| Co-Investigator(Kenkyū-buntansha) |
ブガーエフ エドガー ロシア科学アカデミー, 原子核研究所, 上級研究員
パルフェーノフ ユーリ イルクーツク国立大学, 応用物理研究所, 所長
KIKUCHI Ryusaburo Kyoto University, Graduate School of Science, Research Associate, 理学研究科, 助手 (10025356)
MIYACHI Takashi University of Tokyo, Center for Nuclear Science, Research Associate, 原子核科学研究センター, 助手 (20013401)
KONISHI Eiichi Hirosaki University, Faculty of Science and Technology, Associate Professor, 理工学部, 助教授 (10113789)
YURI Parfenov Irkutsk State University, Applied Physics Institute, Director
EDGAR Bugaev Russian Academy of Sciences, Institute for Nuclear Research, Senior Researcher
エドガー ブガーエフ ロシア科学アカデミー原子核研究所, 上級研究員
ユーリ パルフェーノフ イルクーツク国立大学, 応用物理研究所, 所長
PANFILOV A. ロシア科学アカデミー原子核研究所, 研究員
BUGAEV E. ロシア科学アカデミー原子核研究所, 上級研究員
SINEGOVSKI S イルクーツク大学, 物理学科, 助教授
BEZRUKOV L. ロシア科学アカデミー原紙核研究所, 副所長
BUDNEV N. イルクーツク大学, 応用物理研究所, 助教授
POLITYKO S. イルクーツク大学, 物理学科, 助教授
長谷部 信行 愛媛大学, 工学部, 助教授 (10127904)
PARFENOV I. イルクーツク大学, 応用物理研究所, 所長
LAGOUTINE A. アルタイ大学, 物理学科, 教授
DEDENKO L. モスクワ大学, 物理学科, 教授
三井 清美 山梨学院大学, 経営情報学部, 助教授 (80013340)
藤井 正美 青森大学, 工学部, 教授 (20013691)
御法川 幸雄 近畿大学, 理学部, 教授 (90088500)
高橋 信介 弘前大学, 教養部, 助教授 (40216742)
河野 毅 理化学研究所, 副主任研究員 (60211231)
石渡 光正 埼玉大学, 理学部, 助教授 (80184571)
井上 直也 埼玉大学, 理学部, 助教授 (40168456)
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| Budget Amount *help |
¥17,600,000 (Direct Cost: ¥17,600,000)
Fiscal Year 1997: ¥8,800,000 (Direct Cost: ¥8,800,000)
Fiscal Year 1996: ¥8,800,000 (Direct Cost: ¥8,800,000)
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| Research Abstract |
In this program, we have planned to study various fundamental researches for extremely high energy neutrino astrophysics which has never existed as the brancn of science up to now. In our opinion, one of the biggest characteristics of extremely high energy neutrino astrophysics lies in to observe the universe, the existence of which is never observed by light1 but only by neutrino. The purpose of this program is to develop techniques and theoretical concepts by which such universe could be observed.
We are developing new types of high performance of photon counters based the semiconductor technique, namely counters with both local feed back type and superlattice types (Reference No.14), because the conventional type of photo-multipliers which have been extensively utilized in the Superkamiokande experiment have lost effectiveness in the extremely high energy neutrino astrophysics. Extremely high energy neutrino is detected by the measurement of the emitted Cherenkov radiation from both electron (in the case of electron neutrino) and muon (in the case of muonneutrino). As for electron, we investigated such electron showers in the plasma state (Re.No.1) these in strong magnetic field(Re.No.3) and the LPM effect problems (Re.No.8,9). As for muon, the influence of the heavy atom on the bremsstralilung (Re.no.13) and atmospheric muon problem (Re.No.18) are investigated. Also, the knowledge on the space-temporal structure is requested to detect neutrino(Re.No.10). On the other hand, experimental knowledge on high energy neutrino which is absolutely important for the understanding of behavior of extremely high energy neutrino is obtained (Re.No.5,6,7).
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