Chemical composition and point source of high energy primary cosmic ray and sidereal time variation

我们在印度南部的Ooty制作了GRAPES-3空气簇射阵列，由约350个闪烁体探测器和1GeV能量阈值的大面积(560m^2)跟踪µ子探测器组成。利用奇偶方法和左向右方法这两种重要的方法，得到了GRAPES-3实验的角分辨率。将上述两种方法得到的结果与月亮和太阳阴影观测的结果进行了比较。对于&gt；80TeV，角分辨率为0.5°。我们观察到，在用‘零介子’和‘介子贫乏’标准选择的流星雨中出现了过剩的通量。这些观测产生了高于9TeV能量阈值的(5.08±2.67)×10^&lt；-13&gt；cm^&lt；-2&gt；s^&lt；-1&gt；积分通量和高于30TeV能量的(6.92±2.87)×10^&lt；-14&gt；cm^&lt；-2&gt；s^&lt；-1&gt；积分通量。这是第一次出现无模流星雨。我们测量了初级宇宙射线的成分和能谱。GRAPES-3实验包括用560m^2Muo…观测到的介子多重数分布的细节更多的n探测器作为来自分析的淋浴大小的函数。利用CORSIKA程序提供的一些强子相互作用产生器，将这些分布与蒙特卡罗模拟的预期进行了比较，以推导出100-1000TeV区域内各种核基团的能谱。GRAPES-3的结果与直接测量结果的比较表明，Sibyll产生器为解释EAS数据提供了一个很好的强子相互作用的描述。这些测量扩展了初级宇宙射线的能谱和组成，这与直接测量的外推是一致的。太阳耀斑通过各种机制加速带电粒子，这些机制可能会受到高能观测的限制(&gt；10GeV)。我们使用GRAPES-3实验的大面积跟踪微子望远镜，观测到了与2003年10月28日发生的X17级太阳耀斑有关的能量为&gt；20GeV的质子的直接发射。该望远镜对太阳质子的方向性增强具有很高的探测灵敏度，并获得了太阳耀斑引起的质子通量的上限。较少

We made GRAPES-3 air shower array at Ooty in southeren India, constitutes of about 350 scintillator detectors and large area (560m^2) tracking muon detector with 1GeV energy threshold. We got the angular resolution of the present GRAPES-3 experiment by using the two important methods such as EvenOdd and RightLeft methods. The results obtained from the above two methods have been compared with the outcome of the Moon and the Sun shadow observation. The angular resolution is 0.5° for>80TeV. We observed an excess flux in showers selected with 'zero-muon' and 'muon-poor' criteria. These observations yield an integral flux of (5.08±2.67)×10^<-13>cm^<-2>s^<-1> above an energy threshold of 9 TeV and (6.92±2.87)×10^<-14>cm^<-2>s^<-1> for energy above 30TeV. This is the first result with mu-less showers.The composition and the energy spectrum of the primary cosmic rays were measured. The GRAPES-3 experiment including the details of the muon multiplicity distributions observed with a 560 m^2 muo … More n detector as a function of the shower size from the analysis. These distributions have been compared with the expectations from the Monte Carlo simulations, using some of the hadronic interaction generators available with the CORSIKA code, to deduce the energy spectra for various nuclear groups in the 100-1000 TeV region. A comparison of the GRAPES-3 results with the direct measurements indicates that the SIBYLL generator provides a good description of the hadronic interactions for the interpretation of the EAS data. These measurements extend the energy spectra and the composition of the primary cosmic rays that is consistent with extrapolation of the direct measurements.Solar flares accelerate charged particles through a variety of mechanisms, which may be constrained through observations at high energies (>10 GeV). We observed a search for direct emission of protons of energy>20 GeV in association with an X17 class solar flare that occurred on 28 October 2003, using a large area tracking muon telescope of the GRAPES-3 experiment. The telescope has high sensitivity search for the directional enhancement of the solar protons and got upper limit on the flux of protons due to the solar flare. Less