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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/186677
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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 Técnicas2025-09-29T10:32:35Zoai: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:34982025-09-29 10:32:35.347CONICET 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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1844614339542122496 |
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13.070432 |