A search for Cosmic High Energy Neutron

寻找宇宙高能中子

• 批准号: 04402003
• 负责人: TESHIMA Masahiro
• 金额: $ 24.19万
• 依托单位: University of Tokyo
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for General Scientific Research (A)
• 财政年份: 1992
• 资助国家: 日本
• 起止时间: 1992 至 1994
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-04402003/
• 关键词: Cosmic Ray; Neutron; Air Shower; High Energy Astrophsics; Cerenkov Light; Scintillation Light; 中性子; シンチレーション; 光電子増倍管; 天体物理; ガンマ線; 高エネルギー物理; マルチアノード光電子増倍管; 望遠鏡; 宇宙; 空気シンチレーション光; 反射望遠鏡; 粒子加速

The high resolution cosmic ray detector using optical tequniques were developped to search for high energy cosmic neutrons.The high resolution camera consisiting of eight multi anode photomultipliers of 512 pixels, and the data aquisition electronics were made. It was mounted on the fucul plane of the fixed directional mirror systems provided by University of Utah. The telesope was directed at elevation angle of 19ﾟ to get the best sensitivity for the high energy cosmic rays. The observation were carried out for -100hrs.The monitoring system with Nd : YAG laser were operated by the collaborators of University of Utah. Using this system, we could calibrate our detector and monitor the atmospheric condition.With 100hr observation, we have detected 100 cosmic ray shower images. Among them, 10 shower images were identified as showers with energy of greater than 3*10^<18>eV,and with the impact parameter of 10Km-30Km from detector. Through the data anlaysis, we have demonstrated that the geometry of the shower detector plane can be determined with an acuracy of -0.03ﾟ. This angular resolution is much better than the resolution achieved so far. We have established the experimental method to detect cosmic rays with the high accuracy.

开发了使用光学电视的高分辨率宇宙射线检测器来寻找高能量宇宙中子。八个具有512像素的多阳极光层次的高分辨率摄像头共同组合，并制作了数据育种电子设备。它安装在犹他大学提供的固定定向镜像系统的福克尔平面上。望远镜的指向19 ﾟ的高度角度，以获得对高能量宇宙射线的最佳灵敏度。进行了-100小时的观察。使用ND：YAG激光器的监测系统由犹他大学的合作者运营。使用该系统，我们可以校准检测器并监测大气条件。通过观察100小时，我们检测到100个宇宙射线淋浴图像。其中，将10个淋浴图像鉴定为能量大于3*10^<18> eV的阵雨，并且距离检测器的冲击参数为10km-30km。通过数据anlaysis，我们证明了淋浴检测器平面的几何形状可以用-0.03 ﾟ的精算师确定。该角度分辨率比到目前为止达到的分辨率要好得多。我们已经建立了以高精度检测宇宙射线的实验方法。

项目成果

M.Nagano et al.: "Energy Spectrum of Primary Cosmic RayS above 10X^<17>eV Determined from The Extensive Air Shower Experiment at Akeno," J.Phys.G:Nucl.Phys.18. 423-442 (1992)

M.Nagano等人：“根据Akeno的广泛空气簇射实验确定的10X^ 17 eV以上的初级宇宙射线能量谱”，J.Phys.G：Nucl.Phys.18。

N.Chiba et.al.: "Akeno Giant Air Shower Array(AGASA)covering 100kmX^2 area," Nucl.Inst.and Meth.A311. 338-349 (1992)

N.Chiba 等人：“覆盖 100kmX^2 区域的 Akeno 巨型空气簇射阵列 (AGASA)”，Nucl.Inst.and Meth.A311。

N.Chiba et al.: "Possible Evidence for ≧ 10GeV Neutrons Associated with The Solar Flare of 4 June 1991," Astroparticle Phys.1. 27-32 (1992)

N.Chiba 等人：“与 1991 年 6 月 4 日太阳耀斑相关的 ≧ 10GeV 中子的可能证据”，Astroarticle Phys.1 (1992)。

Yoshida et al.: "The Cosmic Ray Energy Spectrum above3×10^<18>eV by the Akeno Giant Air Shower Array" to be published in Astroparitcle Physics. (1995)

Yoshida 等人：“The Cosmic Ray Energy Spectrum above3×10^<18>eV by the Akeno Giant Air Shower Array”将发表在 Astroparitcle Chemistry (1995) 上。

N.Hayashida et al.: "The Observation of a Very Energetic Cosmic Ray well beyond the Predicted 2.7K Cutoff in the Primary Energy Spectrum" Phys.Rev.Letters. 73. 3491-3494 (1994)

N.Hayashida 等人：“观测到高能宇宙射线远远超出主能谱预测的 2.7K 截止值”Phys.Rev.Letters。