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Authordc.contributor.authorPinilla Alonso, N. 
Authordc.contributor.authorAlvarez Candal, A. es_CL
Authordc.contributor.authorMelita, M. D. es_CL
Authordc.contributor.authorLorenzi, V. es_CL
Authordc.contributor.authorLicandro, J. es_CL
Authordc.contributor.authorCarvano, J. es_CL
Authordc.contributor.authorLazzaro, D. es_CL
Authordc.contributor.authorCarraro, Giovanni es_CL
Authordc.contributor.authorAlí Lagoa, V. es_CL
Authordc.contributor.authorCosta Hechenleitner, Edgardo es_CL
Authordc.contributor.authorHasselmann, P. H. es_CL
Admission datedc.date.accessioned2014-01-27T19:53:45Z
Available datedc.date.available2014-01-27T19:53:45Z
Publication datedc.date.issued2013
Cita de ítemdc.identifier.citationA&A 550, A13 (2013)en_US
Identifierdc.identifier.otherDOI: 10.1051/0004-6361/201220030
Identifierdc.identifier.urihttps://repositorio.uchile.cl/handle/2250/126298
General notedc.descriptionArtículo de publicación ISIen_US
Abstractdc.description.abstractMost of the objects in the trans-Neptunian belt (TNb) and related populations move in prograde orbits with low eccentricity and inclination. However, the list of icy minor bodies moving in orbits with an inclination above 40 has increased in recent years. The origin of these bodies, and in particular of those objects in retrograde orbits, is not well determined, and di erent scenarios are considered, depending on their inclination and perihelion. In this paper, we present new observational and dynamical data of two objects in retrograde orbits, 2008 YB3 and 2005 VD.We find that the surface of these extreme objects is depleted of ices and does not contain the “ultra-red” matter typical of some Centaurs. Despite small di erences, these objects share common colors and spectral characteristics with the Trojans, comet nuclei, and the group of grey Centaurs. All of these populations are supposed to be covered by a mantle of dust responsible for their reddish-to-neutral color. To investigate if the surface properties and dynamical evolution of these bodies are related, we integrate their orbits for 108 years to the past. We find a remarkable di erence in their dynamical evolutions: 2005 VD’s evolution is dominated by a Kozai resonance with planet Jupiter while that of 2008 YB3 is dominated by close encounters with planets Jupiter and Saturn. Our models suggest that the immediate site of provenance of 2005 VD is the in the Oort Cloud, whereas for 2008 YB3 it is in the trans-Neptunian region. Additionally, the study of their residence time shows that 2005 VD has spent a larger lapse of time moving in orbits in the region of the giant planets than 2008 YB3. Together with the small di erences in color between these two objects, with 2005 VD being more neutral than 2008 YB3, this fact suggests that the surface of 2005 VD has su ered a higher degree of processing, which is probably related to cometary activity episodes.en_US
Lenguagedc.language.isoenen_US
Publisherdc.publisherEDP Sciencesen_US
Type of licensedc.rightsAttribution-NonCommercial-NoDerivs 3.0 Chile*
Link to Licensedc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/cl/*
Keywordsdc.subjectKuiper belt objects: individual: 2008 YB3en_US
Títulodc.titleSurface composition? and dynamical evolution of two retrograde objects in the outer solar system: 2008 YB3 and 2005 VDen_US
Document typedc.typeArtículo de revista


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Except where otherwise noted, this item's license is described as Attribution-NonCommercial-NoDerivs 3.0 Chile