论文标题
高度偏心二进制的极地行星是最稳定的
Polar planets around highly eccentric binaries are the most stable
论文作者
论文摘要
我们研究了一个非零质量，近距离圆形轨道行星围绕偏心轨道二进制的轨道稳定性，用于二进制偏心率的各种初始值，二进制质量分数，行星质量，行星半高轴和行星半轴和行星的倾斜度，并通过数值模拟覆盖$ 5 \ times $ 5 \ times times times 10^4 $ barinary Orbits。对于小二元偏心率，延伸到最接近二元的轨道（最稳定轨道）的稳定轨道几乎是逆行和循环的。对于高二元偏心率，最稳定的轨道是高度倾斜的，并在所谓的广义极性轨道附近，这是固定在二进制轨道框架中的固定轨道。对于更极端的质量比二进制文件，具有行星质量和初始倾斜度的稳定区域的尺寸（定义为初始轨道半径和倾斜度）的变化更大，尤其是对于低二元偏心率。对于低二进制偏心，即使在大轨道半径（分隔$> 5 \，a _ {\ rm b} $）中，倾斜的行星轨道也可能不稳定。与不等的质量二进制相比，不稳定行星的逃生时间通常较短。我们的结果对环形行星的形成和进化具有影响，将有助于理解未来的环球行星观测。
We study the orbital stability of a non-zero mass, close-in circular orbit planet around an eccentric orbit binary for various initial values of the binary eccentricity, binary mass fraction, planet mass, planet semi--major axis, and planet inclination by means of numerical simulations that cover $5 \times 10^4$ binary orbits. For small binary eccentricity, the stable orbits that extend closest to the binary (most stable orbits) are nearly retrograde and circulating. For high binary eccentricity, the most stable orbits are highly inclined and librate near the so-called generalised polar orbit which is a stationary orbit that is fixed in the frame of the binary orbit. For more extreme mass ratio binaries, there is a greater variation in the size of the stability region (defined by initial orbital radius and inclination) with planet mass and initial inclination, especially for low binary eccentricity. For low binary eccentricity, inclined planet orbits may be unstable even at large orbital radii (separation $> 5 \,a_{\rm b}$). The escape time for an unstable planet is generally shorter around an equal mass binary compared with an unequal mass binary. Our results have implications for circumbinary planet formation and evolution and will be helpful for understanding future circumbinary planet observations.
