The effects of viscosity on circumplanetary disks  

作　　者：De-Fu Bu Hsien Shang Feng Yuan 

机构地区：[1]Key Laboratory for Research in Galaxies and Cosmology,Shanghai Astronomical Observatories,Chinese Academy of Sciences [2]Institute of Astronomy and Astrophysics,Academia Sinica (ASIAA)

出　　处：《Research in Astronomy and Astrophysics》2013年第1期71-86,共16页天文和天体物理学研究（英文版）

基　　金：Supported by the National Natural Science Foundation of China;supported in part by the Natural Science Foundation of China(Grant Nos.10833002,10825314,11103059,11121062 and 11133005);the National Basic Research Program of China(973 Program,2009CB824800);the CAS/SAFEA International Partnership Program for Creative Research Teams

摘　　要：The effects of viscosity on the circumplanetary disks residing in the vicinity of protoplanets are investigated through two-dimensional hydrodynamical simulations with the shearing sheet model. We find that viscosity can considerably affect properties of the circumplanetary disk when the mass of the protoplanet Mp ~ 33 Me, where Me is the Earth＇s mass. However, effects of viscosity on the circumplanetary disk are negligibly small when the mass of the protoplanet Mp 〉 33 Me. We find that when Mp ~ 33 Me, viscosity can markedly disrupt the spiral structure of the gas around the planet and smoothly distribute the gas, which weakens the torques exerted on the protoplanet. Thus, viscosity can slow the migration speed of a protoplanet. After including viscosity, the size of the circumplanetary disk can be decreased by a factor of 〉~ 20%. Viscosity helps to transport gas into the circumplanetary disk from the differentially rotating circumstellar disk. The mass of the circumplanetary disk can be increased by a factor of 50% after viscosity is taken into account when Mp ~ 33 Me. Effects of viscosity on the formation of planets and satellites are briefly discussed.The effects of viscosity on the circumplanetary disks residing in the vicinity of protoplanets are investigated through two-dimensional hydrodynamical simulations with the shearing sheet model. We find that viscosity can considerably affect properties of the circumplanetary disk when the mass of the protoplanet Mp ~ 33 Me, where Me is the Earth＇s mass. However, effects of viscosity on the circumplanetary disk are negligibly small when the mass of the protoplanet Mp 〉 33 Me. We find that when Mp ~ 33 Me, viscosity can markedly disrupt the spiral structure of the gas around the planet and smoothly distribute the gas, which weakens the torques exerted on the protoplanet. Thus, viscosity can slow the migration speed of a protoplanet. After including viscosity, the size of the circumplanetary disk can be decreased by a factor of 〉~ 20%. Viscosity helps to transport gas into the circumplanetary disk from the differentially rotating circumstellar disk. The mass of the circumplanetary disk can be increased by a factor of 50% after viscosity is taken into account when Mp ~ 33 Me. Effects of viscosity on the formation of planets and satellites are briefly discussed.

关 键 词：ACCRETION accretion disks -- hydrodynamics -- planets and satellites：formation -- solar system： formation 

分 类 号：P185[天文地球—天文学]