| Project/Area Number |
11640260
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| Research Category |
Grant-in-Aid for Scientific Research (C)
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| Allocation Type | Single-year Grants |
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| Section | 一般 |
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| Research Field |
素粒子・核・宇宙線
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| Research Institution | TOKYO INSTITUTE OF TECHNOLOGY |
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Principal Investigator |
KAKIMOTO Fumio Tokyo Institute of Technology. Dep.of Physics, Professor, 大学院・理工学研究科, 教授 (00092544)
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| Co-Investigator(Kenkyū-buntansha) |
OGIO Shoichi Tokyo Institute of Technology. Dep.of Physics, Assistant, 大学院・理工学研究科, 助手 (20242258)
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| Project Period (FY) |
1999 – 2000
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| Project Status |
Completed (Fiscal Year 2000)
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| Budget Amount *help |
¥3,700,000 (Direct Cost: ¥3,700,000)
Fiscal Year 2000: ¥500,000 (Direct Cost: ¥500,000)
Fiscal Year 1999: ¥3,200,000 (Direct Cost: ¥3,200,000)
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| Keywords | Cosmic Rays / Air Shower / Origins of Cosmic Rays / Propagation of Comic Rays / Vela Super Nova Remnant / Anisotropy / Glactic Disk / Primary Gamma Rays |
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| Research Abstract |
The purpose of this research is to get information on the chemical composition of primary cosmic rays with energies above 10 TeV.For this we have observed air cherenkov light at MAS array on Mt. Chacaltaya in Bolivia since August 2000. In 1999 we examined to get the most suitable parameter for use of determination of the chemical composition and to estimate the accuracy in the determination. In this procedure, we used CORSIKA code to simulate air showers. As a result, we confirmed to be able to determine the composition by measuring both the lateral distributions and the arrival time distributions of air Cherenkov light. Then we started to construct detectors up to the end of 1999. In April 2000, we ship these equipments to Bolivia and installed these in MAS array at Mt. Chacaltaya. The operation was started in August 2000 and the observed data was transferred to Japan. The analysis has been made simultaneously in Japan and in Bolivia. The preliminary result shows that observed chemical composition is much consistent with those obtained with direct measurements. This is a crucially important result because this consistency guarantee the rightness to apply our measuring method in more high energy range. We are going to make the observation for more three years and will get the final result.
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