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We know that planetary systems are just as common around white dwarfs asaround main sequence stars. However, self-consistently linking a planetarysystem across these two phases of stellar evolution through the violent giantbranch poses computational challenges, and previous studies restrictedarchitectures to equal-mass planets. Here, we remove this constraint andperform over 450 numerical integrations over a Hubble time (14 Gyr) of packedplanetary systems with unequal-mass planets. We characterize the resultingtrends as a function of planet order and mass. We find that intrusive radialincursions in the vicinity of the white dwarf become less likely as thedispersion amongst planet masses increases. The orbital meandering which maysustain a sufficiently dynamic environment around a white dwarf to explainobservations is more dependent on the presence of terrestrial-mass planets thanany variation in planetary mass. Triggering unpacking or instability during thewhite dwarf phase is comparably easy for systems of unequal-mass planets andsystems of equal-mass planets; instabilities during the giant branch phaseremain rare and require fine-tuning of initial conditions. We list the keydynamical features of each simulation individually as a potential guide forupcoming discoveries.

Full-lifetime simulations of multiple unequal-mass planets across all phases of stellar evolution