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.