Direct iN/i-body Simulations of Satellite Formation around Small Asteroids: Insights from DART's Encounter with the Didymos System

0584653 - ASÚ 2025 RIV US eng J - Journal Article
Agrusa, H. F. - Zhang, Y. - Richardson, D.C. - Pravec, Petr … Total 21 authors
Direct iN/i-body Simulations of Satellite Formation around Small Asteroids: Insights from DART's Encounter with the Didymos System.
The Planetary Science Journal. Roč. 5, č. 2 (2024), č. článku 54. E-ISSN 2632-3338
R&D Projects: GA ČR(CZ) GA20-04431S
Institutional support: RVO:67985815
Keywords : rubble-pile asteroids * top-shaped asteroids * dynamical evolution
OECD category: Astronomy (including astrophysics,space science)
Impact factor: 3.4, year: 2022
Method of publishing: Open access

We explore binary asteroid formation by spin-up and rotational disruption considering the NASA DART mission's encounter with the Didymos-Dimorphos binary, which was the first small binary visited by a spacecraft. Using a suite of N-body simulations, we follow the gravitational accumulation of a satellite from meter-sized particles following a mass-shedding event from a rapidly rotating primary. The satellite's formation is chaotic, as it undergoes a series of collisions, mergers, and close gravitational encounters with other moonlets, leading to a wide range of outcomes in terms of the satellite's mass, shape, orbit, and rotation state. We find that a Dimorphos-like satellite can form rapidly, in a matter of days, following a realistic mass-shedding event in which only similar to 2%-3% of the primary's mass is shed. Satellites can form in synchronous rotation due to their formation near the Roche limit. There is a strong preference for forming prolate (elongated) satellites, although some simulations result in oblate spheroids like Dimorphos. The distribution of simulated secondary shapes is broadly consistent with other binary systems measured through radar or lightcurves. Unless Dimorphos's shape is an outlier, and considering the observational bias against lightcurve-based determination of secondary elongations for oblate bodies, we suggest there could be a significant population of oblate secondaries. If these satellites initially form with elongated shapes, a yet-unidentified pathway is needed to explain how they become oblate. Finally, we show that this chaotic formation pathway occasionally forms asteroid pairs and stable triples, including coorbital satellites and satellites in mean-motion resonances.
Permanent Link: https://hdl.handle.net/11104/0353117