The Eos family halo
Identifikátory výsledku
Kód výsledku v IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F13%3A10174136" target="_blank" >RIV/00216208:11320/13:10174136 - isvavai.cz</a>
Výsledek na webu
<a href="http://dx.doi.org/10.1016/j.icarus.2013.02.002" target="_blank" >http://dx.doi.org/10.1016/j.icarus.2013.02.002</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1016/j.icarus.2013.02.002" target="_blank" >10.1016/j.icarus.2013.02.002</a>
Alternativní jazyky
Jazyk výsledku
angličtina
Název v původním jazyce
The Eos family halo
Popis výsledku v původním jazyce
We study K-type asteroids in the broad surroundings of the Eos family because they seem to be intimately related, according to their colours measured by the Sloan Digital Sky Survey. Such 'halos' of asteroid families have been rarely used as constraintsfor dynamical studies to date. We explain its origin as bodies escaping from the family 'core' due to the Yarkovsky semimajor-axis drift and interactions with gravitational resonances, mostly with the 9/4 mean-motion resonance with Jupiter at 3.03 AU. Our N-body dynamical model allows us to independently estimate the age of the family 1.5-1.9 Gyr. This is approximately in agreement with the previous age estimate by Vokrouhlicky et al. (2006) based on a simplified model (which accounts only for changes of semimajor axis). We can also constrain the geometry of the disruption event which had to occur at the true anomaly f similar or equal to 120-180.
Název v anglickém jazyce
The Eos family halo
Popis výsledku anglicky
We study K-type asteroids in the broad surroundings of the Eos family because they seem to be intimately related, according to their colours measured by the Sloan Digital Sky Survey. Such 'halos' of asteroid families have been rarely used as constraintsfor dynamical studies to date. We explain its origin as bodies escaping from the family 'core' due to the Yarkovsky semimajor-axis drift and interactions with gravitational resonances, mostly with the 9/4 mean-motion resonance with Jupiter at 3.03 AU. Our N-body dynamical model allows us to independently estimate the age of the family 1.5-1.9 Gyr. This is approximately in agreement with the previous age estimate by Vokrouhlicky et al. (2006) based on a simplified model (which accounts only for changes of semimajor axis). We can also constrain the geometry of the disruption event which had to occur at the true anomaly f similar or equal to 120-180.
Klasifikace
Druh
J<sub>x</sub> - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)
CEP obor
BN - Astronomie a nebeská mechanika, astrofyzika
OECD FORD obor
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Návaznosti výsledku
Projekt
<a href="/cs/project/GA13-01308S" target="_blank" >GA13-01308S: Dynamika malých těles sluneční soustavy</a><br>
Návaznosti
Z - Vyzkumny zamer (s odkazem do CEZ)
Ostatní
Rok uplatnění
2013
Kód důvěrnosti údajů
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Údaje specifické pro druh výsledku
Název periodika
Icarus
ISSN
0019-1035
e-ISSN
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Svazek periodika
223
Číslo periodika v rámci svazku
2
Stát vydavatele periodika
US - Spojené státy americké
Počet stran výsledku
6
Strana od-do
844-849
Kód UT WoS článku
000316923200018
EID výsledku v databázi Scopus
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