Japan Geoscience Union Meeting 2016

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Symbol M (Multidisciplinary and Interdisciplinary) » M-GI General Geosciences, Information Geosciences & Simulations

[M-GI22] Development of computational sciences on planetary formation, evolution and surface environment

Tue. May 24, 2016 9:00 AM - 10:30 AM A07 (APA HOTEL&RESORT TOKYO BAY MAKUHARI)

Convener:*Junichiro Makino(RIKEN AICS), Yoshi-Yuki Hayashi(Department of Planetology/CPS, Graduate School of Science, Kobe University), Shigeru Ida(Department of Earth and Planetary Science, Graduate School of Science and Technology, Tokyo Institute of Technology), Yuri Aikawa(Center for Computational Sciences, University of Tsukuba), Masaki Ogawa(Division of General Systems Studies, Graduate School of Arts and Sciences, University of Tokyo), Masayuki Umemura(Center for Computational Sciences,　University of Tsukuba), Chair:Shigeru Ida(Department of Earth and Planetary Science, Graduate School of Science and Technology, Tokyo Institute of Technology)

10:00 AM - 10:15 AM

[MGI22-05] Global High-resolution N-body Simulation of Planet Formation: Planetesimal Driven Migration with Type-I Migration

*Junko Kominami1, Hiroshi Daisaka2, Junichiro Makino3, Masaki Fujimoto4 (1.Tokyo Institute of Technology, 2.Hitotsubashi University, 3.RIKEN AICS, 4.JAXA)

By means of fully self-consistent N-body simulations, we investigated whether outward Planetesimal Driven Migration (PDM) takes place or not when the self gravity of planetesimals is included. We performed N-body simulations of planetesimal disks with large width (0.7 - 4AU) which ranges over the ice line. The simulations consisted of two stages. The first stage simulations were carried out to see the runaway growth phase using the planetesimals of initially the same mass. The runaway growth took place both at the inner edge of the disk and at the region just outside the ice line. This result was utilized for the initial setup of the second stage simulations in which the runaway bodies just outside the ice line were replaced by the protoplanets with about the isolation mass. In the second stage simulations, the outward migration of the protoplanet was followed by the stopping of the migration due to the increase of the random velocity of the planetesimals. Due to this increase of random velocities, one of the PDM criteria derived in Minton and Levison (2014) was broken. In the current simulations, the effect of the gas disk is not considered. It is likely that the gas disk plays an important role in planetesimal driven migration. Hence, we also carried out N-body simulations of PDM including the gas drag and type-I migration. Type-I migration and gas drag are known as the effects that drag the planeteismals and protoplanets toward the central star. We showed that the random velocity of the planetesimals are subdued by the gas drag and enhances the outward migration. We found that in Minimum Mass Solar Nebula (MMSN), there were a period that outward PDM overcomes the type-I mirgation.