Detection of High Energy Cosmic Neutrino in the Deep Ocean

深海高能宇宙中微子的探测

• 批准号: 03044036
• 负责人: OHASHI Yozo
• 金额: $ 5.44万
• 依托单位: University of Tokyo
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for international Scientific Research
• 财政年份: 1991
• 资助国家: 日本
• 起止时间: 1991 至 1992
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-03044036/
• 关键词: Cosmic Neutrino; Deep Sea; Optical Detector; Bioluminescence; 宇宙ニュ-トリノ; 光電子増倍管

This research is an international project organized by scientists from Japan, USA and Europe, and Japanese group are responsible to prepare optical modules for the deep sea water Cerenkov detector. The international collaboration meeting is held four times a year, one of which was held in Japan in 1992. The schedule has been decided to start the construction of the detector off the Big Island of Hawaii from 1993 October.1). The components of the optical modules have been prepared for two strings. Characteristics of PMTs have been measured, the pattern of the circuit board was revised, and the software to control the circuit was changed to the universal OS-9. Running tests have been done with circuit boards in the temperature programmable chamber. Mechanical tests of the optical modules have been done by oscillating the sample module at *2g. The assembled modules have been sent to Ull, and calibrated there using a water tank.2). Workshop on High Energy Neutrino Astrophysics was held March 1992 at UH, Honolulu, where the expected energy spectrum and its flux of neutrinos originated from AGN was widely discussed. Following the above results the sensitivity of the DUMAND array to neutrinos from AGNs was simulated. Capability to detect cascades induced by HE neutrinos from AGN was examined. Sensitivity of the array to neutralino cold dark matter was also examined.3). Background light due to organisms was investigated using a highly sensitive video camera. Images of biolight were recorded at depths of 4500, 3500, and 2500m near DUMAND site and at depths of 5000, 4000 and 3000m off Ibosaki of the Japan Island. Light intensity largely fluctuates time to time, and its mean value decreases with the depth. Comparison of the data at both sites shows that the light intensity at DUMAND site is a factor of (*10) smaller.

这项研究是由日本，美国和欧洲的科学家组织的国际项目，以及日本集团负责为深海水Cerenkov探测器准备光学模块。国际合作会议每年举行四次，其中一次是在1992年在日本举行的。该时间表已决定于1993年10月1日开始在夏威夷大岛上建造探测器。光学模块的组件已经为两个字符串准备了。已经测量了PMT的特征，修改了电路板的模式，并将控制电路的软件更改为通用OS-9。在可编程室内的电路板上进行了运行测试。光学模块的机械测试是通过在 *2G处振荡样品模块来完成的。组装模块已发送到ULL，并使用水箱进行了校准。2）。关于高能中微子天体物理学的研讨会于1992年3月在檀香山的UH举行，在那里预期的能量谱及其源自AGN的中微子的通量进行了广泛讨论。遵循上述结果，模拟了杜非州阵列对中微子的敏感性。检查了从AGN中中微子诱导的级联反应的能力。还检查了阵列对中性寒冷暗物质的敏感性3）。使用高度敏感的摄像机研究了由于生物而引起的背景光。在日本岛的Ibosaki附近，在Dumand遗址附近的4500、3500和2500m的深度记录了生物亮的图像。光强度在很大程度上会不时波动，其平均值随深度的降低。两个站点上数据的比较表明，dumand位点的光强度为（*10）较小。

项目成果

K.KOBAYAKAWA et al.: "High Energy Particles by Shock Acceleration around Superconducting Cosmic Strings" Proc. of the workshop on High Energy Neutrino Astrophysics,Honolulu (March,1992). 141-150 (1992)

K.KOBAYAKAWA 等人：“超导宇宙弦周围冲击加速的高能粒子”Proc。

Hayashino et al.: "Neutralino Dark Matter Search with DUMAND" Proc. of the Inter. Symp. on Neutrino Astrophys.Takayama (Oct.1992), submitted. (1993)

Hayashino 等人：“使用 DUMAND 进行中性子暗物质搜索”Proc。

K.Kobayakawa et al.: "High Energy Particles by Shock Acceleration around Superconducting Cosmic String" Proc. of the Workshop on High Energy Neutrino Astrophys.,Honolulu (March, 1992). 141-150 (1992)

K.Kobayakawa 等人：“超导宇宙弦周围冲击加速的高能粒子”Proc。

K.KOBAYAKAWA et al.: "High Energy Neutrinos and Gamma-Rays from Superconducting Cosmic Strings in the Galaxy" Proc. of the International Symposium on Neutrino Astrophysics Takayama (Oct.1992). (1993)

K.KOBAYAKAWA 等人：“来自银河系超导宇宙弦的高能中微子和伽马射线”Proc。

K.Mitsui: "Muon Energy-loss distribution and its Applications to muon energy determination" Physcal Review. 45. 3051-3060 (1992)

K.Mitsui：“μ子能量损失分布及其在μ子能量测定中的应用”物理评论。