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The potential existence of a distant planet ("Planet Nine") in the Solarsystem has prompted a re-think about the evolution of planetary systems. As theSun transitions from a main sequence star into a white dwarf, Jupiter, Saturn,Uranus and Neptune are currently assumed to survive in expanded but otherwiseunchanged orbits. However, a sufficiently-distant and sufficiently-massiveextra planet would alter this quiescent end scenario through the combinedeffects of Solar giant branch mass loss and Galactic tides. Here, I estimatebounds for the mass and orbit of a distant extra planet that would incitefuture instability in systems with a Sun-like star and giant planets withmasses and orbits equivalent to those of Jupiter, Saturn, Uranus and Neptune. Ifind that this boundary is diffuse and strongly dependent on each of thedistant planet's orbital parameters. Nevertheless, I claim that instabilityoccurs more often than not when the planet is as massive as Jupiter andharbours a semimajor axis exceeding about 300 au, or has a mass of asuper-Earth and a semimajor axis exceeding about 3000 au. These results holdfor orbital pericentres ranging from 100 to at least 400 au. This instabilityscenario might represent a common occurrence, as potentially evidenced by theubiquity of metal pollution in white dwarf atmospheres throughout the Galaxy.

The fates of Solar system analogues with one additional distant planet