A., Science and Technology Facilities Council (STFC), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire Leprince-Ringuet ( LLR ), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -École polytechnique ( X ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
neutron star: binary, Physics::Instrumentation and Detectors, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], KAMIOKANDE, Kilonova, 01 natural sciences, neutrino, 010303 astronomy & astrophysics, gravitational wave, High Energy Astrophysical Phenomena (astro-ph.HE), CALIBRATION, astro-ph.HE, Physics, astroparticle physic, neutrinos, antineutrino, gravitational waves, astroparticle physics, Physical Sciences, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, astroparticle physics gravitational waves neutrinos, Astrophysics::High Energy Astrophysical Phenomena, energy spectrum, FOS: Physical sciences, Astronomy & Astrophysics, gamma ray: burst, gravitational radiation: direct detection, EVENTS, Nuclear physics, neutrino: energy, muon, 0103 physical sciences, 010306 general physics, DETECTOR, Astroparticle physics, Science & Technology, Muon, Gravitational wave, High Energy Physics::Phenomenology, gravitational radiation, Astronomy and Astrophysics, Astronomy and Astrophysic, 0201 Astronomical And Space Sciences, Neutron star, Space and Planetary Science, gravitational radiation: emission, High Energy Physics::Experiment, Gamma-ray burst, Super-Kamiokande, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We report the results of a neutrino search in Super-Kamiokande for coincident signals with the first detected gravitational wave produced by a binary neutron star merger, GW170817, which was followed by a short gamma-ray burst, GRB170817A, and a kilonova/macronova. We searched for coincident neutrino events in the range from 3.5 MeV to $\sim$100 PeV, in a time window $\pm$500 seconds around the gravitational wave detection time, as well as during a 14-day period after the detection. No significant neutrino signal was observed for either time window. We calculated 90% confidence level upper limits on the neutrino fluence for GW170817. From the upward-going-muon events in the energy region above 1.6 GeV, the neutrino fluence limit is $16.0^{+0.7}_{-0.6}$ ($21.3^{+1.1}_{-0.8}$) cm$^{-2}$ for muon neutrinos (muon antineutrinos), with an error range of $\pm5^{\circ}$ around the zenith angle of NGC4993, and the energy spectrum is under the assumption of an index of $-2$. The fluence limit for neutrino energies less than 100 MeV, for which the emission mechanism would be different than for higher-energy neutrinos, is also calculated. It is $6.6 \times 10^7$ cm$^{-2}$ for anti-electron neutrinos under the assumption of a Fermi-Dirac spectrum with average energy of 20 MeV., 8 pages, 4 figures

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70. Neutrinos And Other Matters: Selected Works Of Frederick Reines

Author

William R Kropp, Mildred M Moe, Linda Price, Jonas Schultz, Henry W Sobel, William R Kropp, Mildred M Moe, Linda Price, Jonas Schultz, and Henry W Sobel

Subjects
Neutrinos, Nuclear physics, Astrophysics
Abstract

This volume is a collection of the scientific papers of Frederick Reines. Its publication is to commemorate the 70th birthday, in 1988, of this distinguished scientist. The selected papers here cover many aspects of his work in neutrino physics, astrophysics and conservation law tests. They have been divided into logical groupings, each introduced by a leading authority in that field, who helps the reader to see the reprinted articles with a better historical and scientific perspective.

Published
1991

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