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The Kamiokande Solar Neutrino Experiment

Published online by Cambridge University Press:  12 April 2016

K. S. Hirata ,
T. Kajita ,
T. Kifune ,
K. Kihara ,
M. Nakahata ,
K. Nakamura ,
S. Ohara ,
N. Sato ,
Y. Suzuki  and
Y. Totsuka
...Show all authors
K. S. Hirata
Affiliation:
Institute for Cosmic Ray Research, University of Tokyo, Tanashi, Tokyo 188, Japan
T. Kajita
Affiliation:
Institute for Cosmic Ray Research, University of Tokyo, Tanashi, Tokyo 188, Japan
T. Kifune
Affiliation:
Institute for Cosmic Ray Research, University of Tokyo, Tanashi, Tokyo 188, Japan
K. Kihara
Affiliation:
Institute for Cosmic Ray Research, University of Tokyo, Tanashi, Tokyo 188, Japan
M. Nakahata
Affiliation:
Institute for Cosmic Ray Research, University of Tokyo, Tanashi, Tokyo 188, Japan
K. Nakamura
Affiliation:
Institute for Cosmic Ray Research, University of Tokyo, Tanashi, Tokyo 188, Japan
S. Ohara
Affiliation:
Institute for Cosmic Ray Research, University of Tokyo, Tanashi, Tokyo 188, Japan
N. Sato
Affiliation:
Institute for Cosmic Ray Research, University of Tokyo, Tanashi, Tokyo 188, Japan
Y. Suzuki
Affiliation:
Institute for Cosmic Ray Research, University of Tokyo, Tanashi, Tokyo 188, Japan
Y. Totsuka
Affiliation:
Institute for Cosmic Ray Research, University of Tokyo, Tanashi, Tokyo 188, Japan
Y. Yaginuma
Affiliation:
Institute for Cosmic Ray Research, University of Tokyo, Tanashi, Tokyo 188, Japan
M. Mori
Affiliation:
National Laboratory for High Energy Physics (KEK), Tsukuba, Ibaraki 305, Japan
Y. Oyama
Affiliation:
National Laboratory for High Energy Physics (KEK), Tsukuba, Ibaraki 305, Japan
A. Suzuki
Affiliation:
National Laboratory for High Energy Physics (KEK), Tsukuba, Ibaraki 305, Japan
K. Takahashi
Affiliation:
National Laboratory for High Energy Physics (KEK), Tsukuba, Ibaraki 305, Japan
H. Takei
Affiliation:
National Laboratory for High Energy Physics (KEK), Tsukuba, Ibaraki 305, Japan
T. Tanimori
Affiliation:
National Laboratory for High Energy Physics (KEK), Tsukuba, Ibaraki 305, Japan
M. Koshiba
Affiliation:
Tokai University, Shibuya, Tokyo 151, Japan
T. Suda
Affiliation:
Department of Physics, Kobe University, Kobe, Hyogo 657, Japan
T. Tajima
Affiliation:
Department of Physics, Kobe University, Kobe, Hyogo 657, Japan
K. Miyano
Affiliation:
Niigata University, Niigata, Niigata 950-21, Japan
H. Miyata
Affiliation:
Niigata University, Niigata, Niigata 950-21, Japan
M. Yamada
Affiliation:
Niigata University, Niigata, Niigata 950-21, Japan
Y. Fukuda
Affiliation:
Department of Physics, Osaka University, Toyonaka, Osaka 560, Japan
K. Kaneyuki
Affiliation:
Department of Physics, Osaka University, Toyonaka, Osaka 560, Japan
Y. Nagashima
Affiliation:
Department of Physics, Osaka University, Toyonaka, Osaka 560, Japan
M. Takita
Affiliation:
Department of Physics, Osaka University, Toyonaka, Osaka 560, Japan
E. W. Beier
Affiliation:
Department of Physics, University of Pennsylvania, Philadelphia PA 19104, U. S. A.
L. R. Feldscher
Affiliation:
Department of Physics, University of Pennsylvania, Philadelphia PA 19104, U. S. A.
E. D. Frank
Affiliation:
Department of Physics, University of Pennsylvania, Philadelphia PA 19104, U. S. A.
W. Frati
Affiliation:
Department of Physics, University of Pennsylvania, Philadelphia PA 19104, U. S. A.
S.B. Kim
Affiliation:
Department of Physics, University of Pennsylvania, Philadelphia PA 19104, U. S. A.
A. K. Mann
Affiliation:
Department of Physics, University of Pennsylvania, Philadelphia PA 19104, U. S. A.
F.M. Newcomer
Affiliation:
Department of Physics, University of Pennsylvania, Philadelphia PA 19104, U. S. A.
R Van Berg
Affiliation:
Department of Physics, University of Pennsylvania, Philadelphia PA 19104, U. S. A.
W. Zhang
Affiliation:
Department of Physics, University of Pennsylvania, Philadelphia PA 19104, U. S. A.

Abstract

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The observation of 8B solar Neutrinos in the Kamiokande-II detector is presented. Based on 450 days of data in the time period of January 1987 through May 1988, the measured flux obtained with Ee ≥ 9.3 MeV was 0.46 ± 0.13 (stat) ± 0.08 (sys) of the value predicted by the standard solar model. The detector and analysis methods were improved since June 1988 and the background level has been decreased by a factor of about three since then.

Type
Part 2: Neutrinos
Information
International Astronomical Union Colloquium , Volume 121: Inside the Sun , 1990 , pp. 179 - 186
Copyright
Copyright © Kluwer 1990

References

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