| 研究課題/領域番号 |
23K22542
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| 補助金の研究課題番号 |
22H01271 (2022-2023)
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| 研究種目 |
基盤研究(B)
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| 配分区分 | 基金 (2024)
補助金 (2022-2023) |
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| 応募区分 | 一般 |
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| 審査区分 |
小区分16010:天文学関連
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| 研究機関 | 国立天文台 |
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研究代表者 |
HULL CHARLES 国立天文台, アルマプロジェクト, 特別客員研究員 (70814755)
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| 研究分担者 |
サヌエザ パトリシオ 国立天文台, アルマプロジェクト, 特任助教 (70769348)
中村 文隆 国立天文台, 科学研究部, 准教授 (20291354)
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| 研究期間 (年度) |
2022-04-01 – 2025-03-31
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| 研究課題ステータス |
交付 (2024年度)
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| 配分額 *注記 |
17,420千円 (直接経費: 13,400千円、間接経費: 4,020千円)
2024年度: 5,200千円 (直接経費: 4,000千円、間接経費: 1,200千円)
2023年度: 5,460千円 (直接経費: 4,200千円、間接経費: 1,260千円)
2022年度: 6,760千円 (直接経費: 5,200千円、間接経費: 1,560千円)
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| キーワード | star formation / High-mass star formation / Magnetic Fields / binary stars / polrization / dust / magnetic fields / Star formation / Polarization / Magnetic fields / Binary stars / Dust |
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| 研究開始時の研究の概要 |
How does the magnetic field affect the formation of binary stars? This is a major outstanding question, given that half of Sun-like stars in the Milky Way Galaxy are in binary systems. Recent surveys by other telescopes have shown that very young star-forming sources fragment into binary systems on two different size scales as a result of two different formation mechanisms. Using cutting-edge data from the ALMA observatory, we will test these formation hypotheses in order to gain a better understanding of the origin of binary sources in our Galaxy.
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| 研究実績の概要 |
The main achievement is that we have submitted the first article studying a binary system, including the magnetic field, in the high-mass regime. This article was led by the hired KAKENHI postdoc.
In this work we find a binary system forming immersed in a magnetic field having a hourglass morphology. All evidence points to a strongly magnetized environment: mass-to-flux ratio of 1.43, no coherent velocity gradients at large scales, lack of core/disk rotation, and absence of molecular outflows. However, in spite of being a strong regulator, the magnetic field fails to prevent the formation of the binary system.
In addition, we have carried out a large portion of data calibration and imaging of the main data set.
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| 現在までの達成度 (区分) |
現在までの達成度 (区分)
3: やや遅れている
理由
The main data set to be used during this research arrived later than expected. However, this inconvenient did not stop to continue addressing the main scientific questions using the other data sets part of the project.
Because we had scripts ready, now with the main data in hand, we move faster than initially expected and we believe we will complete our project on time by the end of the fiscal year.
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| 今後の研究の推進方策 |
The team, led by the hired postdoc, is working and will continue working hard to complete the data reduction (calibration, self-calibration, continuum imaging, and line imaging) as soon as possible.
The first publication of ALPPS will consist in a summary paper led by the hired postdoc. In this paper, we will determine the outflow orientation and search for the presence of velocity gradients and calculate their direction. These quantities will be compared with the magnetic field orientation to evaluate the importance of the magnetic field.
The second publication will combine the information extracted from paper 1 with the binary systems (information published in earlier works). We will then know if the magnetic field has any role in determining binary/multiple systems.
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