Study on sidereal daily variation of primary cosmic rays and particle acceleration mechanism in Solar flare

由16个独立单元组成的巨型Muon探测器已于1997年底在印度南部的Ooty新建。它的总基准面积约为560m^2。它可以探测1GeV以上的宇宙线µ子能量。每一秒记录一次计数率。这是世界上最大的以调制测量为目的的Muon探测器。这些探测器已经被改装，可以使用GRANT IN AIDE在每10秒内测量单个介子的角度。我们希望研究100GeV以上初级宇宙线的恒星变化、行星际磁场结构和太阳高能耀斑产生的等离子体激波锋。目前，所有16个单元(560米^2)的角度测量都已开始运行，观测正在进行中。到目前为止，我们已经分析了部分数据，可以确认我们的Muon探测器的性能是相当成功的。以下是最新观察的一些结果1。我们已经对太阳能…进行了分析日变化较大，峰值出现在13.5小时方向(当地时间)，波幅约为0.4%。这可以用所谓的扩散-对流模型和地球磁场的影响来很好地解释。我们通过对IMF方向的分类来分析数据，可以观察到Swinsson缺陷(约0.15%)的恒星变化。这主要是由于宇宙线密度的径向不对称所致。3.恒星日变化存在两种异常，一种是损失的亏损，另一种是效应中的尾部过剩。这些幅度约为0.1%。由于我们的探测器位于赤道附近，我们可以同时获得这两个异常。我们一直在继续分析来自角度测量的新数据。到目前为止，我们已经完成了对1998年4月至2000年3月期间测量的总数的分析。我们发现1998年的数据集与1999年的数据集在这些恒星异常的位置上有大约2小时的差异。因此，造成这种差异的原因目前正在密切调查中。同时，我们还分析了福布什下降的时间分布和角度分布。我们想继续我们目前的观察，并积累数据。较少

Huge Muon detectors consists of 16 independent units have been newly constructed in Ooty, South India by 1997 end. Its total fiducial area is about 560 m^2. It can detect the cosmic ray muons energy above 1GeV.The counting rate is recorded at every one second. This is the largest muon detector in the world for the purpose of modulation measurement. These detectors have been modified to enable the angle measurement of individual muons in each 10 seconds using this Grant in Aide. We wish to study the sidereal variation on primary cosmic rays above 100 GeV, the structure of interplanetary magnetic field and shock front of plasma created by energetic Solar flare. At this moment angle measurement of all the 16 units (560 m^2) are operational and the observation is going on. We have analyzed part of these data so far and could confirm that the performance of our muon detectors is quite successful. The followings are some of the results from the latest observation.1. We have analyzed on solar … More daily variation and detected the peak at direction of 13.5 hour (Local Time) with amplitude of about 0.4%. This can be well understood by so called Diffusion-Convection Model and influence of the Earth's magnetic field.2. We analyzed the data by classifying IMF direction and could observe the sidereal variation by Swinsson Flaw (about 0.15%). This is mainly due to radial asymmetry of cosmic ray density.3.There were two anomalies in sidereal daily variation, one is the deficit by Loss corn and another is excess by Tail in effects. These amplitudes are about 0.1%. Since our detector is located near equator, we could get these two anomalies simultaneously.We have been continuing analysis on new data from angle measurements. We have completed the analysis of total counts measurements from April 1998 to March 2000 so far. We realized that there are about 2 hour difference between 1998 data set and 1999 data set in the position of these sidereal anomalies. So the cause of this discrepancy is under close investigation now. Same time we are analyzing the time and angular profile of Forbush Decrease. We would like to continue our present observation and accumulate the data. Less