Study of chemical composition and acceleration mechanism of primary cosmic ray at mountain altitude in India

印度山区初级宇宙线化学成分及加速机制研究

• 批准号: 09045037
• 负责人: KAWAKAMI Saburo
• 金额: $ 3.39万
• 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 (B).
• 财政年份: 1997
• 资助国家: 日本
• 起止时间: 1997 至 1999
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-09045037/
• 关键词: chemical composition; Ectensive Air Shower; primary cosmic; Monte Carlo Simulation; diffused gamma ray; モンテカルロ・シミュレーション; 宇宙線; 化学組成; γ線点源; 等方的γ線; ミューオン成分; 電磁成分; 宇宙線組成; 太陽活動; γ線源

It is important to study the chemical composition of primary cosmic rays to know the origin and propagation and acceleration mechanism of them. At a same time the change in slope of energy spectrum around energy range of 10ィイD113ィエD1〜10ィイD116ィエD1eV, so called "knee" region, is also the primary object of our present observation.We have established the huge detector array for Extensive Air Shower (EAS) observation at Ooty (800g/cmィイD12ィエD1). It is named with GRAPES III. It consists of 217 (each 1mィイD12ィエD1) scintillation detectors (SCD) and 16 (each 36mィイD12ィエD1) proportional counter detectors (PCD). PCD can detect the low energy muons energy grater than 1 GeV. We observe the direction of EAS and the lateral density distribution of electro-magnetic components and muon components precisely. We can study the chemical composition of primary cosmic rays though these observations. Our array is designed to optimize to observe EAS size around 10ィイD14ィエD1 to 10ィイD17ィエD1. So far we are operating our apparatus continuously without much problems and obtained the following results.1. We have derived the size spectrum of EAS between 10ィイD14ィエD1 and 10ィイD16ィエD1. Those results showed reasonable agreement within the experimental error with other measurements.2. Our observed lateral density distribution of muons showed good agreement with the results of Monte Carlo simulation, though there are small difference among the model of hadron interaction.3. We have got upper limit for the ratio between diffused gamma rays and cosmic rays and cosmic rays as 3x10ィイD1-3ィエD1.This value gives the best value of upper limit in the energy range 10ィイD114ィエD1〜10ィイD115ィエD1eV at present. We are satisfied to know our observation system is working pretty well as it was aimed so. We are planning to improve the analysis method and accumulate the simulation results. Comparison between those results will surely tell us the chemical composition of primary cosmic rays.

研究初级宇宙线的化学成分对了解初级宇宙线的起源、传播和加速机制具有重要意义。同时，能谱在10 μ m D113 μ m D110 μ m D116 μ m D1 eV附近的斜率变化，即所谓的“膝”区，也是我们目前观测的主要对象。它被命名为GRAPES III。它由217个（每个1 m长的D12闪烁D1）闪烁探测器（SCD）和16个（每个36 m长的D12闪烁D1）正比计数器探测器（PCD）组成。PCD可以探测能量大于1GeV的低能μ子。我们精确地观测到了EAS的方向以及电磁分量和μ子分量的横向密度分布。通过这些观测，我们可以研究初级宇宙线的化学组成。我们的阵列旨在优化观察EAS大小约10 μ m D14 μ m D1至10 μ m D17 μ m D1。到目前为止，我们一直在操作我们的设备，没有太多的问题，并获得了以下结果.我们导出了10 μ m D14 μ m D1和10 μ m D16 μ m D1之间EAS的尺寸谱。这些结果与其他测量结果在实验误差范围内显示出合理的一致性.我们观测到的μ子横向密度分布与Monte Carlo模拟的结果吻合较好，尽管强子相互作用模型之间的差别很小.得到了扩散γ射线与宇宙射线和宇宙射线比值的上限为3 × 10 ~（-1）D ~（1 -3）D ~（1 -3）D ~（1 -3）D ~（1 - 3），这是目前在10 ~（-1）D ~（114）D ~（1 - 1）10 ~（-1）D ~（115）D ~（1 - 1）eV能量范围内的最佳上限值。我们很满意地知道，我们的观测系统工作得很好，因为它是这样的目的。我们计划改进分析方法，积累模拟结果。这些结果之间的比较肯定会告诉我们初级宇宙射线的化学成分。

项目成果

T.Yamamoto et al.: "The energy spectrum of high energy gamma rays from Mrk501 by the stereoscopic analysis"Proc. of 26th Int. Cosmic Ray Conf.. V3. 297-300 (1999)

T.Yamamoto 等人：“通过立体分析获得 Mrk501 高能伽马射线的能谱”Proc.

M.Sasano et al.: "Limits on the isotropic γray/Cosimc ray ratio in the ultra high energy region from the EAS experiment at Ooty"Proc. of 26th Int. Cosmic Ray Conf.. V4. 85-88 (1999)

M.Sasano 等人：“Ooty 的 EAS 实验中各向同性 γ 射线/Cosimc 射线比率的限制”第 26 届宇宙射线会议 V4（1999）。

Y.Hayashi, N.Ito, S.Kawakami, et.al.: "A study on Fine Features in the Energy Spectrum of Primary Cosmic Rays Over the Energy range 1x10^14-3x10^16eV with the GRAPES III array at Ooty" 25th Int. Cosmic Ray Conference,DURBAN. 4. 153-156 (1997)

Y.Hayashi、N.Ito、S.Kawakami 等人：“利用 Ooty 的 GRAPES III 阵列对 1x10^14-3x10^16eV 能量范围内初级宇宙射线能谱的精细特征进行研究”

H.Adarkar et al.: "Cosmic Ray Composition with KGF Underground Detector"Physical Review D. 57. 2653-2664 (1998)

H.Adarkar 等人：“Cosmic Ray Composition with KGF Underground Detector”Physical Review D. 57. 2653-2664 (1998)

D.Nishikawa et al.: "Periodicity in the TeV gamma rays and X rays from Markarian501"Proc.of 26th Int. Cosmic Ray Conf.. 3. 354-357 (1999)

D.Nishikawa 等人：“来自 Markarian501 的 TeV 伽马射线和 X 射线的周期性”Proc.of 26th Int.