Surface composition and dynamical evolution of two retrograde objects in the outer solar system: 2008 YB3 and 2005 VD

Most 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 particula...

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Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v550_n_p_PinillaAlonso
http://hdl.handle.net/20.500.12110/paper_00046361_v550_n_p_PinillaAlonso
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spelling paper:paper_00046361_v550_n_p_PinillaAlonso2023-06-08T14:28:02Z Surface composition and dynamical evolution of two retrograde objects in the outer solar system: 2008 YB3 and 2005 VD Kuiper belt objects: individual: 2005 VD Kuiper belt objects: individual: 2008 YB3 Methods: numerical Oort Cloud Techniques: photometric Techniques: spectroscopic Kuiper belt objects Methods: numericals Oort cloud Techniques: photometric Techniques: spectroscopic Color Interplanetary flight Numerical methods Orbits Solar system Surface properties Planets Most 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 different 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 differences, 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 difference 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 differences 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 suffered a higher degree of processing, which is probably related to cometary activity episodes. © 2013 ESO. 2013 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v550_n_p_PinillaAlonso http://hdl.handle.net/20.500.12110/paper_00046361_v550_n_p_PinillaAlonso
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Kuiper belt objects: individual: 2005 VD
Kuiper belt objects: individual: 2008 YB3
Methods: numerical
Oort Cloud
Techniques: photometric
Techniques: spectroscopic
Kuiper belt objects
Methods: numericals
Oort cloud
Techniques: photometric
Techniques: spectroscopic
Color
Interplanetary flight
Numerical methods
Orbits
Solar system
Surface properties
Planets
spellingShingle Kuiper belt objects: individual: 2005 VD
Kuiper belt objects: individual: 2008 YB3
Methods: numerical
Oort Cloud
Techniques: photometric
Techniques: spectroscopic
Kuiper belt objects
Methods: numericals
Oort cloud
Techniques: photometric
Techniques: spectroscopic
Color
Interplanetary flight
Numerical methods
Orbits
Solar system
Surface properties
Planets
Surface composition and dynamical evolution of two retrograde objects in the outer solar system: 2008 YB3 and 2005 VD
topic_facet Kuiper belt objects: individual: 2005 VD
Kuiper belt objects: individual: 2008 YB3
Methods: numerical
Oort Cloud
Techniques: photometric
Techniques: spectroscopic
Kuiper belt objects
Methods: numericals
Oort cloud
Techniques: photometric
Techniques: spectroscopic
Color
Interplanetary flight
Numerical methods
Orbits
Solar system
Surface properties
Planets
description Most 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 different 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 differences, 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 difference 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 differences 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 suffered a higher degree of processing, which is probably related to cometary activity episodes. © 2013 ESO.
title Surface composition and dynamical evolution of two retrograde objects in the outer solar system: 2008 YB3 and 2005 VD
title_short Surface composition and dynamical evolution of two retrograde objects in the outer solar system: 2008 YB3 and 2005 VD
title_full Surface composition and dynamical evolution of two retrograde objects in the outer solar system: 2008 YB3 and 2005 VD
title_fullStr Surface composition and dynamical evolution of two retrograde objects in the outer solar system: 2008 YB3 and 2005 VD
title_full_unstemmed Surface composition and dynamical evolution of two retrograde objects in the outer solar system: 2008 YB3 and 2005 VD
title_sort surface composition and dynamical evolution of two retrograde objects in the outer solar system: 2008 yb3 and 2005 vd
publishDate 2013
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v550_n_p_PinillaAlonso
http://hdl.handle.net/20.500.12110/paper_00046361_v550_n_p_PinillaAlonso
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