CAPTURE AND EVOLUTION OF PLANETESIMALS IN CIRCUMJOVIAN DISKS
CAPTURE AND EVOLUTION OF PLANETESIMALS IN CIRCUMJOVIAN DISKS
复制标题
环木星盘中星子的捕获和演化
DOI：
10.1088/0004-637x/806/2/203
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发表时间：
2015
期刊：
影响因子：
--
通讯作者：
M. Podolak
中科院分区：
文献类型：
--
作者：
G. D’Angelo;M. Podolak
我们研究的演变，星子在演变的气体磁盘，轨道太阳质量的星星和港口的一颗行星质量的行星在一个p <5？> Au。的气体动力学建模与三维流体动力学代码，采用嵌套网格，并实现了一个木星半径的分辨率在环行星盘。该代码将实体建模为单个粒子。微行星受到星星和行星的引力、气体的拖曳力、冲压压力的破坏和烧蚀的质量损失。固体的质量演化是根据其温度、速度和位置自洽地计算的。我们考虑半径为0.1-100公里的冰和冰/岩石天体，最初部署在星星周围的轨道上，在行星轨道的几个希尔半径（RH）内。微行星向内、向外和向半径为r a p？>的盘区域分散。.散射可以重新定位大量的固体，前提是区域r − a p 3？> RH被星子补充。分散的天体可以暂时被行星中心轨道捕获。烧蚀消耗几乎所有的固体在气体温度220？> K.围绕气体间隙外边缘和超出气体间隙外边缘的超克普勒旋转可以分离0.1公里？>体，在尺寸相关的径向位置处产生实心间隙边缘。固体的捕获、分解和烧蚀导致了一个充满灰尘的环行星盘，表面密度很低，只有千米大小的星子，这意味着卫星形成的时间相对较长。在一颗巨大的行星获得大部分质量后，固体的吸积不太可能显著改变其重元素含量。由固体吸积产生的光度和收缩光度可以是相似的数量级。
We study the evolution of planetesimals in evolved gaseous disks that orbit a solar-mass star and harbor a Jupiter-mass planet at a p ≈ 5 ?> AU. The gas dynamics are modeled with a three-dimensional hydrodynamics code that employs nested grids and achieves a resolution of one Jupiter radius in the circumplanetary disk. The code models solids as individual particles. Planetesimals are subjected to gravitational forces by the star and the planet, a drag force by the gas, disruption via ram pressure, and mass loss through ablation. The mass evolution of solids is calculated self-consistently with their temperature, velocity, and position. We consider icy and icy/rocky bodies of radius 0.1–100 km, initially deployed on orbits around the star within a few Hill radii (RH) of the planet's orbit. Planetesimals are scattered inward, outward, and toward disk regions of radius r ≫ a p ?> . Scattering can relocate significant amounts of solids, provided that regions ∣ r − a p ∣ ∼ 3 ?> RH are replenished with planetesimals. Scattered bodies can be temporarily captured on planetocentric orbits. Ablation consumes nearly all solids at gas temperatures ≳ 220 ?> K. Super-Keplerian rotation around and beyond the outer edge of the gas gap can segregate ≲ 0.1 km ?> bodies, producing solid gap edges at size-dependent radial locations. Capture, break-up, and ablation of solids result in a dust-laden circumplanetary disk with low surface densities of kilometer sized planetesimals, implying relatively long timescales for satellite formation. After a giant planet acquires most of its mass, accretion of solids is unlikely to significantly alter its heavy element content. The luminosity generated by accretion of solids and the contraction luminosity can be of similar orders of magnitude.
影响因子：
3.2
作者：
V. Mannings;A. Boss;S. Russell
通讯作者：
V. Mannings;A. Boss;S. Russell
影响因子：
4.8
作者：
Bell, Cameron P. M.;Naylor, Tim;Littlefair, S. P.
通讯作者：
Littlefair, S. P.