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.

为了寻找高能宇宙中子，研制了利用光学技术的高分辨率宇宙线探测器，制作了由8个512象素的多阳极光电倍增管组成的高分辨率相机和数据采集电子学。它安装在犹他州大学提供的固定定向镜系统的焦平面上。望远镜的仰角为19 °，以获得对高能宇宙射线的最佳灵敏度。采用犹他州大学合作者研制的Nd：YAG激光监测系统，进行~ 100小时的监测。利用该系统，我们可以对探测器进行定标和大气监测，在100小时的观测中，我们已经探测到了100幅宇宙线簇射图像。其中10个簇射图像被识别为能量大于3*10^ eV的簇射<18>，并且来自探测器的撞击参数为10 Km-30 Km。通过数据分析，我们证明了簇射探测器平面的几何形状可以用-0.03 μ m的精度来确定。这个角度分辨率比迄今为止实现的分辨率好得多。建立了高精度探测宇宙线的实验方法。

项目成果

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。

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。

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.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)。

Honda et al.: "Inelastic Cross Section for P-Air Collisions from Air Shower Ex-periment and Total Cross Section for P-P Collisions up to √s=24Te" Phys.Rev.Lett.50. 2058-2061 (1993)

Honda 等人：“来自空气喷淋实验的 P-Air 碰撞的非弹性横截面和高达 √s=24Te 的 P-P 碰撞的总横截面”Phys.Rev.Lett.50 (1993)。