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Statements

Subject Item
n2:RIV%2F00216208%3A11320%2F13%3A10174136%21RIV14-GA0-11320___
rdf:type
n13:Vysledek skos:Concept
rdfs:seeAlso
http://dx.doi.org/10.1016/j.icarus.2013.02.002
dcterms:description
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 constraints for 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. 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 constraints for 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.
dcterms:title
The Eos family halo The Eos family halo
skos:prefLabel
The Eos family halo The Eos family halo
skos:notation
RIV/00216208:11320/13:10174136!RIV14-GA0-11320___
n13:predkladatel
n15:orjk%3A11320
n3:aktivita
n4:P n4:Z
n3:aktivity
P(GA13-01308S), Z(MSM0021620860)
n3:cisloPeriodika
2
n3:dodaniDat
n10:2014
n3:domaciTvurceVysledku
n20:6515649
n3:druhVysledku
n16:J
n3:duvernostUdaju
n7:S
n3:entitaPredkladatele
n18:predkladatel
n3:idSjednocenehoVysledku
73086
n3:idVysledku
RIV/00216208:11320/13:10174136
n3:jazykVysledku
n17:eng
n3:klicovaSlova
Migration; Planets; Orbital; Resonances; Dynamics; Asteroids
n3:klicoveSlovo
n9:Migration n9:Orbital n9:Resonances n9:Asteroids n9:Dynamics n9:Planets
n3:kodStatuVydavatele
US - Spojené státy americké
n3:kontrolniKodProRIV
[21869048CBD2]
n3:nazevZdroje
Icarus
n3:obor
n22:BN
n3:pocetDomacichTvurcuVysledku
1
n3:pocetTvurcuVysledku
2
n3:projekt
n21:GA13-01308S
n3:rokUplatneniVysledku
n10:2013
n3:svazekPeriodika
223
n3:tvurceVysledku
Morbidelli, A. Brož, Miroslav
n3:wos
000316923200018
n3:zamer
n14:MSM0021620860
s:issn
0019-1035
s:numberOfPages
6
n8:doi
10.1016/j.icarus.2013.02.002
n12:organizacniJednotka
11320