The migration and growth of protoplanets in protostellar discs

被引:302
作者
Nelson, RP
Papaloizou, JCB
Masset, F
Kley, W
机构
[1] Univ London Queen Mary & Westfield Coll, Astron Unit, London E1 4NS, England
[2] Univ Jena, Inst Theoret Phys, D-07743 Jena, Germany
[3] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany
关键词
accretion; accretion discs; methods : numerical; planets and satellites : general; Solar system : formation; planetary systems;
D O I
10.1046/j.1365-8711.2000.03605.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We investigate the gravitational interaction of a Jovian-mass protoplanet with a gaseous disc with aspect ratio and kinematic viscosity expected for the protoplanetary disc from which it formed. Different disc surface density distributions are investigated. We focus on the tidal interaction with the disc with the consequent gap formation and orbital migration of the protoplanet. Non-linear two-dimensional hydrodynamic simulations are employed using three independent numerical codes. A principal result is that the direction of the orbital migration is always inwards and such that the protoplanet reaches the central star in a near-circular orbit after a characteristic viscous time-scale of similar to 10(4) initial orbital periods. This is found to be independent of whether the protoplanet is allowed to accrete mass or not. Inward migration is helped by the disappearance of the inner disc, and therefore the positive torque it would exert, because of accretion on to the central star. Maximally accreting protoplanets reach about 4 Jovian masses on reaching the neighbourhood of the central star. Our results indicate that a realistic upper limit for the masses of closely orbiting giant planets is similar to 5 Jupiter masses, if they originate in protoplanetary discs similar to the minimum-mass solar nebula. This is because of the reduced accretion rates obtained for planets of increasing mass. Assuming that some process such as termination of the inner disc through a magnetospheric cavity stops the migration, the range of masses estimated for a number of close orbiting giant planets as well as their inward orbital migration can be accounted for by consideration of disc-protoplanet interactions during the late stages of giant planet formation.
引用
收藏
页码:18 / 36
页数:19
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