Počet záznamů: 1
Direct iN/i-body Simulations of Satellite Formation around Small Asteroids: Insights from DART's Encounter with the Didymos System
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SYSNO ASEP 0584653 Druh ASEP J - Článek v odborném periodiku Zařazení RIV J - Článek v odborném periodiku Poddruh J Článek ve WOS Název Direct iN/i-body Simulations of Satellite Formation around Small Asteroids: Insights from DART's Encounter with the Didymos System Tvůrce(i) Agrusa, H. F. (US)
Zhang, Y. (US)
Richardson, D.C. (US)
Pravec, Petr (ASU-R) RID, ORCIDCelkový počet autorů 21 Číslo článku 54 Zdroj.dok. The Planetary Science Journal. - : American Astronomical Society
Roč. 5, č. 2 (2024)Poč.str. 30 s. Forma vydání Online - E Jazyk dok. eng - angličtina Země vyd. US - Spojené státy americké Klíč. slova rubble-pile asteroids ; top-shaped asteroids ; dynamical evolution Obor OECD Astronomy (including astrophysics,space science) CEP GA20-04431S GA ČR - Grantová agentura ČR Způsob publikování Open access Institucionální podpora ASU-R - RVO:67985815 UT WOS 001177759100001 EID SCOPUS 85188202633 DOI 10.3847/PSJ/ad206b Anotace 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. Pracoviště Astronomický ústav Kontakt Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Rok sběru 2025 Elektronická adresa https://hdl.handle.net/11104/0353117
Počet záznamů: 1