MIGRATION OF GAS GIANT PLANETS IN GRAVITATIONALLY UNSTABLE DISKS
MIGRATION OF GAS GIANT PLANETS IN GRAVITATIONALLY UNSTABLE DISKS
复制标题
气态巨行星在引力不稳定的圆盘中的迁移
DOI：
10.1088/2041-8205/737/2/l42
复制
发表时间：
2011
期刊：
影响因子：
--
通讯作者：
A. Boley
中科院分区：
文献类型：
--
作者：
S. Michael;R. Durisen;A. Boley
引力不稳定圆盘中的迁移特征对于理解由圆盘不稳定形成的原行星的命运是必要的。作为更大规模研究的一部分，我们正在使用三维辐射流体动力学代码来研究嵌入的气态巨行星如何与经历重力不稳定（GI）的气盘相互作用。这封信介绍了一颗木星质量行星在 0.14 M☉ 盘内 25 天文单位轨道上的模拟结果。该圆盘围绕一颗 1 M☉ 恒星跨越 5-40 个天文单位，最初有点不稳定。在一项模拟中，行星是在 GI 喷发之前插入的；在另一种情况下，它仅在磁盘进入准稳定 GI 激活状态后才插入，其中 GI 的加热大致平衡了辐射冷却。当行星从一开始就存在时，它自己的尾流会刺激与其强烈相互作用的特定全球模式的增长，并且行星在大约 103 年里向内倾斜 6 个天文单位。在这两种嵌入行星的情况下，有时行星的径向运动很慢并且方向发生变化。在其他时候，当地球似乎与强螺旋模式相互作用时，向内和向外的迁移可能相对较快，在数百年的时间里覆盖了几个天文单位。两种情况下的迁移似乎都在主要低阶模式的内部 Lindblad 共振附近停止。在整个模拟的 GI 活跃阶段，行星轨道偏心率在 0.02 和 0.1 之间快速波动。
Characterization of migration in gravitationally unstable disks is necessary to understand the fate of protoplanets formed by disk instability. As part of a larger study, we are using a three-dimensional radiative hydrodynamics code to investigate how an embedded gas giant planet interacts with a gas disk that undergoes gravitational instabilities (GIs). This Letter presents results from simulations with a Jupiter-mass planet placed in orbit at 25 AU within a 0.14 M☉ disk. The disk spans 5–40 AU around a 1 M☉ star and is initially marginally unstable. In one simulation, the planet is inserted prior to the eruption of GIs; in another, it is inserted only after the disk has settled into a quasi-steady GI-active state, where heating by GIs roughly balances radiative cooling. When the planet is present from the beginning, its own wake stimulates growth of a particular global mode with which it strongly interacts, and the planet plunges inward 6 AU in about 103 years. In both cases with embedded planets, there are times when the planet's radial motion is slow and varies in direction. At other times, when the planet appears to be interacting with strong spiral modes, migration both inward and outward can be relatively rapid, covering several AUs over hundreds of years. Migration in both cases appears to stall near the inner Lindblad resonance of a dominant low-order mode. Planet orbit eccentricities fluctuate rapidly between about 0.02 and 0.1 throughout the GI-active phases of the simulations.
引入平滑粒子流体动力学的混合辐射传递方法
DOI：
10.1111/j.1365-2966.2008.14373.x
发表时间：
2009
影响因子：
4.8
作者：
Forgan D
通讯作者：
Forgan D