A Study of Point Source and Acceleration Mechanism.

点源及加速机制研究。

• 批准号: 05045022
• 负责人: ITO Nobuo
• 金额: $ 3.84万
• 依托单位: Osaka City University
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for international Scientific Research
• 财政年份: 1993
• 资助国家: 日本
• 起止时间: 1993 至 1995
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-05045022/
• 关键词: Extensive Air Shower; gamma-ray point source; Chemical Composition; Acceleration Mechanism; Nuclear Interaction; 点源探索; 高エネルギーγ線; 一次線組成

To study primary cosmic ray composition, point source of high energy gamma-ray and characteristic feature of nuclear interactions, a new extesive air shower array is under construction at Ooty in southern India, at an altitude of 2,200m above s・l.This air shower array contains about 1,000 plastic scintillators (area 1m^2 each) to be covered 300m*300m in area and 4 units of muon detectors (each unit consists of 36m^2*4 in area) to be covered 564m^2 in area at the central region of above EAS array. These muon detector consist of 4 layrs of proportional counters in orthogonal conditions, and energy of muons to be passed through in verticalis-0.6GeV.This EAS array promise us to be able to establish primary composition upto energy of -10^<16> eV and give clear identification of parent particles by measuring both lateral density distribution of electons and muons. In addition to this, we can also measure the multiplicity distribution for showers initiated by primaries of various energy groups. From the comparison of Monte Carlo simulations concerning the detection efficiencey and expected event rate classified by primary composition gives us very accurate information concerning the primary composition.Huge muon detector gives us very clear cut to identify between primary gamma-ray and nuclear compositions. In addition to the above considering development of EAS,we can select gamma-ray primaries. From both accurate determination ofarrival direction of EAS and gamma-rays, if gamma-ray sources exist, we can be identified for them.

为了研究初级宇宙线成分、高能伽马射线点源和核相互作用的特征，在印度南部乌蒂海拔2,200m以上的地方正在建造一个新的大型空气淋浴阵列。该空气淋浴阵列包含约1,000个塑料闪烁体（每个面积1m^2），覆盖面积为300m*300m，以及4个μ子探测器（每个单元由 36m^2*4 面积）覆盖上述 EAS 阵列中心区域 564m^2 面积。这些μ子探测器由正交条件下的4层正比计数器组成，垂直穿过的μ子能量为-0.6GeV。该EAS阵列使我们能够确定能量高达-10^<16> eV的初级成分，并通过测量电子和μ子的横向密度分布来清晰地识别母粒子。除此之外，我们还可以测量由不同能量组的初级引发的流星雨的多重分布。通过蒙特卡罗模拟对按主要成分分类的检测效率和预期事件发生率的比较，我们可以得到有关主要成分的非常准确的信息。巨大的μ子探测器使我们可以非常清晰地识别主要伽马射线和核成分。除了上述考虑EAS的发展外，我们还可以选择伽马射线原色。通过对EAS和伽马射线到达方向的准确测定，如果存在伽马射线源，我们就可以对其进行识别。

项目成果

H.Adarkar: "Search for Neutrino Osillation Using K.G.F.Data" Proc.23rd International Cosmic Ray conference.H.E 4. 487-490 (1993)

H.Adarkar：“使用 K.G.F.Data 搜索中微子振荡”Proc.23rd 国际宇宙射线会议。H.E 4. 487-490 (1993)

N.Ito,S.Kawakami,Y.Hayashi,Y.Uchihori,V.S.Narasimham,M.R.Krishnaswamy et al.: "Special type of Events observed at Great Underground Depth" Proc.VIII Int.Symposium on Very High Energy Cosmic Ray Interaction. 699-710 (1994)

N.Ito,S.Kawakami,Y.Hayashi,Y.Uchihori,V.S.Narasimham,M.R.Krishnaswamy 等人：“在地下大深度观察到的特殊类型的事件”Proc.VIII 极高能宇宙射线相互作用国际研讨会。

H.Adarkar,M.G.K.Menon,V.S.Narasimham,B.V.Sreekantan,Y.Hayashi,N.Ito,S.Kawakami: "Search for Neutrino Osillation Using K.G.F.Data" Proc.23rd International Cosmic Ray Conference.H.E. 4. 487-490 (1993)

H.Adarkar,M.G.K.Menon,V.S.Narasimham,B.V.Sreekantan,Y.Hayashi,N.Ito,S.Kawakami：“使用 K.G.F.Data 搜索中微子振荡”Proc.23rd 国际宇宙射线会议。

N.Ito,Y.Hayashi,S.Kawakami,Y.Uchihori,V.S.Naraimham,M.R.Krishnaswamy,N.K.Mondal et al.: "Point Source Search at Great Underground depth" XXIV ICRC Roma HE4 発表予定.

N. Ito、Y. Hayashi、S. Kawakami、Y. Uchihori、V. S. Naraimham、M. R. Krishnaswamy、N. K. Mondal 等人：“大地下深处的点源搜索” XXIV 红十字国际委员会罗马 HE4 即将推出。

K.Sivaprasad: "Study of Primary Cosmic Ray Energy Spectrum with a Compact Electorn Detecctor Array" Proc.24th International Cosmic Ray Conference.H.E 1. 490-490 (1995)

K.Sivaprasad：“利用紧凑型电子探测器阵列研究初级宇宙射线能谱”Proc.24th International Cosmic Ray Conference.H.E 1. 490-490 (1995)