Interstellar Objects Follow the Collapse of Molecular Clouds

The Astrophysical Journal, vol. 921, pp. 168

Abstract

Abstract Interstellar objects (ISOs), the parent population of 1i/‘Oumuamua and 2i/Borisov, are abundant in the interstellar medium of the Milky Way. This means that the interstellar medium, including molecular-cloud regions, has three components: gas, dust, and ISOs. From observational constraints of the field density of ISOs drifting in the solar neighborhood, we infer that a typical molecular cloud of 10 pc diameter contains some 1018 ISOs. At typical sizes ranging from hundreds of meters to tens of kilometers, ISOs are entirely decoupled from the gas dynamics in these molecular clouds. Here we address the question of whether ISOs can follow the collapse of molecular clouds. We perform low-resolution simulations of the collapse of molecular clouds containing initially static ISO populations toward the point where stars form. In this proof-of-principle study, we find that the interstellar objects definitely follow the collapse of the gas—and many become bound to the new-forming numerical approximations to future stars (sinks). At minimum, 40% of all sinks have one or more ISO test particles gravitationally bound to them for the initial ISO distributions tested here. This value corresponds to at least 1010 actual ISOs being bound after three initial freefall times. Thus, ISOs are a relevant component of star formation. We find that more massive sinks bind disproportionately large fractions of the initial ISO population, implying competitive capture of ISOs. Sinks can also be solitary, as their ISOs can become unbound again—particularly if sinks are ejected from the system. Emerging planetary systems will thus develop in remarkably varied environments, ranging from solitary to richly populated with bound ISOs.

Authors 4

1. Susanne Pfalzner corresponding

   Forschungszentrum Jülich · Max Planck Institute for Radio Astronomy · Jülich Supercomputing Centre

   Affiliation as printed

   Jülich Supercomputing Center, Forschungszentrum Jülich, D-52428 Jülich, Germany; s.pfalzner@fz-juelich

   Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany

2. Dylan Paterson

   University of Canterbury

   Affiliation as printed

   School of Physical and Chemical Sciences ∣ Te Kura Matū, University of Canterbury, Private Bag 4800, Christchurch 8140, New Zealand

3. Michele T. Bannister

   University of Canterbury

   Affiliation as printed

   School of Physical and Chemical Sciences ∣ Te Kura Matū, University of Canterbury, Private Bag 4800, Christchurch 8140, New Zealand

4. Simon Portegies Zwart Aachen Leiden Observatory

   Leiden University · Leiden Observatory

   Affiliation as printed

   Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands