| Project/Area Number |
16340174
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| Research Category |
Grant-in-Aid for Scientific Research (B)
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| Allocation Type | Single-year Grants |
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| Section | 一般 |
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| Research Field |
Geochemistry/Astrochemistry
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| Research Institution | Kyushu University |
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Principal Investigator |
NAKAMURA Tomoki Kyushu University, Faculty of Science, Associate Professor (20260721)
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| Co-Investigator(Kenkyū-buntansha) |
SEKIYA Minoru KYUSHU UNIVERSITY, Faculty of Science, Professor (60202420)
NOGUCHI Takaaki Ibaraki University, Faculty of Science, Associate Professor (40222195)
OKAZAKI Ryuji KYUSHU UNIVERSITY, Faculty of Science, Research associate (40372750)
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| Project Period (FY) |
2004 – 2007
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| Project Status |
Completed (Fiscal Year 2007)
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| Budget Amount *help |
¥13,020,000 (Direct Cost: ¥12,600,000、Indirect Cost: ¥420,000)
Fiscal Year 2007: ¥1,820,000 (Direct Cost: ¥1,400,000、Indirect Cost: ¥420,000)
Fiscal Year 2006: ¥1,400,000 (Direct Cost: ¥1,400,000)
Fiscal Year 2005: ¥6,600,000 (Direct Cost: ¥6,600,000)
Fiscal Year 2004: ¥3,200,000 (Direct Cost: ¥3,200,000)
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| Keywords | Solar nebula / Carbonaceous chondrites / Cr-Mn chronolo / Cr・Mn年代 / 炭素質コンドライド / Mn-Cr年代 / 水質変成 |
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| Research Abstract |
Mineralogical and isotope study was carried out on the primitive meteorites, CV3 carbonaceous chondrites. The meteorites contain fayalite veins that formed by replacement of magnetite during extensive aqueous alteration. Radiogenic ^<53>Cr excess was detected from the fayalite veins in the Vigarano CV3 chondrite during high-resolution, high-sensitive analysis using secondary ion mass spectrometer. The formation age of the fayalite was obtained to be 4561±3 Ma based on the Mn-Cr chronometer. The age is consistent with that of some other CV3. This suggests that prevailed aqueous alteration took place in the CV3 parent body. Laser-probe noble gas analysis was performed on the sample taken from a portion close to the fayalite. The results of analysis indicate that solar noble gases are contained in the Vigarano sample. The solar gases may have been implanted prior to the formation of the fayalite vein, thus suggesting that solar nebula was dissipated at the time of 4561.3 Ma. Further analysis was planned on the portion including the fayalite veins in order to confirm the results of the present study.
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