Direct N-body simulations of satellite formation around small asteroids: Insights from DART's encounter with the Didymos system
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F24%3A00584653" target="_blank" >RIV/67985815:_____/24:00584653 - isvavai.cz</a>
Result on the web
<a href="https://hdl.handle.net/11104/0353117" target="_blank" >https://hdl.handle.net/11104/0353117</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.3847/PSJ/ad206b" target="_blank" >10.3847/PSJ/ad206b</a>
Alternative languages
Result language
angličtina
Original language name
Direct N-body simulations of satellite formation around small asteroids: Insights from DART's encounter with the Didymos system
Original language description
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.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/GA20-04431S" target="_blank" >GA20-04431S: Physical and dynamical properties of space mission target asteroids, and their evolutionary paths</a><br>
Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2024
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
The Planetary Science Journal
ISSN
2632-3338
e-ISSN
2632-3338
Volume of the periodical
5
Issue of the periodical within the volume
2
Country of publishing house
US - UNITED STATES
Number of pages
30
Pages from-to
54
UT code for WoS article
001177759100001
EID of the result in the Scopus database
2-s2.0-85188202633