| Project Area | Nuclear matter in neutron stars investigated by experiments and astronomical observations |
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| Project/Area Number |
24105004
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| Research Category |
Grant-in-Aid for Scientific Research on Innovative Areas (Research in a proposed research area)
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| Allocation Type | Single-year Grants |
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| Review Section |
Science and Engineering
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| Research Institution | Kyoto University |
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Principal Investigator |
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| Co-Investigator(Kenkyū-buntansha) |
家城 和夫 立教大学, 理学部, 教授 (10159577)
磯部 忠昭 国立研究開発法人理化学研究所, その他部局等, 研究員 (40463880)
川畑 貴裕 京都大学, 理学(系)研究科(研究院), 准教授 (80359645)
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| Co-Investigator(Renkei-kenkyūsha) |
TAKETANI Atsushi 国立研究開発法人理化学研究所, 中性子ビーム技術開発チーム, 副チームリーダー (30222095)
MIZOI Yutaka 大阪電気通信大学, 工学部, 講師 (30388392)
KURITA Kazuhiro 立教大学, 理学部, 教授 (90234559)
BABA Hidetada 国立研究開発法人理化学研究所, 仁科加速器センター, 研究員 (10415268)
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| Research Collaborator |
Lynch W. NSCL, Michigan State University, Professor
Tsang M. B. NSCL, Michigan State University, Professor
Yennello S. J. Cyclotron Inst., Texas A&M Univ., Professor
Xiao Z. Tsinghua Univ., Department of Physics, Professor
Lukasik J. INP, Professor
Pawlowski P. INP, Professor
Hong B. Korea Univ., Department of Physics, Professor
Pollacco E. IRFU/SPhN, CEA-Saclay, Professor
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| Project Period (FY) |
2012-06-28 – 2017-03-31
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| Project Status |
Completed (Fiscal Year 2016)
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| Budget Amount *help |
¥168,740,000 (Direct Cost: ¥129,800,000、Indirect Cost: ¥38,940,000)
Fiscal Year 2016: ¥33,410,000 (Direct Cost: ¥25,700,000、Indirect Cost: ¥7,710,000)
Fiscal Year 2015: ¥21,710,000 (Direct Cost: ¥16,700,000、Indirect Cost: ¥5,010,000)
Fiscal Year 2014: ¥33,930,000 (Direct Cost: ¥26,100,000、Indirect Cost: ¥7,830,000)
Fiscal Year 2013: ¥33,670,000 (Direct Cost: ¥25,900,000、Indirect Cost: ¥7,770,000)
Fiscal Year 2012: ¥46,020,000 (Direct Cost: ¥35,400,000、Indirect Cost: ¥10,620,000)
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| Keywords | 中性子星 / 高密度核物質 / 状態方程式 / 時間射影型検出器 / 高密度原子核物質 / 核物質の状態方程式 / 中間エネルギー重イオン反応 / 実験核物理 / 宇宙物理 / 原子核物質の状態方程式 / 対称エネルギー / 荷電粒子ガス検出器 / 高密度読み出し回路 / 荷電粒子検出器 |
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| Outline of Final Research Achievements |
Neutron star is believed to be created as a remnant of super nova explosion. In order to determine a thermodynamical character of outer core of neutron star through terrestrial experiments we have performed a series of measurements using RIKEN Radio Isotope Beam Factory (RIBF). Various central collisions between neutron-rich tin nucleus and normal tin nucleus were measured. The density achieved by the collisions nearly corresponds to the one for the outer core of neutron star. Both positive and negative pions emitted from the high density nuclear matter were detected by a newly developed large time projection chamber which can provide 3-dimensional image of their tracks. We have successfully accumulated data with higher statistics than planned. Data analysis to extract precise yield ratios between charged pions is in progress. We expect to constrain the EOS for neutron star soon.
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