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

巨大的μ子探测器由16个独立的单元组成，从1999年开始在印度南部泰米尔纳德邦的Ooty全面投入使用。它的总有效面积约为560 m^2。它可以探测到能量在1GeV以上的宇宙射线介子，它们对应于~ 70GeV的银河宇宙射线。测量单个方向的记录设备是由以前的科学研究资助基金安装的。同时记录225个方向的计数率，每10秒一次。这是世界上最大的用于太阳耀斑和调制测量的介子探测器。本研究的目的是测量~ 70 GeV以上初级宇宙射线的恒星各向异性，以及高能太阳耀斑日冕物质抛射产生的行星际磁场和等离子体激波前的结构。我们在日本山梨县东京大学宇宙射线研究所秋野天文台新建了3台μ子望远镜（~ 75m^2），并与Ooty的GRAPES μ子望远镜进行了同步观测。在2004年7月30日，两台望远镜都观测到损耗锥型缺陷。这是首次用两个相距约7000公里的窄角μ子望远镜观测到Loss锥缺陷的前驱型。经过仔细的分析和计算，表明在这一时刻，与行星际磁场一起存在着瓶颈结构。我们分析了5年的数据，我们已经能够通过测量以下已经建立的各向异性，太阳时间各向异性（0.4%）宇宙射线，这是由所谓的扩散-对流模型和伪恒星时间各向异性，史文森流（0.15%）建立我们的μ子探测器的卓越性能。我们通过分析宇宙射线的恒星变化观察到所谓的尾向各向异性。振幅约为0.1%。这些结果发表在2005年8月在印度浦那举行的第29届国际宇宙射线会议上。少

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