THE STUDY OF SOLAR FLARE AND ANISOTROPY OF GALACTIC COSMIC RAYS WITH LARGE MUON TELESCOPE

大型介子望远镜对太阳耀斑和银河宇宙线各向异性的研究

• 批准号: 14540276
• 负责人: KAWAKAMI SABURO
• 金额: $ 1.79万
• 依托单位: OSAKA CITY UNIVERSITY
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Scientific Research (C)
• 财政年份: 2002
• 资助国家: 日本
• 起止时间: 2002 至 2004
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-14540276/
• 关键词: 銀河宇宙線; モジュレーション; 太陽フレア; Coronal Mass Ejection; 惑星間磁場; 宇宙天気予報

Huge Muon detectors consists of 16 independent units have become fully operational from 1999 at Ooty, Tamil Nadu, South India. Its total effective area is about 560 m^2. It can detect the cosmic ray muons energy above 1GeV, they correspond to 〜70GeV galactic cosmic rays. The recording devices for measuring the individual directions are installed by previous Grant in Aid for Scientific Research. The counting rates for 225 directions are recorded simultaneously at every ten second. This is the largest muon detector in the world for the purpose of Solar flare and modulation measurement. The aim of present study is to measure the sidereal anisotropy of primary cosmic rays above 〜70 GeV and the structure of interplanetary magnetic field along with shock front of plasma created by energetic Solar flare's Coronal mass ejection.We have newly constructed three muon telescopes (〜75m^2) using present Grand in Aide at Akeno observatory of Institute for Cosmic Rays of Tokyo University in Yamanashi … More prefecture Japan and have started a simultaneous observation with Ooty's GRAPES muon telescopes.Loss cone type of defect was observed in both telescopes on 30^<th> July 2004. This is the first occasion that precursor type of Loss cone defect has been observed by two narrow angle muon telescope separated by about 7000 km. It turned out that there must have been bottle neck structure along with the Interplanetary Magnetic Field at this occasion by the careful analysis and calculation.We have analyzed the five years of data and we have been able to establish excellent performance of our muon detectors by measuring the following well established anisotropy, the Solar time anisotropy (0.4%) of cosmic rays which is expected by so called Diffusion -Convection Model and pseudo sidereal time anisotropy, Swinson flow (0.15%).We observed so called Tail-in anisotropy by analyzing the sidereal variation of cosmic rays. This amplitude was around 0.1%. Those results have been presented in the 29^<th> International cosmic rays conference held at Pune, India August 2005. Less

由 16 个独立单元组成的巨型 Muon 探测器从 1999 年起在印度南部泰米尔纳德邦的乌蒂全面投入运行。其总有效面积约为560 m^2。它可以探测能量在1GeV以上的宇宙线μ子，它们对应〜70GeV的银河宇宙线。用于测量各个方向的记录装置是由先前的科学研究援助拨款安装的。每十秒同时记录 225 个方向的计数率。这是世界上最大的用于太阳耀斑和调制测量的μ子探测器。本研究的目的是测量〜70 GeV以上的初级宇宙线的恒星各向异性以及行星际磁场的结构以及由高能太阳耀斑的日冕物质抛射产生的等离子体激波前部。我们使用东京宇宙线研究所明野天文台现有的Grand in Aide新建了三架μ子望远镜（〜75m^2） 日本山梨县大学开始与Ooty的GRAPES μ子望远镜进行同步观测。2004年7月30日，两台望远镜均观测到了损失锥型缺陷。这是首次由相隔约7000公里的两台窄角μ子望远镜观测到损失锥型缺陷。经过仔细的分析和计算，发现此时的行星际磁场肯定存在瓶颈结构。我们分析了五年的数据，通过测量以下已确立的各向异性，即所谓的扩散对流模型和伪恒星时所预期的宇宙线太阳时各向异性（0.4％），我们已经能够建立我们的μ子探测器的优异性能 各向异性，斯温森流（0.15%）。我们通过分析宇宙线的恒星变化观察到了所谓的尾部各向异性。该幅度约为0.1%。这些结果已在 2005 年 8 月在印度浦那举行的第 29 届国际宇宙射线会议上公布。 更少

项目成果

Upper Limit on the Diffuse Gamma Ray Flux Using Air Shower Observations at Ooty

使用乌提空气喷淋观测得出的漫射伽马射线通量上限

• 发表时间: 2003
• 期刊: Proc.of the 28^<th> Int.Cosmic Ray Conference (Tsukuba), 1
• 作者: Y.Hayashi;S.Kawakami et al.
• 通讯作者: S.Kawakami et al.

T.Yamamoto, S.Kawakami et al.: "Development of Atmospheric Monitoring System at Akeno Observatory for the Telescope Array Project"Nuclear Instruments and Methods in Physics Research. 488. 191-208 (2002)

T.Yamamoto、S.Kawakami 等人：“明野天文台望远镜阵列项目大气监测系统的开发”物理研究中的核仪器和方法。

The acceleration of cosmic-ray protons in the supernova remnant RX J1713.7–3946

• DOI: 10.1038/416823a
• 发表时间: 2002-04
• 期刊: Nature
• 影响因子: 64.8
• 作者: R. Enomoto;T. Tanimori;T. Naito;T. Yoshida;S. Yanagita;M. Mori;P. G. Edwards;A. Asahara;G. B

Solar cycle variations of modulation parameters of galactic cosmic-rays in the heliosphere

日光层银河宇宙线调制参数的太阳周期变化

• 发表时间: 2002
• 期刊: Advanced Space Research 29
• 作者: K.Munakata;K.Fujimoto et al.
• 通讯作者: K.Fujimoto et al.

K.Shinozaki, S.Kawakami et al.: "Upper limit on Gamma-ray Flux above 10^<19>eV Estimated by the Akeno Giant Air Shower Array Experiment"Astrophysical Journal. 571. 117-120 (2002)

K.Sinozaki、S.Kawakami等人：“Akeno巨型空气簇射阵列实验估计的10^ 19 eV以上伽马射线通量的上限”天体物理学杂志。