[P-PS07] 惑星科学

[PPS07-19] 巨大惑星まわりの周惑星円盤への衛星材料の供給：ダスト鉛直分布と惑星質量への依存性

*前田 夏穂¹、大槻 圭史¹、末次 竜²、谷川 享行³、町田 正博⁴ (1.神戸大学、2.大島商船高等専門学校、3.一関工業高等専門学校、4.九州大学)

キーワード：惑星形成、衛星形成

The principal satellites of giant planets, such as Galilean satellites and Titan, are considered to be formed by the accretion of solid materials in the gaseous disk around a giant planet, i.e., circumplanetary disk. Although building blocks of the satellites are likely to be supplied from the protoplanetary disk into the circumplanetary disk, there are many unknowns in the supply process. Recent numerical studies show that three-dimensional gas flow around a planet significantly influences the supply of solid materials (Tanigawa et al. 2012, 2014; Homma et al. 2020). On the other hand, it is not well understood yet how the process depends on planetary mass. In this work, we calculate the orbits of solid particles considering the gas drag force using the gas field obtained by the local three-dimensional hydrodynamic simulation (Maeda et al. 2022). Then we investigate the planetary-mass dependence of the supply process of dust particles to the circumplanetary disk.
We found that the larger the planetary mass, the more dust is captured by the circumplanetary disk over a larger radial region. We also found that the dust mass accretion rate into the circumplanetary disk highly depends on dust scale height in the protoplanetary disk but not so much on the planetary mass. In addition, we found that the planetary mass of the dust-to-gas inflow rate ratio into the circumplanetary disk depends on the degree of dust stirring in the protoplanetary disk.
We will discuss the implication for satellite formation around a giant planet based on the above results, the latest satellite formation model, and observations of the circumplanetary candidates.