日本地球惑星科学連合2021年大会

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セッション記号 P (宇宙惑星科学) » P-CG 宇宙惑星科学複合領域・一般

[P-CG19] 宇宙における物質の形成と進化

2021年6月4日(金) 13:45 〜 15:15 Ch.04 (Zoom会場04)

コンビーナ:瀧川 晶(東京大学 大学院理学系研究科 地球惑星科学専攻)、三浦 均(名古屋市立大学大学院理学研究科)、大坪 貴文(自然科学研究機構 国立天文台)、野村 英子(国立天文台 科学研究部)、座長:大屋 瑶子(東京大学)、野津 翔太(理化学研究所 開拓研究本部 坂井星・惑星形成研究室)

14:15 〜 14:30

[PCG19-09] 磁気駆動円盤風で進化する原始惑星系円盤におけるケイ酸塩ダストの結晶化度

*荒川 創太1、松本 侑士2、本田 充彦3 (1.国立天文台、2.台湾中央研究院、3.岡山理科大学)

キーワード:原始惑星系円盤、ダスト、結晶化度、磁気駆動円盤風

Understanding the process of radial mixing in protoplanetary disks is of great importance in the context of star and planet formation in the solar and extrasolar systems. In particular, the radial distribution of crystalline silicate dust particles in disks is the key to understanding the material mixing process from astronomical observations (e.g., Honda et al. 2006; Maaskant et al. 2015). In protoplanetary disks, dust particles are radially transported by three processes, namely, advection, diffusion, and the radial drift of dust particles. The effects of these processes in viscous accretion disks are studied so far (e.g., Gail 2001; Pavlyuchenkov & Dullemond 2007).
Recent observations of protoplanetary disks by ALMA revealed that the disk structure (e.g., rings, gaps, and spirals) formed in the early stage of disk evolution. The magnetically driven disk wind (e.g., Suzuki et al. 2010) is one of the candidates to create observed structures, and the effects of disk winds on the evolution of dust and gas are investigated in previous studies (e.g., Takahashi & Muto 2018).
Here we calculate the radial distribution of crystalline silicate dust particles in evolving protoplanetary disks due to magnetically driven disk winds. We found that the radial distribution of the crystallinity strongly depends on the timescales of viscous evolution, the radial drift of dust particles, and wind mass loss, as the structure of gas and dust also depends on these timescales (e.g., Takahashi & Muto 2018). The crystallinity of dust particles may relate to the structure of protoplanetary disks.