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We perform $N$-body simulations of the early phases of open cluster evolutionincluding a large population of planetesimals, initially arranged inKuiper-belt like discs around each star. Using a new, 4th-order andtime-reversible $N$-body code on Graphics Processing Units (GPUs), we evolvethe whole system under the stellar gravity, i.e. treating planetesimals as testparticles, and consider two types of initial cluster models, similar to IC348and the Hyades, respectively. In both cases, planetesimals can be dynamicallyexcited, transferred between stars or liberated to become free-floating (suchas A/2017 U1 or 'Oumuamua) during the early cluster evolution. We find thatplanetesimals captured from another star are not necessarily dynamicallydistinct from those native to a star. After an encounter both native andcaptured planetesimals can exhibit aligned periastrons, qualitatively similarto that seen in the Solar system and commonly thought to be the signature ofPlanet 9. We discuss the implications of our results for both our Solar systemand exoplanetary systems.

The fate of planetesimal discs in young open clusters: implications for 1I/'Oumuamua, the Kuiper belt, the Oort cloud and more