Magnetohydrodynamic simulations of the final process of accretion process onto a protostar
| Project/Area Number |
18K13579
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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 | Osaka University (2019-2021)
Nagoya University (2018) |
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Principal Investigator |
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| Project Period (FY) |
2018-04-01 – 2022-03-31
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| Project Status |
Completed (Fiscal Year 2021)
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| Budget Amount *help |
¥3,380,000 (Direct Cost: ¥2,600,000、Indirect Cost: ¥780,000)
Fiscal Year 2021: ¥910,000 (Direct Cost: ¥700,000、Indirect Cost: ¥210,000)
Fiscal Year 2020: ¥910,000 (Direct Cost: ¥700,000、Indirect Cost: ¥210,000)
Fiscal Year 2019: ¥780,000 (Direct Cost: ¥600,000、Indirect Cost: ¥180,000)
Fiscal Year 2018: ¥780,000 (Direct Cost: ¥600,000、Indirect Cost: ¥180,000)
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| Keywords | 星形成 / 降着円盤 / 磁気流体力学 / 磁気流体シミュレーション |
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| Outline of Final Research Achievements |
The transition region between a protostar and a surrounding accretion disk is called the boundary layer. To update the evolution models of protostars, we need to understand the transport processes in this layer. It is particularly important to reveal the roles of magnetic fields, which have been ignored in most of the previous studies. We have conducted three-dimensional magnetohydrodynamic simulations of the accretion just around a protostar. We found that an accreting protostar can produce violent explosions that suddenly release magnetic energy. In addition, our simulation indicates that magnetic fields extract a large amount of angular momentum of the accreting gas in the connecting layer.
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| Academic Significance and Societal Importance of the Research Achievements |
星は宇宙の最小構成要素であり、本研究はその誕生過程の一端を明らかにしたものである。特に原始星フレアは強いX線を生じて惑星形成のもととなる星形成領域の化学組成に影響を及ぼすことが言われていたが、原始星が進化のどの段階から強いX線を出すかについてはよくわかっていなかった。本研究は、原始星はこれまでよりも早い段階から強いX線を繰り返し出す可能性を理論的に示した。この結果は、太陽をはじめとする星の起源のみならず、その周りの惑星がどのような環境で生まれるのかについても示唆を与えるものである。
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Report
(5 results)
Research Products
(39 results)
