  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 late
times. Here, we perform 3-body simulations which include realistic post-MS
stellar mass loss and span the entire lifetime of exosystems with two massive
planets, from the endpoint of formation to several Gyr into the WD phase of the
host star. We find that both MS and WD systems experience ejections and
star-planet collisions (Lagrange instability) even if the planet-planet
separation well-exceeds the analytical orbit-crossing (Hill instability)
boundary. Consequently, MS-stable planets do not need to be closely-packed to
experience instability during the WD phase. This instability may pollute the WD
directly through collisions, or, more likely, indirectly through increased
scattering of smaller bodies such as asteroids or comets. Our simulations show
that this instability occurs predominately between tens of Myr to a few Gyrs of
WD cooling.
