| Project/Area Number |
25400281
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| Research Category |
Grant-in-Aid for Scientific Research (C)
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| Allocation Type | Multi-year Fund |
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| Section | 一般 |
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| Research Field |
Particle/Nuclear/Cosmic ray/Astro physics
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| Research Institution | National Institute of Technology, Kumamoto College |
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Principal Investigator |
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| Project Period (FY) |
2013-04-01 – 2017-03-31
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| Project Status |
Completed (Fiscal Year 2016)
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| Budget Amount *help |
¥4,940,000 (Direct Cost: ¥3,800,000、Indirect Cost: ¥1,140,000)
Fiscal Year 2015: ¥1,170,000 (Direct Cost: ¥900,000、Indirect Cost: ¥270,000)
Fiscal Year 2014: ¥1,690,000 (Direct Cost: ¥1,300,000、Indirect Cost: ¥390,000)
Fiscal Year 2013: ¥2,080,000 (Direct Cost: ¥1,600,000、Indirect Cost: ¥480,000)
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| Keywords | 超新星爆発 / 元素合成 / 大質量星進化 / 核反応 / 恒星進化 / 大質量星 |
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| Outline of Final Research Achievements |
The project has three major outcomes; (1) By performing simulations of aspherical supernova (SN) explosion of progenitors, which have (10-40) solar masses and nucleosynthetic calculation in SN ejecta, I evaluate abundances and masses of elements of the SN ejecta. In case of early explosion, in which SN explosion occurs 300-400msec after the core-bounce, the evaluated abundances and masses of the ejecta well reproduce the solar abundances and observed masses of elements in SN1987A. (2) We have developed a 2D hydrodynamic code, in which heat produced through nuclear reactions are taken into account. I have examined effects of the heats on the SN explosion in terms of the 2D code. I found that the effects are small on the explosion and nucleosynthesis. (3) I found two progenitors(19.4 and 25 solar masses), whose SN ejecta have abundant 44Ti comparable to the mass observed in SN1987A if I use experimental upper bound of 40Ca(alpha,gamma)44Ti rates and lower bound of 44Ti(alpha,p)47V rates.
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