Pure three-body simulations: initial planet location relative to the primary star’s Hill radius, a_p,0/R_Hill,1, versus the mean value of the planet’s acceleration due to the secondary star (${\ddot{x}}_{\text{secondary}}$) normalized by the acceleration due to the primary star (${\ddot{x}}_{\text{primary}}$). The dashed gray and black lines indicate orbital distances of 1/3 and 1/2 of R_Hill,1, respectively. The dotted-dashed gray line indicates where ${\ddot{x}}_{\text{secondary}}={\ddot{x}}_{\text{primary}}$. Blue circle markers represent planets that remain in the system, orange crosses indicate planets that are lost due to either ejection or instability due to a close encounter with the central star. We note that some blue markers are covered by the orange ones.