The dynamics of objects in the inner edgeworth-kuiper belt

Objects in 3:2 mean motion resonance with Neptune are protected from close encounters with Neptune by the resonance. Bodies in orbits with semi-major axis between 39.5 and about 42 AU are not protected by the resonance; indeed due to overlapping secular resonances, the eccentricities of orbits in th...

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Detalles Bibliográficos
Autores principales:	Jones, D.C., Williams, I.P., Melita, M.D.
Formato:	JOUR
Materias:	Celestial mechanics Numerical methods: N-body Trans-Neptunian objects Neptune numerical model resonance solar system Neptunia
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_01679295_v97_n3-4_p435_Jones
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	todo:paper_01679295_v97_n3-4_p435_Jones
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spelling	todo:paper_01679295_v97_n3-4_p435_Jones2023-10-03T15:05:32Z The dynamics of objects in the inner edgeworth-kuiper belt Jones, D.C. Williams, I.P. Melita, M.D. Celestial mechanics Numerical methods: N-body Trans-Neptunian objects Neptune numerical model resonance solar system Neptunia Objects in 3:2 mean motion resonance with Neptune are protected from close encounters with Neptune by the resonance. Bodies in orbits with semi-major axis between 39.5 and about 42 AU are not protected by the resonance; indeed due to overlapping secular resonances, the eccentricities of orbits in this region are driven up so that a close encounter with Neptune becomes inevitable. It is thus expected that such orbits are unstable. The list of known Trans-Neptunian objects shows a deficiency in the number of objects in this gap compared to the 43-50 AU region, but the gap is not empty. We numerically integrate models for the initial population in the gap, and also all known objects over the age of the Solar System to determine what fraction can survive. We find that this fraction is significantly less than the ratio of the population in the gap to that in the main belt, suggesting that some mechanism must exist to introduce new members into the gap. By looking at the evolution of the test body orbits, we also determine the manner in which they are lost. Though all have close encounters with Neptune, in most cases this does not lead to ejection from the Solar System, but rather to a reduced perihelion distance causing close encounters with some or all of the other giant planets before being eventually lost from the system, with Saturn appearing to be the cause of the ejection of most of the objects. © Springer Science+Business Media, Inc. 2006. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_01679295_v97_n3-4_p435_Jones
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Celestial mechanics Numerical methods: N-body Trans-Neptunian objects Neptune numerical model resonance solar system Neptunia
spellingShingle	Celestial mechanics Numerical methods: N-body Trans-Neptunian objects Neptune numerical model resonance solar system Neptunia Jones, D.C. Williams, I.P. Melita, M.D. The dynamics of objects in the inner edgeworth-kuiper belt
topic_facet	Celestial mechanics Numerical methods: N-body Trans-Neptunian objects Neptune numerical model resonance solar system Neptunia
description	Objects in 3:2 mean motion resonance with Neptune are protected from close encounters with Neptune by the resonance. Bodies in orbits with semi-major axis between 39.5 and about 42 AU are not protected by the resonance; indeed due to overlapping secular resonances, the eccentricities of orbits in this region are driven up so that a close encounter with Neptune becomes inevitable. It is thus expected that such orbits are unstable. The list of known Trans-Neptunian objects shows a deficiency in the number of objects in this gap compared to the 43-50 AU region, but the gap is not empty. We numerically integrate models for the initial population in the gap, and also all known objects over the age of the Solar System to determine what fraction can survive. We find that this fraction is significantly less than the ratio of the population in the gap to that in the main belt, suggesting that some mechanism must exist to introduce new members into the gap. By looking at the evolution of the test body orbits, we also determine the manner in which they are lost. Though all have close encounters with Neptune, in most cases this does not lead to ejection from the Solar System, but rather to a reduced perihelion distance causing close encounters with some or all of the other giant planets before being eventually lost from the system, with Saturn appearing to be the cause of the ejection of most of the objects. © Springer Science+Business Media, Inc. 2006.
format	JOUR
author	Jones, D.C. Williams, I.P. Melita, M.D.
author_facet	Jones, D.C. Williams, I.P. Melita, M.D.
author_sort	Jones, D.C.
title	The dynamics of objects in the inner edgeworth-kuiper belt
title_short	The dynamics of objects in the inner edgeworth-kuiper belt
title_full	The dynamics of objects in the inner edgeworth-kuiper belt
title_fullStr	The dynamics of objects in the inner edgeworth-kuiper belt
title_full_unstemmed	The dynamics of objects in the inner edgeworth-kuiper belt
title_sort	dynamics of objects in the inner edgeworth-kuiper belt
url	http://hdl.handle.net/20.500.12110/paper_01679295_v97_n3-4_p435_Jones
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The dynamics of objects in the inner edgeworth-kuiper belt

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