Did Hypernova Explosions of the First Generation Stars Produce the Chemical Peculiarity of the Objects in Early Universe?
| Project/Area Number |
16540229
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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 |
Particle/Nuclear/Cosmic ray/Astro physics
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| Research Institution | The University of Tokyo |
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Principal Investigator |
NOMOTO Ken'ichi The University of Tokyo, Graduate School of Science, Professor, 大学院・理学系研究科, 教授 (90110676)
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| Co-Investigator(Kenkyū-buntansha) |
SUZUKI Tomoharu The University of Tokyo, Graduate School of Science, Research Associate, 大学院・理学系研究科, 助手 (20280935)
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| Project Period (FY) |
2004 – 2005
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| Project Status |
Completed (Fiscal Year 2005)
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| Budget Amount *help |
¥3,600,000 (Direct Cost: ¥3,600,000)
Fiscal Year 2005: ¥1,700,000 (Direct Cost: ¥1,700,000)
Fiscal Year 2004: ¥1,900,000 (Direct Cost: ¥1,900,000)
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| Keywords | stellar evolution / stellar population / stellar abundance / supernova / hypernova / nucleosynthesis / iron / galactic chemical evolution |
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| Research Abstract |
The first generation of stars, called Population III stars, in the Universe do not contain heavy elements. In this study, we tried to investigate their nature from the comparison between nucleosynthesis and the chemical abundances of extremely metal-poor (EMP) stars. We focus on the peculiar abundance pattern of EMP stars, in particular, those of the hyper metal-poor (HMP) star discovered by SUBARU telescope, whose, metallicity is only less than 5 orders of magnitude. This HMP star has extremely large C/Fe but also large (Na,Mg,Al)/Fe. Such an abundance pattern may stem from nucleosynthesis in Pop III stars.
In this study, we extended our study of nucleosynthesis in Pop III stars to the aspherical explosion models. Our findings are summarized as follows :
1) Among the HMP/EMP stars, many C and N-rich stars with quite large ratios of (C,N)/Fe have been discovered. We showed that such large ratios can be explained with the black-hole-forming supernovae.
2) Variations of (Na,Mg,Al)/Fe among the C-rich HMP/EMP stars can be explained with the mixing and the fallback mechanism, and the dependence on the explosion energy.
3) In spherical models, large fallback is realized in the relatively low energy explosions.
4) In bipolar explosions, the mixing-fallback like events are naturally induced, so that hypernova explosion model can work.
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Report
(3 results)
Research Products
(14 results)
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[Journal Article] Evidence for Nucleosynthesis in the Supernova γ-Process : Universal Scaling for ρ Nuclei2004
Author(s)
Hayakawa, T., Iwamoto, N., Shizuma, T., kajino, T., Umeda, H., Nomoto, K.
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Journal Title
Physical Review Letters 93
Related Report
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[Journal Article] Properties of Two Hypernovae Entering the Nebular Phase : SN 1997ef and SN 1997dq2004
Author(s)
Mazzali, P.A., Deng, J., Maeda, K., Nomoto, K., Filippenko, A.V., Matheson, T.
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Journal Title
Astrophys.J. 614
Pages: 858-863
Related Report
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