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大学・研究所にある論文を検索できる 「星形成過程の円盤初期進化段階におけるダストのダイナミクスと惑星形成への示唆」の論文概要。リケラボ論文検索は、全国の大学リポジトリにある学位論文・教授論文を一括検索できる論文検索サービスです。
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星形成過程の円盤初期進化段階におけるダストのダイナミクスと惑星形成への示唆

古賀, 駿大 KOGA, Shunta コガ, シュンタ 九州大学

2022.03.23

概要

Stars form in molecular cloud cores composed of gas and dust particles, and it is understood that planetary nuclei, which are dust particle aggregates, appear within the rotationally supported disks that grow in star formation processes. However, while the dynamics of dust in star formation processes have been investigated in both theoretical and observa- tional studies, they remain poorly understood because of the dust property uncertainties. Accordingly, this study proposes a method for calculating dust particle trajectories in which dust particles are treated as Lagrangian particles. I then implement my method in a previously developed nested grid code in which the local physical quantities of gas fluid are used to calculate dust dynamics. More specifically, I perform three-dimensional (3D) magnetohydrodynamic (MHD) simulations that include dust particle trajectory calcula- tions to investigate dust dynamics in a collapsing cloud with variously-sized dust particles. I then show that the obtained results are qualitatively and quantitatively consistent with previous studies that adopted one- or two-fluid approximations with the Eulerian approach. I also find that dust particles that satisfy ad ≤ 10 µm (where ad is the dust particle size) couple with the gas during gravitational collapse until the protostellar mass reaches about 8% of the initial cloud core mass. This coupling condition is also consistent with previous studies. Next, I show that the trajectory calculation adopted in this study is appropriate for tracing dust dynamics in star formation processes. Then, focusing on the trajectories of the dust particles in the disk, I determine that dust particles with an initial large θ (θ is the zenith angle) enter the disk from the equatorial plane rather than from the above, and that such dust particles do not spiral down into the central star even though they move in a circular motion. Furthermore, while the gas within 10 au loses its angular momentum, the gas beyond that distance receives angular momentum due to gravitational torque. Thus, dust particles that are strongly coupled with gas at a distance of around 10 au move also undergo circular motion.

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