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Statements

Subject Item
n2:RIV%2F00216208%3A11320%2F14%3A10286599%21RIV15-MSM-11320___
rdf:type
n16:Vysledek skos:Concept
rdfs:seeAlso
http://dx.doi.org/10.1016/j.icarus.2014.07.016
dcterms:description
In this work, we construct a new model for the collisional evolution of the main asteroid belt. Our goals are to test the scaling law of Benz and Asphaug (Benz, W., Asphaug, E. [1999]. Icarus, 142, 5-20) and ascertain if it can be used for the whole belt. We want to find initial size-frequency distributions (SEDs) for the considered six parts of the belt (inner, middle, %22pristine%22, outer, Cybele zone, high-inclination region) and to verify if the number of synthetic asteroid families created during the simulation matches the number of observed families as well. We used new observational data from the WISE satellite (Masiero et al., 2011) to construct the observed SFDs. We simulate mutual collisions of asteroids with a modified version of the Boulder code (Morbidelli, A., et al. [2009]. Icarus, 204, 558-573), where the results of hydrodynamic (SPH) simulations of Durda et al. (Durda, D.D., et al. 120071 Icarus, 498-516) and Benavidez et al. (Benavidez, P.G., et al. [2012]. 219, 57-76) are included. Because material characteristics can significantly affect breakups, we created two models - for monolithic asteroids and for rubble-piles. To explain the observed SFDs in the size range D = 1 to 10 km we have to also account for dynamical depletion due to the Yarkovsky effect. The assumption of (purely) rubble-pile asteroids leads to a significantly worse fit to the observed data, so that we can conclude that majority of main-belt asteroids are rather monolithic. Our work may also serve as a motivation for further SPH simulations of disruptions of smaller targets (with a parent body size of the order of 1 km). In this work, we construct a new model for the collisional evolution of the main asteroid belt. Our goals are to test the scaling law of Benz and Asphaug (Benz, W., Asphaug, E. [1999]. Icarus, 142, 5-20) and ascertain if it can be used for the whole belt. We want to find initial size-frequency distributions (SEDs) for the considered six parts of the belt (inner, middle, %22pristine%22, outer, Cybele zone, high-inclination region) and to verify if the number of synthetic asteroid families created during the simulation matches the number of observed families as well. We used new observational data from the WISE satellite (Masiero et al., 2011) to construct the observed SFDs. We simulate mutual collisions of asteroids with a modified version of the Boulder code (Morbidelli, A., et al. [2009]. Icarus, 204, 558-573), where the results of hydrodynamic (SPH) simulations of Durda et al. (Durda, D.D., et al. 120071 Icarus, 498-516) and Benavidez et al. (Benavidez, P.G., et al. [2012]. 219, 57-76) are included. Because material characteristics can significantly affect breakups, we created two models - for monolithic asteroids and for rubble-piles. To explain the observed SFDs in the size range D = 1 to 10 km we have to also account for dynamical depletion due to the Yarkovsky effect. The assumption of (purely) rubble-pile asteroids leads to a significantly worse fit to the observed data, so that we can conclude that majority of main-belt asteroids are rather monolithic. Our work may also serve as a motivation for further SPH simulations of disruptions of smaller targets (with a parent body size of the order of 1 km).
dcterms:title
A six-part collisional model of the main asteroid belt A six-part collisional model of the main asteroid belt
skos:prefLabel
A six-part collisional model of the main asteroid belt A six-part collisional model of the main asteroid belt
skos:notation
RIV/00216208:11320/14:10286599!RIV15-MSM-11320___
n3:aktivita
n10:Z n10:S n10:P
n3:aktivity
P(GA13-01308S), S, Z(MSM0021620860)
n3:cisloPeriodika
říjen
n3:dodaniDat
n17:2015
n3:domaciTvurceVysledku
n19:6191576 n19:6515649
n3:druhVysledku
n12:J
n3:duvernostUdaju
n4:S
n3:entitaPredkladatele
n18:predkladatel
n3:idSjednocenehoVysledku
1185
n3:idVysledku
RIV/00216208:11320/14:10286599
n3:jazykVysledku
n14:eng
n3:klicovaSlova
Solar System; Origin; Collisional physics; Asteroids
n3:klicoveSlovo
n8:Collisional%20physics n8:Origin n8:Asteroids n8:Solar%20System
n3:kodStatuVydavatele
US - Spojené státy americké
n3:kontrolniKodProRIV
[5C5F8799BCAD]
n3:nazevZdroje
Icarus
n3:obor
n7:BN
n3:pocetDomacichTvurcuVysledku
2
n3:pocetTvurcuVysledku
3
n3:projekt
n13:GA13-01308S
n3:rokUplatneniVysledku
n17:2014
n3:svazekPeriodika
241
n3:tvurceVysledku
Cibulková, Helena Benavidez, P. G. Brož, Miroslav
n3:wos
000343617900026
n3:zamer
n5:MSM0021620860
s:issn
0019-1035
s:numberOfPages
15
n20:doi
10.1016/j.icarus.2014.07.016
n15:organizacniJednotka
11320