PASJ: Publications of the Astronomical Society of Japan | |
Non-linear development of secular gravitational instability in protoplanetary disks | |
Takahashi, Sanemichi Z1  Tominaga, Ryosuke T2  Inutsuka, Shu-ichiro2  | |
[1] Astronomical Institute, Tohoku University, 6-3 Aoba, Aramaki, Aoba-ku, Sendai, Miyagi 980-8578, Japan;Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8602, Japan | |
关键词: instabilities; methods: numerical; protoplanetary disks; | |
DOI : 10.1093/pasj/psx143 | |
学科分类:天文学(综合) | |
来源: Oxford University Press | |
【 摘 要 】
We perform non-linear simulation of secular gravitational instability (GI) in protoplanetary disks, which has been proposed as a mechanism of planetesimal and multiple ring formation. Since the timescale of the growth of the secular GI is much longer than the Keplerian rotation period, we develop a new numerical scheme for a long-term calculation utilizing the concept of symplectic integration. With our new scheme, we first investigate the non-linear development of the secular GI in a disk without a pressure gradient in the initial state. We find that the surface density of dust increases by more than a factor of 100 while that of gas does not increase even by a factor of 2, which results in the formation of dust-dominated rings. A line mass of the dust ring tends to be very close to the critical line mass of a self-gravitating isothermal filament. Our results indicate that the non-linear growth of the secular GI provides a powerful mechanism to concentrate the dust. We also find that the dust ring formed via the non-linear growth of the secular GI migrates inward with a low velocity, which is driven by the self-gravity of the ring. We give a semi-analytical expression for the inward migration speed of the dusty ring.
【 授权许可】
CC BY
【 预 览 】
Files | Size | Format | View |
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RO201910257581723ZK.pdf | 1924KB | download |