The phase space structure of retrograde mean motion resonances with Neptune: the 4/5, 7/9, 5/8 and 8/13 cases

Registro completo de metadados
MetadadosDescriçãoIdioma
Autor(es): dc.contributorAristotle University of Thessaloniki-
Autor(es): dc.contributorUniversidade Estadual Paulista (UNESP)-
Autor(es): dc.creatorKotoulas, Thomas-
Autor(es): dc.creatorMorais, Maria Helena Moreira-
Autor(es): dc.creatorVoyatzis, George-
Data de aceite: dc.date.accessioned2025-08-21T16:02:55Z-
Data de disponibilização: dc.date.available2025-08-21T16:02:55Z-
Data de envio: dc.date.issued2023-07-29-
Data de envio: dc.date.issued2023-07-29-
Data de envio: dc.date.issued2022-11-30-
Fonte completa do material: dc.identifierhttp://dx.doi.org/10.1007/s10569-022-10106-3-
Fonte completa do material: dc.identifierhttp://hdl.handle.net/11449/246284-
Fonte: dc.identifier.urihttp://educapes.capes.gov.br/handle/11449/246284-
Descrição: dc.descriptionWe compute planar and three-dimensional retrograde periodic orbits in the vicinity of the restricted three-body problem (RTBP) with the Sun and Neptune as primaries and we concentrate on the dynamics of higher-order exterior mean motion resonances with Neptune. By using the circular planar model as the basic model, families of retrograde symmetric periodic orbits are computed at the 4/5, 7/9, 5/8 and 8/13 resonances. We determine the bifurcation points from the planar circular to the planar elliptic problem and we find all the corresponding families. In order to obtain a global view of the families of periodic orbits, the eccentricity of the primaries takes values in the whole interval 0 < e′< 1. Then, we find all the possible vertical critical orbits (v.c.o) of the planar circular problem and we proceed to the three-dimensional circular restricted 3-body problem. In this model, retrograde periodic orbits are generated mainly from the retrograde v.c.o. Also, if we continue families of direct orbits for i> 90 ∘, then we can obtain families of 3D symmetric retrograde periodic orbits. The linear stability is examined too. Stable periodic orbits are associated with phase space domains of resonant motion where TNOs can be captured. In order to study the phase space structure of the above resonances, we construct dynamical stability maps for the whole inclination interval (0 < i< 180 ∘) by using the well-known “MEGNO Chaos Indicator”. Finally, we discuss about TNOs which are currently located at these resonances.-
Descrição: dc.descriptionResearch Committee, Aristotle University of Thessaloniki-
Descrição: dc.descriptionAristotle University of Thessaloniki-
Descrição: dc.descriptionDepartment of Physics Aristotle University of Thessaloniki-
Descrição: dc.descriptionInstituto de Geociências e Ciências Exatas Universidade Estadual Paulista (UNESP), Av. 24-A, 1515, SP-
Descrição: dc.descriptionInstituto de Geociências e Ciências Exatas Universidade Estadual Paulista (UNESP), Av. 24-A, 1515, SP-
Idioma: dc.languageen-
Relação: dc.relationCelestial Mechanics and Dynamical Astronomy-
???dc.source???: dc.sourceScopus-
Palavras-chave: dc.subjectPeriodic orbits-
Palavras-chave: dc.subjectRestricted three-body problem-
Palavras-chave: dc.subjectMEGNO chaos indicator-
Palavras-chave: dc.subjectDynamical stability maps-
Palavras-chave: dc.subjectKuiper belt-
Palavras-chave: dc.subjectTrans-Neptunian objects-
Título: dc.titleThe phase space structure of retrograde mean motion resonances with Neptune: the 4/5, 7/9, 5/8 and 8/13 cases-
Tipo de arquivo: dc.typelivro digital-
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