Satellite Formation around the Largest Asteroids
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F25%3A10511116" target="_blank" >RIV/00216208:11320/25:10511116 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=ypaIFQgXhn" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=ypaIFQgXhn</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.3847/2041-8213/adc562" target="_blank" >10.3847/2041-8213/adc562</a>
Alternative languages
Result language
angličtina
Original language name
Satellite Formation around the Largest Asteroids
Original language description
Satellites around large asteroids are preferentially found among those with the most rapid rotation and elongated shape. The taxonomic statistics are similarly skewed; in total, 13 asteroids larger than 100 km are known to have satellites, but none have been discovered among S-type asteroids. Previous modeling suggests that satellites could be generated by impacts, but spin and shape have never been tracked in models to relate collisional circumstances with those two observed properties concerning the primary. Here we show, by combining simulations of impacts into porous low-density asteroids, their subsequent disruption, reaccumulation, and long-term satellite stability, a direct pathway for the formation of satellites. The immediate distortion and elongation of a rotating target body provide a launching point for some debris distinct from simple ballistic ejecta trajectories. The debris that are found to originate from the distorted long axis is sourced primarily from 10 to 20 km below the surface and can be placed directly onto eccentric orbits with sufficiently large pericenter distances that avoid rapid reimpact. The specific energy and resultant total mass loss in satellite-forming collisions are not constraining, which explains the observed lack of correlation between asteroids with satellites and those that are part of large asteroid families.
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/GA22-17783S" target="_blank" >GA22-17783S: There is strength in numbers - Exploitation of Unistellar eVscope network of citizen scientiest for the study of asteroids</a><br>
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Others
Publication year
2025
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Astrophysical Journal Letters
ISSN
2041-8205
e-ISSN
2041-8213
Volume of the periodical
986
Issue of the periodical within the volume
1
Country of publishing house
US - UNITED STATES
Number of pages
19
Pages from-to
L12
UT code for WoS article
001503477700001
EID of the result in the Scopus database
2-s2.0-105007734598