Migration of massive planets in accreting disks
Migration of massive planets in accreting disks
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DOI：
10.1051/0004-6361/201424837
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发表时间：
2014-11
期刊：
影响因子：
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通讯作者：
Christoph Durmann;W. Kley
中科院分区：
文献类型：
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作者：
Christoph Durmann;W. Kley
据信，在吸积盘上打开缺口的大质量行星会以恰好与吸积盘相同的粘性速度迁移，这一机制被称为第二类迁移。人口合成模型表明，标准的II型迁移速度太快，与观测结果不符。我们研究了质量为0.2到2的木星质量为M_J$的大质量行星在10^-4到10^-3之间的迁移。以便估计与第二类移民相比的迁移率。我们跟踪嵌入在具有非零质量吸积的二维局部等温盘中的行星的演化，这是使用适当的流入和流出边界条件来明确建模的，以确保特定的吸积率。在一定的松弛时间后，我们释放行星，并测量其通过圆盘的迁移以及对诸如粘度、吸积率和行星质量等参数的依赖。我们研究吸积行星和非吸积行星。所推断的行星迁移率完全由作用在其上的盘力矩决定，与粘性流入速度完全无关，因此不存在经典的第二类迁移区。根据本地磁盘质量的不同，迁移速度可能比第二类迁移更快，也可能更慢。从盘中的扭矩和吸积率剖面我们可以看到，行星形成的间隙并没有像第二类迁移所必需的那样将内盘和外盘分开，而是气体穿过了间隙或被吸积到行星上。
Massive planets that open a gap in the accretion disk are believed to migrate with exactly the viscous speed of the disk, a regime termed type II migration. Population synthesis models indicate that standard type II migration is too rapid to be in agreement with the observations. We study the migration of massive planets between $2\times10^{-4}$ and $2\times10^{-3} M_\odot$ corresponding to 0.2 to 2 Jupiter masses $M_J$. in order to estimate the migration rate in comparison to type II migration. We follow the evolution of planets embedded in two-dimensional, locally isothermal disks with non-zero mass accretion which is explicitly modelled using suitable in- and outflow boundary conditions to ensure a specific accretion rate. After a certain relaxation time we release the planet and measure its migration through the disk and the dependence on parameters such as viscosity, accretion rate and planet mass. We study accreting and non-accretion planets. The inferred migration rate of the planet is determined entirely by the disk torques acting on it and is completely independent of the viscous inflow velocity, so there is no classical type II migration regime. Depending on the local disk mass the migration rate can be faster or slower than type II migration. From the torques and the accretion rate profile in the disk we see that the gap formed by the planet does not separate the inner from the outer disk as necessary for type II migration, rather gas crosses the gap or is accreted onto the planet.