论文标题
二进制恒星系统行星运动的稳定性
Stability of Planetary Motion in Binary Star Systems
论文作者
论文摘要
我们考虑了二进制恒星系统中有限质量行星的稳定性问题。我们为S型的行星轨道选择了一组大量的初始条件，以执行高精度和非常扩展的时间整合。 对于我们的数值集成，我们诉诸使用第15阶集成方案（IAS15，在篮板框架内可用），为长期时间集成提供了最佳解决方案。我们估计了不同类型的不稳定性的概率：行星与从二进制恒星系统弹出的主要或次要恒星或行星的碰撞。我们确认并概括了巨大的行星，临界半轴轴对Holman and Wiegert（1999）已经发现的二进制的偏心率和质量比的依赖性。根据Musielak等人提出的分类，我们还能够选择大量仅“边缘”稳定的轨道。 （2005）。 A，这项工作的自然扩展是对传球恒星诱导的扰动的影响的研究，就像经常发生在星团中一样。该分析的目标之一是研究一个可能在两颗恒星之一周围稳定的S型轨道上的行星可以转移到稳定的P型轨道（或Viceversa）的可能性。我们进行了一系列4500多个散射实验，这些实验具有不同的小星形群中典型相遇的不同初始条件。我们在扰动后发现了系统的一些有趣的行为，并展示了从内部（S型）稳定轨道向电路（P-Type）（P-Type）（和反之亦然）的过渡如何具有很低（但非无效）概率。
We considered the problem of stability for planets of finite mass in binary star systems. We selected a huge set of initial conditions for planetary orbits of the S-type, to perform high precision and very extended in time integrations. For our numerical integrations, we resorted to the use of a 15th order integration scheme (IAS15, available within the REBOUND framework), that provides an optimal solution for long-term time integrations. We estimated the probability of different types of instability: planet collisions with the primary or secondary star or planet ejected away from the binary star system. We confirm and generalize to massive planets the dependence of the critical semi-major axis on eccentricity and mass ratio of the binary already found by Holman and Wiegert (1999). We were also able to pick a significant number of orbits that are only `marginally' stable, according to the classification introduced by Musielak et al. (2005). A, natural, extension of this work has been the study of the effect of perturbations induced to circumbinary planet motion by a passing-by star, like it often happens in a star cluster. One of the targets of this analysis is the investigation of the possibility that a planet, formerly on a stable S-type orbit around one of the two stars, could transit to a stable P-type orbit (or viceversa). We performed a series of more than 4500 scattering experiments with different initial conditions typical of encounters in small star clusters. We found some interesting behaviors of the systems after perturbation and showed how a transition from an inner (S-type) stable orbit to a circumbinary (P-type) (and vice-versa) has a very low (but non null) probability.
