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Total flux of Cosmic Rays around knee region using Tibet Air Shower Array

使用西藏空气淋浴阵列计算膝部周围宇宙射线的总通量

基本信息

批准号：
06640374
负责人：
HOTTA Naoki
金额：
$ 1.34万
依托单位：
Utsunomiya University
依托单位国家：
日本
项目类别：
Grant-in-Aid for General Scientific Research (C)
财政年份：
1994
资助国家：
日本
起止时间：
1994 至 1995
项目状态：
已结题

来源：
https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-06640374/
关键词：
Cosmic ray Flux of primary cosmic-rays Air shower Knee region ニ-領域

项目摘要

We analyzed the experimental data obtained with Tibet array and obtained the energy spectrum of the primary cosmic rays in the energy range between 3*10^<14>and2*10^<16>eV.The overall primary energy spectrum obtained does not resemble a single power law and shows a gradual steepening of the slope at energies around E_b=10^<15.25>eV.The spectrum can be expressed asJ(E_o)=1.5*10^<-20>(E_o/10^<14.75>eV)^<-2.60<plus-minus>0.04>(m^<-2>sec^<-1>sr^<-1>eV^<-1>)atE_o<10^<14.75>eVand=1.2*10^<-23>(E_o/10^<15.85>eV)^<-3.00<plus-minus>0.05>(m^<-2>sec^<-1>sr^<-1>eV^<-1>)atE_o>10^<15.85>eV,while this changes gradually between 10^<14.75>and 10^<15.85>eV and takes the value J(E_o)=6.7*10^<-22>(m^<-2>sec^<-1>sr^<-1>eV^<-1>)atE_o=10^<15.25>eVOur spectrum to be smoothly connected to the direct measurements by Grigorov et al.(1971) and JACEE Collaboration (Burnett et al.1993) at the lower energy region. The flux values around 10^<15> eV are higher than the Akeno data (Nagano et al.1984), while those at energies around 10^<16> are about 10 % lower than theirs. The bending of the spectrum is not as abrupt as the Akeno and its energy (E_b) is also lower than theirs. Their lower flux at energies around 10^<15> could be attributed to very low detection effciencies of air showers at the Akeno altitude.Our spectrum obtained around the knee is almost independent of the primary mass composition and will be rated as most standard.The gradual steepening of the spectrum at lower energy may be in favor of shock acceleration at SNRs which suggests a considerable change in the relative abundance of the various cosmic ray nuclei as the energy increases, but its confirmation requires more direct information about the primary mass composition at energies around the knee.

对西藏天线阵的实验数据进行了分析，得到了初级宇宙线在3×10^~2×10^~2×10^~(16)eV能量范围内的能谱，总的能谱不是单次幂函数，而是在能量E_b=10^~(-1)~(15.25)~(？)eV附近呈现出一个逐渐变陡的斜率，谱可表示为asJ(E_o)=1.5*10^&lt；-20&gt；(E_o/10^&lt；14.75&gt；eV)^&lt；-2.60&lt；plus-minus&gt；0.04&gt；(m^&lt；-2&gt；sec^&lt；-1&gt；sr^&lt；-1&gt；eV^&lt；-1&gt；)atE_o&lt；10^&lt；14.75&gt；eVand=1.2*10^&lt；-23&gt；(E_o/10^&lt；15.85&gt；eV)^&lt；-3.00&lt；plus-minus&gt；0.05&gt；(m^&lt；-2&gt；sec^&lt；-1&gt；sr^&lt；-1&gt；eV^&lt；-1&gt；)atE_o&gt；10^&lt；15.85&gt；eV，，而这在10^lt；14.75ev和10^lt；15.85ev之间逐渐变化，取值为J(E_o)=6.7*10^&lt；-22&gt；(m^&lt；-2&gt；sec^&lt；-1&gt；sr^&lt；-1&gt；Ev^&lt；-1&gt；)ATE_o=10^&lt；15.25&gt；eVOur谱与Grigorov等人(1971)和Jacee Collaboration(Burnett等人1993)在低能区的直接测量结果一致。10^&lt；15&gt；ev附近的通量值高于Akeno数据(Nagano et al.1984)，而能量在10^&lt；16&gt；ev附近的通量值比他们的低约10%。光谱的弯曲不像Akeno那样突然，它的能量(E_B)也比他们的低。它们在能量约10^&lt；15&gt；时的低通量可以归因于Akeno高度空气簇射的探测效率非常低。我们在膝盖周围获得的光谱几乎与初级质量组成无关，将被评为最标准的光谱。在较低能量下光谱的逐渐陡峭可能有利于SNR处的激波加速，这表明随着能量的增加，各种宇宙线核的相对丰度发生了相当大的变化，但它的证实需要关于膝盖周围能量的初级质量组成的更直接信息。