JpGU-AGU Joint Meeting 2020

Presentation information

[J] Oral

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

[M-GI40] Development of computational sciences on planetary formation, evolution and surface environment

convener:Yoshi-Yuki Hayashi(Department of Planetology/CPS, Graduate School of Science, Kobe University), Masaki Ogawa(Division of General Systems Studies, Graduate School of Arts and Sciences, University of Tokyo), Shigeru Ida(Earth-Life Science Institute, Tokyo Institute of Technology), Kanya Kusano(Institute for Space-Earth Environmental Research, Nagoya University)

[MGI40-07] Development of P3T Code for Planetary System Formation: GPLUM

*Yota Ishigaki1,2, Junko Kominami, Junichiro Makino3,4, Masaki Fujimoto2, Masaki Iwasawa4 (1.University of Tokyo, 2.Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3.Kobe University, 4.RIKEN Center for computational Science)

Keywords:N-body simulation, planetary system formation

In the standard theory of the formation of planets in our Solar System, terrestrial planets and the cores of gas giant planets are formed through accretion of km size objects (planetesimals) in the protoplanetary disk. The accretion process of the planets has been mainly investigated using the gravitational N-body simulations of planetesimal systems. However, the use of N-body simulations has been limited to idealized model (e.g., perfect accretion) and/or narrow radial range, due to limited number of particles available.
We have developed a new N-body simulation code with particle-particle particle-tree (P3T) scheme for planetary system formation, GPLUM. GPLUM uses a fourth-order Hermite scheme to calculate gravitational interactions between particles within cut-off radii of individual particles and a Barnes-Hut tree scheme for gravitational interactions with particles outside the cut-off radii. In existing implementations of the P3T schemes, the same cut-off radius is used for all particles. Thus, when the range of the mass of the planetesimals becomes large, the calculation speed decreases. We have solved this problem by allowing each particle to determine its appropriate cutoff radius depending on its mass and distance from the central star.
GPLUM allows us to perform N-body simulations with ~106-107 particles. By using GPLUM, we will perform N-body simulations with wide range and high resolution and investigate various parameters by perform parameter studies with N-body simulations. By using GPLUM, we will perform N-body simulations with wide range and high resolution and investigate various parameters by perform parameter survays with N-body simulations.