| Project/Area Number |
18K13595
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| Research Category |
Grant-in-Aid for Early-Career Scientists
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| Allocation Type | Multi-year Fund |
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| Review Section |
Basic Section 16010:Astronomy-related
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| Research Institution | Institute of Physical and Chemical Research |
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Principal Investigator |
Ohashi Satoshi 国立研究開発法人理化学研究所, 開拓研究本部, 研究員 (50808730)
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| Project Period (FY) |
2018-04-01 – 2020-03-31
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| Project Status |
Completed (Fiscal Year 2019)
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| Budget Amount *help |
¥3,900,000 (Direct Cost: ¥3,000,000、Indirect Cost: ¥900,000)
Fiscal Year 2019: ¥1,820,000 (Direct Cost: ¥1,400,000、Indirect Cost: ¥420,000)
Fiscal Year 2018: ¥2,080,000 (Direct Cost: ¥1,600,000、Indirect Cost: ¥480,000)
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| Keywords | 原始惑星系円盤 / 分子雲コア / 星形成 / 惑星形成 / 電波天文 / 偏光 / 偏光観測 |
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| Outline of Final Research Achievements |
The formation of stars and planetary systems is investigated by detailed observations of molecular cloud cores and millimeter-wave polarization observations of protoplanetary disks. Observations of the molecular cloud core reveal how the core splits due to gravitational instability and how multiple stars are born at the same time.
In the millimeter-wave polarization observation of the disk, we show that the polarization mechanism is different depending on the size of the dust by using observations and models. A detailed polarization model and comparison with observations show that the dust size of the protoplanetary disk HD 163296 is different between the rings and the gaps. Furthermore, it was found that the turbulence in this disk is smaller in the inner part of the disk.
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| Academic Significance and Societal Importance of the Research Achievements |
地球を有する太陽系のような星・惑星系の形成を理解することは、太陽系や生命の起源だけでなく銀河形成などの宇宙論的な問題や宇宙の歴史を知るといった、宇宙科学の根源的な問いに答える。
本研究は、星形成を起こす直前の分子雲コアを詳細に観測し、その物理状態を明らかにすることで複数の星が重力不安定によって誕生する様子を示唆した。
さらに原始惑星系円盤ではミリ波偏光のメカニズムを新たに解明し、ダストサイズが偏光メカニズムを変える重要な要因であることを示し、実際にダストが円盤内で成長し惑星形成を開始する様子を捉えた。
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