Origin of γ-ray bursts, magnetars and UHE cosmic rays
| Project/Area Number |
12640302
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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 | Kana Eawa University (2002)
Institute of Space and Astronautical Science (2000-2001) |
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Principal Investigator |
MURAKAMI Toshio Kana Eawa University, Faculty of Scieuce, Kanazawa Univ., Professor (60092350)
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| Co-Investigator(Kenkyū-buntansha) |
NORIAKI Shibazaki Rikkyo Univ., Department of Physics, Professor (50206124)
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| Project Period (FY) |
2000 – 2002
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| Project Status |
Completed (Fiscal Year 2002)
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| Budget Amount *help |
¥2,800,000 (Direct Cost: ¥2,800,000)
Fiscal Year 2002: ¥700,000 (Direct Cost: ¥700,000)
Fiscal Year 2001: ¥900,000 (Direct Cost: ¥900,000)
Fiscal Year 2000: ¥1,200,000 (Direct Cost: ¥1,200,000)
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| Keywords | γ-ray bursts / magnetar / OHE cosmic rays / マグネター / パルサー / X線星 / 宇宙線 |
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| Research Abstract |
We have targeted the three topics in this project, which are Gamma-Ray Bursts (GRBs), Magnetars and Ultra High Energy (UHE) cosmic-rays. In GRBs, we studied the iron feature in the X-ray afterglow spectrum. This feature might be a best key to solve the origin of GRBs. If exist, GRBs should be from the evolved environment which is a star forming region. There was a serious discrepancy in the iron line energy and the redshift for the case of GRB 970828 which was observed with ASCA. We solved this discrepancy as the result of the non-equilibrium ionization plasma. If so, the GRB is very far and from the evolved environment, which is consistent with other GRBs.
Concerning Magnetars, we have observed SGR1900-00 and discovered a pulsar component following the our discovery of SGR 1806-20. This was the 2nd discovery of our group. Then we have searched the 3rd one but failed. In any case, the reality of the super-strong magnetic field and neutron star are established through these observations.
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Report
(4 results)
Research Products
(29 results)
