| Project/Area Number |
10041112
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| Research Category |
Grant-in-Aid for Scientific Research (A).
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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 |
KAMIMOTO 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) |
TAJIMA Norio The Institute of Physical and Chemical Research, Engineer, 技術部・専任技師
YOSHII Hisashi Ehime Unibersity, Dep. of Physics, Professor, 理学部, 教授 (00036360)
OGIO Shoichi Tokyo Institute of Technology, Dep. of Physics, Assistant, 大学院・理工学研究科, 助手 (20242258)
VELARDE Alfo サンアンドレス大学, 理学部, 教授
MIRANDA Pedr サンアンドレス大学, 物理学研究所, 教授
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| Project Period (FY) |
1998 – 1999
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| Project Status |
Completed (Fiscal Year 1999)
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| Budget Amount *help |
¥9,700,000 (Direct Cost: ¥9,700,000)
Fiscal Year 1999: ¥4,300,000 (Direct Cost: ¥4,300,000)
Fiscal Year 1998: ¥5,400,000 (Direct Cost: ¥5,400,000)
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| Keywords | Cosmic Rays / Air Shower / Origins of Cosmic Rays / Propagation of Cosmic Rays / Vela Super Nova Remnant / Anisotropy / Glactic Disk / Primary Gamma Rays |
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| Research Abstract |
The origins of primary cosmic rays with energies above 10 TeV are investigated to observe their arrival directional distribution. In this research, we observe air showers at a new air shower array at Mt. Chacaltaya in Bolivia. This new array is constructed to add new detectors to a existing air shower array. For these new detectors we developed a new pre-amplifier, which enables us to observe both local particle densities and arrival times of air shower particles with one photomultiplier.
We start the preliminary observation from October 1998, and the real one from April 1999. In 1999 we change the data store system replacing a 8mm data drive to a DVD-RAM drive and simultaneously change the operating system of data taking PC to the LINUX. After this improvement the dead time of the total measuring system is reduced.
The data are immediately analyzed with a computer and the preliminary results are obtained. These results show the enhancement of cosmic rays along the galactic disk with the galactic longitude around 270 in degree. The degree of this enhancement is about 0.4%. Then we start a computer simulation to account for this enhancement. The preliminary result shows that cosmic rays accelerated at the Vela super nova remnant may explain the observed enhancement. These results are presented by oral at the 26th International Cosmic Ray Conference.
To confirm the present result with enough data, we continue the observation for more three years. Moreover, the simulation calculation with more precise information, for example the information on the galactic magnetic field structure must be done to get final conclusions.
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