Mapping the ν⊙ secular resonance for retrograde irregular satellites

Autores
Correa Otto, Jorge Alfredo; Leiva, Alejandro Martín; Giuppone, Cristian Andrés; Beauge, Cristian
Año de publicación
2010
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Constructing dynamical maps from the filtered output of numerical integrations, we analyse the structure of the ν⊙ secular resonance for fictitious irregular satellites in retrograde orbits. This commensurability is associated with the secular angle θ=π{variant}-π{variant}⊙, where π{variant} is the longitude of the pericentre of the satellite and .π{variant}⊙ corresponds to the (fixed) planetocentric orbit of the Sun. Our study is performed in the restricted three-body problem, where the satellites are considered as massless particles around a massive planet and perturbed by the Sun.Depending on the initial conditions, the resonance presents a diversity of possible resonant modes, including librations of θ around 0 (as found for Sinope and Pasiphae) or 180° as well as asymmetric librations (e.g. Narvi). Symmetric modes are present in all giant planets, although each regime appears restricted to certain values of the satellite inclination. Asymmetric solutions, on the other hand, seem absent around Neptune due to its almost circular heliocentric orbit.Simulating the effects of a smooth orbital migration on the satellite, we find that the resonance lock is preserved as long as the induced change in the semimajor axis is much slower compared to the period of the resonant angle (adiabatic limit). However, the librational mode may vary during the process, switching between symmetric and asymmetric oscillations.Finally, we present a simple scaling transformation that allows us to estimate the resonant structure around any giant planet from the results calculated around a single primary mass. © 2009 The Authors. Journal compilation © 2009 RAS.
Fil: Correa Otto, Jorge Alfredo. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Geofísica y Astronomía; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Leiva, Alejandro Martín. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Giuppone, Cristian Andrés. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Fil: Beauge, Cristian. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Materia
CELESTIAL MECHANICS
PLANETS AND SATELLITES: GENERAL
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/186677
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/186677
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Mapping the ν⊙ secular resonance for retrograde irregular satellitesCorrea Otto, Jorge AlfredoLeiva, Alejandro MartínGiuppone, Cristian AndrésBeauge, CristianCELESTIAL MECHANICSPLANETS AND SATELLITES: GENERALhttps://purl.org/becyt/ford/1.7https://purl.org/becyt/ford/1Constructing dynamical maps from the filtered output of numerical integrations, we analyse the structure of the ν⊙ secular resonance for fictitious irregular satellites in retrograde orbits. This commensurability is associated with the secular angle θ=π{variant}-π{variant}⊙, where π{variant} is the longitude of the pericentre of the satellite and .π{variant}⊙ corresponds to the (fixed) planetocentric orbit of the Sun. Our study is performed in the restricted three-body problem, where the satellites are considered as massless particles around a massive planet and perturbed by the Sun.Depending on the initial conditions, the resonance presents a diversity of possible resonant modes, including librations of θ around 0 (as found for Sinope and Pasiphae) or 180° as well as asymmetric librations (e.g. Narvi). Symmetric modes are present in all giant planets, although each regime appears restricted to certain values of the satellite inclination. Asymmetric solutions, on the other hand, seem absent around Neptune due to its almost circular heliocentric orbit.Simulating the effects of a smooth orbital migration on the satellite, we find that the resonance lock is preserved as long as the induced change in the semimajor axis is much slower compared to the period of the resonant angle (adiabatic limit). However, the librational mode may vary during the process, switching between symmetric and asymmetric oscillations.Finally, we present a simple scaling transformation that allows us to estimate the resonant structure around any giant planet from the results calculated around a single primary mass. © 2009 The Authors. Journal compilation © 2009 RAS.Fil: Correa Otto, Jorge Alfredo. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Geofísica y Astronomía; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Leiva, Alejandro Martín. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; ArgentinaFil: Giuppone, Cristian Andrés. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaFil: Beauge, Cristian. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaWiley Blackwell Publishing, Inc2010-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/186677Correa Otto, Jorge Alfredo; Leiva, Alejandro Martín; Giuppone, Cristian Andrés; Beauge, Cristian; Mapping the ν⊙ secular resonance for retrograde irregular satellites; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 402; 3; 1-2010; 1959-19680035-87111365-2966CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2009.16022.xinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/402/3/1959/989612info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T12:04:58Zoai:ri.conicet.gov.ar:11336/186677instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-22 12:04:59.078CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Mapping the ν⊙ secular resonance for retrograde irregular satellites
title Mapping the ν⊙ secular resonance for retrograde irregular satellites
spellingShingle Mapping the ν⊙ secular resonance for retrograde irregular satellites
Correa Otto, Jorge Alfredo
CELESTIAL MECHANICS
PLANETS AND SATELLITES: GENERAL
title_short Mapping the ν⊙ secular resonance for retrograde irregular satellites
title_full Mapping the ν⊙ secular resonance for retrograde irregular satellites
title_fullStr Mapping the ν⊙ secular resonance for retrograde irregular satellites
title_full_unstemmed Mapping the ν⊙ secular resonance for retrograde irregular satellites
title_sort Mapping the ν⊙ secular resonance for retrograde irregular satellites
dc.creator.none.fl_str_mv Correa Otto, Jorge Alfredo
Leiva, Alejandro Martín
Giuppone, Cristian Andrés
Beauge, Cristian
author Correa Otto, Jorge Alfredo
author_facet Correa Otto, Jorge Alfredo
Leiva, Alejandro Martín
Giuppone, Cristian Andrés
Beauge, Cristian
author_role author
author2 Leiva, Alejandro Martín
Giuppone, Cristian Andrés
Beauge, Cristian
author2_role author
author
author
dc.subject.none.fl_str_mv CELESTIAL MECHANICS
PLANETS AND SATELLITES: GENERAL
topic CELESTIAL MECHANICS
PLANETS AND SATELLITES: GENERAL
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.7
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Constructing dynamical maps from the filtered output of numerical integrations, we analyse the structure of the ν⊙ secular resonance for fictitious irregular satellites in retrograde orbits. This commensurability is associated with the secular angle θ=π{variant}-π{variant}⊙, where π{variant} is the longitude of the pericentre of the satellite and .π{variant}⊙ corresponds to the (fixed) planetocentric orbit of the Sun. Our study is performed in the restricted three-body problem, where the satellites are considered as massless particles around a massive planet and perturbed by the Sun.Depending on the initial conditions, the resonance presents a diversity of possible resonant modes, including librations of θ around 0 (as found for Sinope and Pasiphae) or 180° as well as asymmetric librations (e.g. Narvi). Symmetric modes are present in all giant planets, although each regime appears restricted to certain values of the satellite inclination. Asymmetric solutions, on the other hand, seem absent around Neptune due to its almost circular heliocentric orbit.Simulating the effects of a smooth orbital migration on the satellite, we find that the resonance lock is preserved as long as the induced change in the semimajor axis is much slower compared to the period of the resonant angle (adiabatic limit). However, the librational mode may vary during the process, switching between symmetric and asymmetric oscillations.Finally, we present a simple scaling transformation that allows us to estimate the resonant structure around any giant planet from the results calculated around a single primary mass. © 2009 The Authors. Journal compilation © 2009 RAS.
Fil: Correa Otto, Jorge Alfredo. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Geofísica y Astronomía; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Leiva, Alejandro Martín. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Giuppone, Cristian Andrés. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Fil: Beauge, Cristian. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
description Constructing dynamical maps from the filtered output of numerical integrations, we analyse the structure of the ν⊙ secular resonance for fictitious irregular satellites in retrograde orbits. This commensurability is associated with the secular angle θ=π{variant}-π{variant}⊙, where π{variant} is the longitude of the pericentre of the satellite and .π{variant}⊙ corresponds to the (fixed) planetocentric orbit of the Sun. Our study is performed in the restricted three-body problem, where the satellites are considered as massless particles around a massive planet and perturbed by the Sun.Depending on the initial conditions, the resonance presents a diversity of possible resonant modes, including librations of θ around 0 (as found for Sinope and Pasiphae) or 180° as well as asymmetric librations (e.g. Narvi). Symmetric modes are present in all giant planets, although each regime appears restricted to certain values of the satellite inclination. Asymmetric solutions, on the other hand, seem absent around Neptune due to its almost circular heliocentric orbit.Simulating the effects of a smooth orbital migration on the satellite, we find that the resonance lock is preserved as long as the induced change in the semimajor axis is much slower compared to the period of the resonant angle (adiabatic limit). However, the librational mode may vary during the process, switching between symmetric and asymmetric oscillations.Finally, we present a simple scaling transformation that allows us to estimate the resonant structure around any giant planet from the results calculated around a single primary mass. © 2009 The Authors. Journal compilation © 2009 RAS.
publishDate 2010
dc.date.none.fl_str_mv 2010-01
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/186677
Correa Otto, Jorge Alfredo; Leiva, Alejandro Martín; Giuppone, Cristian Andrés; Beauge, Cristian; Mapping the ν⊙ secular resonance for retrograde irregular satellites; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 402; 3; 1-2010; 1959-1968
0035-8711
1365-2966
CONICET Digital
CONICET
url http://hdl.handle.net/11336/186677
identifier_str_mv Correa Otto, Jorge Alfredo; Leiva, Alejandro Martín; Giuppone, Cristian Andrés; Beauge, Cristian; Mapping the ν⊙ secular resonance for retrograde irregular satellites; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 402; 3; 1-2010; 1959-1968
0035-8711
1365-2966
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2009.16022.x
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/402/3/1959/989612
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 12.982451

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