论文标题
近距离收获的几乎共兰纳尔的起源
The origins of nearly coplanar, non-resonant systems of close-in super-Earths
论文作者
论文摘要
某些近距离“超级地铁”系统包含五个或更多行星，但在非谐波但紧凑且几乎是共面轨道上。 Kepler-11系统是此类系统的标志性代表。鉴于行星磁盘相互作用被认为对维持如此高度的共同性是必不可少的，这是一个挑战，但这些相同的相同相同的互动总是会导致行星迁移到平均运动共振的链中。在这里，我们通过迁移挖掘了超级地层的动态模拟数据集。只要共振的绝大多数行星对变得动态不稳定，这些模拟与观察到的周期比分布相匹配。当发生不稳定性时，在巨大影响的后期发生了共振，典型的生存系统具有具有明显的相互轨道倾斜的行星对。但是，我们不稳定的模拟子集与Coplanarity，Compactness，Planet-Multiplicity和非谐振状态有关的Kepler-11系统匹配。该子集具有动态不稳定阶段通常比普通系统短得多。如果行星在非常低的轨道倾斜（$ \ Lessim1^\ Circ $）相撞，或者如果碰撞促进有效的轨道倾斜度阻尼，则不稳定的系统可能会保持高度稳定后的稳定后稳定性。 If planetary scattering during the instability takes place at low orbital inclinations ($\text{i}\lesssim1^\circ$), orbital inclinations are barely increased by encounters before planets collide.When planetary scattering pumps orbital inclinations to higher values ($\gtrsim 1^\circ$) planets tend to collide at higher mutual orbital inclinations, but depending on the碰撞合并的几何形状可以有效地抑制。这些地层途径中的每一个都可以产生与开普勒-11系统的类似物。
Some systems of close-in "super-Earths" contain five or more planets on non-resonant but compact and nearly coplanar orbits. The Kepler-11 system is an iconic representative of this class of system. It is challenging to explain their origins given that planet-disk interactions are thought to be essential to maintain such a high degree of coplanarity, yet these same interactions invariably cause planets to migrate into chains of mean motion resonances. Here we mine a large dataset of dynamical simulations of super-Earth formation by migration. These simulations match the observed period ratio distribution as long as the vast majority of planet pairs in resonance become dynamically unstable. When instabilities take place resonances are broken during a late phase of giant impacts, and typical surviving systems have planet pairs with significant mutual orbital inclinations. However, a subset of our unstable simulations matches the Kepler-11 system in terms of coplanarity, compactness, planet-multiplicity and non-resonant state. This subset have dynamical instability phases typically much shorter than ordinary systems. Unstable systems may keep a high degree of coplanarity post-instability if planets collide at very low orbital inclinations ($\lesssim1^\circ$) or if collisions promote efficient damping of orbital inclinations. If planetary scattering during the instability takes place at low orbital inclinations ($\text{i}\lesssim1^\circ$), orbital inclinations are barely increased by encounters before planets collide.When planetary scattering pumps orbital inclinations to higher values ($\gtrsim 1^\circ$) planets tend to collide at higher mutual orbital inclinations, but depending on the geometry of collisions mergers' orbital inclinations may be efficiently damped. Each of these formation pathways can produce analogues to the Kepler-11 system.
