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The orbital architecture of the Solar System is thought to have been sculptedby a dynamical instability among the giant planets. During the instability aprimordial outer disk of planetesimals was destabilized and ended up onplanet-crossing orbits. Most planetesimals were ejected into interstellar spacebut a fraction were trapped on stable orbits in the Kuiper belt and Oort cloud.We use a suite of N-body simulations to map out the diversity of planetesimals'dynamical pathways. We focus on two processes: tidal disruption from very closeencounters with a giant planet, and loss of surface volatiles from repeatedpassages close to the Sun. We show that the rate of tidal disruption is morethan a factor of two higher for ejected planetesimals than for survivingobjects in the Kuiper belt or Oort cloud. Ejected planetesimals arepreferentially disrupted by Jupiter and surviving ones by Neptune. Given thatthe gas giants contracted significantly as they cooled but the ice giants didnot, taking into account the thermal evolution of the giant planets decreasesthe disruption rate of ejected planetesimals. The frequency of volatile lossand extinction is far higher for ejected planetesimals than for surviving onesand is not affected by the giant planets' contraction. Even if all interstellarobjects were ejected from Solar System-like systems, our analysis suggests thattheir physical properties should be more diverse than those of Solar Systemsmall bodies as a result of their divergent dynamical histories. This isconsistent with the characteristics of the two currently-known interstellarobjects.

Survivor bias: divergent fates of the Solar System's ejected vs. persisting planetesimals