Orbital Stability of Circumstellar Planets in Binary Systems

Tar archives of simulations for circumstellar planets orbiting a range of host binary stars, where the archives are delineated by the mutual inclination in the filename. Each file in the archive has the assumed mass ratio, mu, and binary eccentricity, e_bin, in the file name as a tuple (mu,e_bin). Tools in python to manipulate and plot the data are provided through a GitHub repository, https://github.com/saturnaxis/ThreeBody_Stability. Inside each file contains a comma delimited text file, where the columns are the initial semimajor axis ratio, the initial phase of the planet, the maximum planetary eccentricity attained over the simulation time, the minimum planetary eccentricity attained over the simulation time, and the collision/escape time. Collisions are defined as collisions with either star, where the escape is when the radial distance of the planet exceeds 200 AU.本数据集包含围绕多类主星双星系统运行的环星行星的数值模拟结果打包归档文件，各归档以文件名中记录的双星轨道相互倾角进行区分。每个归档内的文件，其文件名以(mu,e_bin)元组形式标注了该组模拟对应的质量比μ与双星偏心率e_bin。本数据集配套提供用于数据处理与绘图的Python工具，托管于GitHub仓库https://github.com/saturnaxis/ThreeBody_Stability。每个文件均为逗号分隔的文本文件，各列依次为：初始半长轴比、行星初始相位、模拟时长内行星获得的最大偏心率、模拟时长内行星获得的最小偏心率，以及碰撞或逃逸时刻。其中碰撞定义为行星与任意一颗主星发生碰撞，逃逸则指行星径向距离超过200天文单位（AU）的情形。