N-body simulation of planetary formation through pebble accretion in a radially structured protoplanetary disk

被引:0
作者
Jinno, Tenri [1 ]
Saitoh, Takayuki R. [1 ]
Ishigaki, Yota [2 ]
Makino, Junichiro [1 ]
机构
[1] Kobe Univ, Grad Sch Sci, Dept Planetol, 1-1 Rokkodai Cho,Nada Ku, Kobe, Hyogo 6578501, Japan
[2] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan
关键词
methods: numerical; planets and satellites: formation; planets and satellites: terrestrial planets; PARTICLE PARTICLE-TREE; MAGNETOROTATIONAL INSTABILITY; TERRESTRIAL PLANETS; OLIGARCHIC GROWTH; GIANT PLANETS; SOLAR NEBULA; TURBULENCE; EVOLUTION; CORES; SUBSTRUCTURES;
D O I
10.1093/pasj/psad053
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
In the conventional theory of planet formation, it is assumed that protoplanetary disks are axisymmetric and have a smooth radial profile. However, recent radio observations of protoplanetary disks have revealed that many of them have complex radial structures. In this study, we perform a series of N-body simulations to investigate how planets are formed in protoplanetary disks with radial structures. For this purpose, we consider the effect of continuous pebble accretion onto the discontinuity boundary within the terrestrial planet-forming region (similar to 0.6 au). We find that protoplanets grow efficiently at the discontinuity boundary, reaching the Earth mass within similar to 104 yr. We confirm that giant collisions of protoplanets occur universally in our model. Moreover, we find that multiple planet-sized bodies form at regular intervals in the vicinity of the discontinuity boundary. These results indicate the possibility of the formation of solar system-like planetary systems in radially structured protoplanetary disks.
引用
收藏
页码:951 / 969
页数:19
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