恒星飞掠对行星系的影响：星周盘阻尼效应的三维模拟
Effects of stellar flybys on planetary systems: 3D modeling of the circumstellar disks damping effects
摘要：
星团中的恒星飞掠被怀疑会影响行星系的轨道结构，导致偏心率激发和行星轨道与恒星赤道面之间的轨道不对准。我们探讨是否在行星的轨道要素的脉冲变化，所造成的双曲线恒星飞越，可以完全阻尼周围的恒星盘。分散星团所需的时间实际上与星周盘的寿命相当。我们在3D中模拟了一个由太阳型恒星组成的系统，该恒星被一个低密度盘包围，其中嵌入了一颗巨大的行星，第二颗恒星以双曲线的轨道与第二颗恒星相遇，第二颗恒星具有相似的质量和自己的盘。我们专注于极端的配置，一个非常深的恒星飞越扰动外部轨道上的类木行星。这可以完全测试磁盘消除恒星相遇影响的能力。我们发现，在恒星飞掠过程中的磁盘的质量损失量小于在2D模型中，其中一个单一的磁盘被认为是由于在遇到两个磁盘之间的质量交换。偏心率的阻尼比2D模型中的阻尼稍快，并且它发生在几千年量级的时间尺度上。大约10^4年后，在行星系统中留下的唯一痕迹是恒星赤道面和行星轨道之间的一个小于9度的小偏差。在一个现实的模型的基础上的三维模拟的恒星-行星-磁盘的相互作用，我们发现，恒星飞掠不能激发显着的偏心率和倾角的行星在星团。行星所在的星周盘在很短的时间尺度上阻尼了任何恒星相遇过程中产生的两个轨道参数的所有阶跃变化。所有过去的遭遇记录都被删除了。
英文摘要：
Stellar flybys in star clusters are suspected to affect the orbital architecture of planetary systems causing eccentricity excitation and orbital misalignment between the planet orbit and the equatorial plane of the star. We explore whether the impulsive changes in the orbital elements of planets, caused by an hyperbolic stellar flyby, can be fully damped by the circumstellar disk surrounding the star. The time required to disperse stellar clusters is in fact comparable to circumstellar disk's lifetime. We have modelled in 3D a system made of a solar type star surrounded by a low density disk with a giant planet embedded in it approached on a hyperbolic encounter trajectory by a second star, of similar mass and with its own disk. We focus on extreme configurations where a very deep stellar flyby perturbs a Jovian planet on an external orbit. This allows to test in full the ability of the disk to erase the effects of the stellar encounter. We find that the amount of mass lost by the disk during the stellar flyby is less than in 2D models where a single disk was considered due to the mass exchange between the two disks at the encounter. The damping in eccentricity is slightly faster than in 2D models and it occurs on timescales of the order of a few kyr. The only trace of the flyby left in the planet system, after about 10^4 yr, is a small misalignment, lower than 9 degrees, between the star equatorial plane and the planet orbit. In a realistic model based on 3D simulations of star--planet--disk interactions, we find that stellar flybys cannot excite significant eccentricities and inclinations of planets in stellar clusters. The circumstellar disks hosting the planets damp on a short timescale all the step changes in the two orbital parameters produced during any stellar encounter. All records of past encounters are erased.
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