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

初级宇宙线恒星日变化及太阳耀斑粒子加速机制研究

• 批准号: 11640287
• 负责人: KAWAKAMI Saburo
• 金额: $ 2.24万
• 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: 1999
• 资助国家: 日本
• 起止时间: 1999 至 2000
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-11640287/
• 关键词: Primary Cosmic Rays; Modulation; Sidereal variation; Solar time variation; Interstellar magnetic field

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

巨大的μ子探测器由16个独立的单元组成，于1997年底在印度南部的Ooty新建。它的总基准面积约为560 m^2。它可以探测到1GeV以上的宇宙射线介子能量。计数率每一秒记录一次。这是世界上最大的用于调制测量的μ子探测器。这些探测器已经被修改，使每10秒使用这个格兰特在Aide测量单个μ子的角度。我们希望研究100 GeV以上初级宇宙射线的恒星变化、行星际磁场结构和高能太阳耀斑产生的等离子体激波锋。在这个时刻，所有16个单位（560 m^2）的角度测量都是可操作的，观测正在进行中。到目前为止，我们已经分析了这些数据的一部分，可以确认我们的μ子探测器的性能是相当成功的。以下是最近观察得出的一些结果。我们分析了太阳日变化，在13.5小时（当地时间）方向检测到峰值，振幅约为0.4%。这可以通过所谓的扩散-对流模型和地球磁场的影响来很好地理解。我们对数据进行了IMF方向分类分析，通过Swinsson缺陷（约0.15%）可以观察到恒星的变化。这主要是由于宇宙射线密度的径向不对称造成的。恒星日变化有两种异常，一种是损失玉米的亏缺，另一种是尾效应的过剩。这些振幅约为0.1%。由于我们的探测器位于赤道附近，我们可以同时得到这两个异常。我们一直在继续分析角度测量的新数据。我们已完成1998年4月至2000年3月的总计数分析。我们意识到1998年的数据集和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。同时分析了forbushreduction的时间和角度轮廓。我们想继续我们目前的观察和积累数据。少

项目成果

S.Kawakami, Y.Hayashi, N.Ito et al.: "Observation of Cosmic ray modulation and possible detection of the solar flares with GRAPES III muon telescope at Ooty"Proc. of 26th Int.Cosmic Ray Conf.. Vol.4. 275-278 (1999)

S.Kawakami、Y.Hayashi、N.Ito 等人：“乌蒂的 GRAPES III 介子望远镜对宇宙射线调制的观测和太阳耀斑的可能检测”Proc。

T.Nishiyama et al.: "Detection of a new TeV gamma ray source of BLLac object IESI959-650"Proc. of 26th Int.Cosmic Ray Conf.. Vol.3. 370-373 (1999)

T.Nishiyama 等人：“BLLac 物体 IESI959-650 的新 TeV 伽马射线源的检测”Proc。

Y. Hayashi et al.: "The size spectrum of small Air Showers at Ooty GRAPES III(800g/cm2)"Proc. of 26th Int. Cosmic Ray Conf.. V1. 236-239 (1999)

Y. Hayashi 等人：“Ooty GRAPES III 小型空气阵雨的尺寸范围（800g/cm2）”Proc。

Y. Hayashi et al.: "A study on the lateral structure of Muons in Extensive Air Showers with the GRAPES III array at Ooty"Proc. of 26th Int. Cosmic Ray Conf.. V1. 276-279 (1999)

Y. Hayashi 等人：“利用 Ooty 的 GRAPES III 阵列对大范围空气阵雨中 Mu 子的横向结构进行研究”Proc。

T. Nishiyama et al.: "Detection of a new TeV gamma ray source of BLLac object 1ES1959+650"Proc. of 26th Int. Cosmic Ray Conf.. V3. 370-373 (1999)

T. Nishiyama 等人：“BLLac 物体 1ES1959 650 的新 TeV 伽马射线源的检测”Proc.