Satellite Formation around the Largest Asteroids

Kód výsledku v 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>

Výsledek na webu

<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>

Jazyk výsledku

angličtina

Název v původním jazyce

Satellite Formation around the Largest Asteroids

Popis výsledku v původním jazyce

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.

Název v anglickém jazyce

Satellite Formation around the Largest Asteroids

Popis výsledku anglicky

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.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA22-17783S" target="_blank" >GA22-17783S: V množství je síla - Využití sítě dalekohledů Unistellar eVscope občanských vědců pro studium planetek</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2025

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astrophysical Journal Letters

ISSN

2041-8205

e-ISSN

2041-8213

Svazek periodika

986

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

19

Strana od-do

L12

Kód UT WoS článku

001503477700001

EID výsledku v databázi Scopus

2-s2.0-105007734598