论文标题
用外球门动力学约束原球门磁盘：开普勒-419作为示例
Constraining protoplanetary disks with exoplanetary dynamics: Kepler-419 as an example
论文作者
论文摘要
我们研究了Kepler-419的起源，Kepler-419是一个具有近似抗对准的Apsidal取向的奇特系统，具有两个近乎共同的气体和高度偏心的气体巨头，并使用该系统对其出生原理磁盘的特性放置约束。我们遵循Petrovich，Wu和Ali-Dib（2019）提出的提案，即这些行星已被放在这些轨道上，这是散发大规模磁盘的前进作用的自然结果，并通过使用直接的N体模拟和模型来扩展其用于包括光电蒸发在内的气盘的演化。基于参数空间探索，我们发现，要重现系统，初始磁盘质量必须至少为95 m_jup，并在至少10^4 yr的时间表上消散。该质量与观察到的磁盘质量分布的上端一致，并且耗散时间尺度与光蒸发模型一致。我们使用简化的1D薄磁盘模型研究了此类磁盘的性能，并表明它们在重力稳定上是重力稳定的，这表明这两个行星必须通过核心积聚形成，从而容易磁盘迁移。因此，我们最终研究了该机制对外行星半轴的敏感性，并发现附近的7：1、8：1和9：1的均值平均动作共振可以完全淬灭这种机制，而甚至更高阶的共振也会显着影响该系统。假设这两个行星避免了这些高阶共振和/或紧密相遇，则动力学似乎对行星C半轴轴不敏感，因此由磁盘驱动的轨道迁移。
We investigate the origins of Kepler-419, a peculiar system hosting two nearly coplanar and highly eccentric gas giants with apsidal orientations librating around anti-alignment, and use this system to place constraints on the properties of their birth protoplanetary disk. We follow the proposal by Petrovich, Wu, & Ali-Dib (2019) that these planets have been placed on these orbits as a natural result of the precessional effects of a dissipating massive disk and extend it by using direct N-body simulations and models for the evolution of the gas disks, including photoevaporation. Based on a parameter space exploration, we find that in order to reproduce the system the initial disk mass had to be at least 95 M_Jup and dissipate on a timescale of at least 10^4 yr. This mass is consistent with the upper end of the observed disk masses distribution, and the dissipation timescale is consistent with photoevaporation models. We study the properties of such disks using simplified 1D thin disk models and show that they are gravitationally stable, indicating that the two planets must have formed via core accretion and thus prone to disk migration. We hence finally investigate the sensitivity of this mechanism to the outer planet's semi major axis, and find that the nearby 7:1, 8:1, and 9:1 mean-motion resonances can completely quench this mechanism, while even higher order resonances can also significantly affect the system. Assuming the two planets avoid these high order resonances and/or close encounters, the dynamics seems to be rather insensitive to planet c semi major axis, and thus orbital migration driven by the disk.
