Interstellar planetesimals: potential seeds for planet formation?

Abstract

We investigate the trapping of interstellar objects during the early stages of star and planet formation. Our results show a very wide range of possible values that will be narrowed down as the population of interstellar objects becomes better characterized. When assuming a background number density of 2$\cdot$10$^{15}$ pc$^{-3}$ (based on 1I/'Oumuamua detection), a velocity dispersion of 30 km/s and an equilibrium size distribution, the number of interstellar objects captured by a molecular cloud and expected to be incorporated to each protoplanetary disk during its formation is O(10$^{9}$) (50 cm-5 m), O(10$^{5}$) (5 m-50 m), O(10$^{2}$) (50 m-500 m), O(10$^{-2}$) (500 m-5 km). After the disk formed, the number of interstellar objects it could capture from the ISM during its lifetime is 6$\cdot$10$^{11}$ (50 cm-5 m), 2$\cdot$10$^{8}$ (5 m-50 m), 6$\cdot$10$^{4}$ (50 m-500 m), 20 (500 m-5 km); in an open cluster where 1% of stars have undergone planet formation, these values increase by a factor of O(10$^{2}$-10$^{3}$). These trapped interstellar objects might be large enough to rapidly grow into larger planetesimals via the direct accretion of the sub-cm sized dust grains in the protoplanetary disk before they drift in due to gas drag, helping overcome the meter-size barrier, acting as "seeds" for planet formation. They should be considered in future star and planet formation models and in the potential spread of biological material across the Galaxy.