• DOI:10.1093/pasj/psx143
• Corpus ID: 59384555

Non-linear Development of Secular Gravitational Instability in Protoplanetary Disks

@article{Tominaga2017NonlinearDO,
  title={Non-linear Development of Secular Gravitational Instability in Protoplanetary Disks},
  author={Ryosuke T. Tominaga and Shu-ichiro Inutsuka and Sanemichi Z. Takahashi},
  journal={arXiv: Earth and Planetary Astrophysics},
  year={2017}
}

• Ryosuke T. Tominaga, S. Inutsuka, Sanemichi Z. Takahashi
• Published 16 November 2017
• Physics, Geology
• arXiv: Earth and Planetary Astrophysics

We perform non-linear simulation of secular gravitational instability (GI) in protoplanetary disks that has been proposed as a mechanism of the planetesimal formation and the 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 integrator. 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 one hundred while that of gas does not increase even by a factor of two, 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.