PECULIAR EUPHROSYNE

dc.contributorUniversidade Estadual Paulista (Unesp)
dc.contributorUniv Namur
dc.contributorUniv Paris 06
dc.creatorCarruba, V. [UNESP]
dc.creatorAljbaae, S. [UNESP]
dc.creatorSouami, D.
dc.date2015-03-18T15:54:35Z
dc.date2015-03-18T15:54:35Z
dc.date2014-09-01
dc.date.accessioned2023-09-12T03:02:39Z
dc.date.available2023-09-12T03:02:39Z
dc.identifierhttp://dx.doi.org/10.1088/0004-637X/792/1/46
dc.identifierAstrophysical Journal. Bristol: Iop Publishing Ltd, v. 792, n. 1, 15 p., 2014.
dc.identifier0004-637X
dc.identifierhttp://hdl.handle.net/11449/116970
dc.identifier10.1088/0004-637X/792/1/46
dc.identifierWOS:000341172100046
dc.identifier4750709016042276
dc.identifier.urihttps://repositorioslatinoamericanos.uchile.cl/handle/2250/8766455
dc.descriptionThe asteroid (31) Euphrosyne is the largest body of its namesake family, and it contains more than 99% of the family mass. Among large asteroid families, the Euphrosyne group is peculiar because of its quite steep size-frequency distribution (SFD), significantly depleted in large-and medium-sized asteroids (8 < D < 12 km). The current steep SFD of the Euphrosyne family has been suggested to be the result of a grazing impact in which only the farthest, smallest members failed to accrete. The Euphrosyne family is, however, also very peculiar because of its dynamics: near its center it is crossed by the nu(6) = g - g(6) linear secular resonance, and it hosts the largest population (140 bodies) of asteroids in nu(6) antialigned librating states (or Tina-like asteroids) in the main belt. In this work we investigated the orbital evolution of newly obtained members of the dynamical family, with an emphasis on its interaction with the nu(6) resonance. Because of its unique resonant configuration, large-and medium-sized asteroids tend to migrate away from the family orbital region faster than small-sized objects, which were ejected farther away from the family center. As a consequence, the SFD of the Euphrosyne family becomes steeper in time with a growing depletion in the number of the largest family members. We estimate that the current SFD could be attained from a typical, initial SFD on timescales of 500 Myr, consistent with estimates of the family age obtained with other independent methods.
dc.descriptionFundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)
dc.descriptionConselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)
dc.descriptionNational Aeronautics and Space Administration
dc.descriptionPlanetary Science Division of the National Aeronautics and Space Administration
dc.descriptionUniv Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP, Brazil
dc.descriptionUniv Namur, Dept Math, Namur Ctr Complex Syst, NAXYS, B-5000 Namur, Belgium
dc.descriptionUniv Paris 06, F-75005 Paris, France
dc.descriptionUniv Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP, Brazil
dc.descriptionCNPq: 305453/2011-4
dc.description11/19863-3
dc.description13/15357-1
dc.description14/06762-2
dc.format15
dc.languageeng
dc.publisherIop Publishing Ltd
dc.relationAstrophysical Journal
dc.relation5.551
dc.rightsAcesso restrito
dc.sourceWeb of Science
dc.subjectcelestial mechanics
dc.subjectminor planets, asteroids: general
dc.subjectminor planets, asteroids: individual (Euphrosyne)
dc.titlePECULIAR EUPHROSYNE
dc.typeArtigo


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