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Exoplanets have been observed at many stages of their host star's life,including the main sequence (MS), subgiant and red giant branch stages. Also,polluted white dwarfs (WDs) likely represent dynamically active systems at latetimes. Here, we perform 3-body simulations which include realistic post-MSstellar mass loss and span the entire lifetime of exosystems with two massiveplanets, from the endpoint of formation to several Gyr into the WD phase of thehost star. We find that both MS and WD systems experience ejections andstar-planet collisions (Lagrange instability) even if the planet-planetseparation well-exceeds the analytical orbit-crossing (Hill instability)boundary. Consequently, MS-stable planets do not need to be closely-packed toexperience instability during the WD phase. This instability may pollute the WDdirectly through collisions, or, more likely, indirectly through increasedscattering of smaller bodies such as asteroids or comets. Our simulations showthat this instability occurs predominately between tens of Myr to a few Gyrs ofWD cooling.

Simulations of two-planet systems through all phases of stellar evolution: implications for the instability boundary and white dwarf pollution