Orbital migrations in planetesimal discs: N-body simulations and the resonant dynamical friction

Autores
Cionco, Rodolfo Gustavo; Brunini, Adrián
Año de publicación
2002
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We have performed N-body numerical simulations of the exchange of angular momentum between a massive planet and a 3D Keplerian disc of planetesimals. Our interest is directed at the study of the classical analytical expressions of the lineal theory of density waves, as representative of the dynamical friction in discs 'dominated by the planet' and the orbital migration of the planets with regard to this effect. By means of a numerical integration of the equations of motion, we have carried out a set of numerical experiments with a large number of particles (N ≥ 10 000), and planets with the mass of Jupiter, Saturn and one core mass of the giant planets in the Solar system (Mc = 10M⊕). The torque, measured in a phase in which a 'steady forcing' is clearly measurable, yields inward migration in a minimum-mass solar disc (∑ ∼ 10 g cm-2 ), with a characteristic drift time of ∼ a few 106 yr. The planets predate the disc, but the orbital decay rate is not sufficient to allow accretion in a time-scale relevant to the formation of giant planets. We found reductions of the measured torque on the planet, with respect to the linear theory, by a factor of 0.38 for Mc, 0.04 for Saturn and 0.01 for Jupiter, due to the increase in the perturbation on the disc. The behaviour of planets whose mass is larger than Mc is similar to the one of type II migrators in gaseous discs. Our results suggest that, in a minimum mass, solar planetesimals disc, type I migrations occur for masses smaller than Mc, whereas for this mass value it could be a transition zone between the two types of migration.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
Materia
Ciencias Astronómicas
Celestial mechanics
Planetary systems
Planets and satellites: General
Solar system: Formation
Stellar dynamics
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/84600

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/84600
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network_name_str SEDICI (UNLP)
spelling Orbital migrations in planetesimal discs: N-body simulations and the resonant dynamical frictionCionco, Rodolfo GustavoBrunini, AdriánCiencias AstronómicasCelestial mechanicsPlanetary systemsPlanets and satellites: GeneralSolar system: FormationStellar dynamicsWe have performed N-body numerical simulations of the exchange of angular momentum between a massive planet and a 3D Keplerian disc of planetesimals. Our interest is directed at the study of the classical analytical expressions of the lineal theory of density waves, as representative of the dynamical friction in discs 'dominated by the planet' and the orbital migration of the planets with regard to this effect. By means of a numerical integration of the equations of motion, we have carried out a set of numerical experiments with a large number of particles (N ≥ 10 000), and planets with the mass of Jupiter, Saturn and one core mass of the giant planets in the Solar system (M<SUB>c</SUB> = 10M⊕). The torque, measured in a phase in which a 'steady forcing' is clearly measurable, yields inward migration in a minimum-mass solar disc (∑ ∼ 10 g cm<SUP>-2</SUP> ), with a characteristic drift time of ∼ a few 10<SUP>6</SUP> yr. The planets predate the disc, but the orbital decay rate is not sufficient to allow accretion in a time-scale relevant to the formation of giant planets. We found reductions of the measured torque on the planet, with respect to the linear theory, by a factor of 0.38 for M<SUB>c</SUB>, 0.04 for Saturn and 0.01 for Jupiter, due to the increase in the perturbation on the disc. The behaviour of planets whose mass is larger than M<SUB>c</SUB> is similar to the one of type II migrators in gaseous discs. Our results suggest that, in a minimum mass, solar planetesimals disc, type I migrations occur for masses smaller than M<SUB>c</SUB>, whereas for this mass value it could be a transition zone between the two types of migration.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2002info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf77-86http://sedici.unlp.edu.ar/handle/10915/84600enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/doi/10.1046/j.1365-8711.2002.05477.xinfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:15Zoai:sedici.unlp.edu.ar:10915/84600Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:16.256SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Orbital migrations in planetesimal discs: N-body simulations and the resonant dynamical friction
title Orbital migrations in planetesimal discs: N-body simulations and the resonant dynamical friction
spellingShingle Orbital migrations in planetesimal discs: N-body simulations and the resonant dynamical friction
Cionco, Rodolfo Gustavo
Ciencias Astronómicas
Celestial mechanics
Planetary systems
Planets and satellites: General
Solar system: Formation
Stellar dynamics
title_short Orbital migrations in planetesimal discs: N-body simulations and the resonant dynamical friction
title_full Orbital migrations in planetesimal discs: N-body simulations and the resonant dynamical friction
title_fullStr Orbital migrations in planetesimal discs: N-body simulations and the resonant dynamical friction
title_full_unstemmed Orbital migrations in planetesimal discs: N-body simulations and the resonant dynamical friction
title_sort Orbital migrations in planetesimal discs: N-body simulations and the resonant dynamical friction
dc.creator.none.fl_str_mv Cionco, Rodolfo Gustavo
Brunini, Adrián
author Cionco, Rodolfo Gustavo
author_facet Cionco, Rodolfo Gustavo
Brunini, Adrián
author_role author
author2 Brunini, Adrián
author2_role author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Celestial mechanics
Planetary systems
Planets and satellites: General
Solar system: Formation
Stellar dynamics
topic Ciencias Astronómicas
Celestial mechanics
Planetary systems
Planets and satellites: General
Solar system: Formation
Stellar dynamics
dc.description.none.fl_txt_mv We have performed N-body numerical simulations of the exchange of angular momentum between a massive planet and a 3D Keplerian disc of planetesimals. Our interest is directed at the study of the classical analytical expressions of the lineal theory of density waves, as representative of the dynamical friction in discs 'dominated by the planet' and the orbital migration of the planets with regard to this effect. By means of a numerical integration of the equations of motion, we have carried out a set of numerical experiments with a large number of particles (N ≥ 10 000), and planets with the mass of Jupiter, Saturn and one core mass of the giant planets in the Solar system (M<SUB>c</SUB> = 10M⊕). The torque, measured in a phase in which a 'steady forcing' is clearly measurable, yields inward migration in a minimum-mass solar disc (∑ ∼ 10 g cm<SUP>-2</SUP> ), with a characteristic drift time of ∼ a few 10<SUP>6</SUP> yr. The planets predate the disc, but the orbital decay rate is not sufficient to allow accretion in a time-scale relevant to the formation of giant planets. We found reductions of the measured torque on the planet, with respect to the linear theory, by a factor of 0.38 for M<SUB>c</SUB>, 0.04 for Saturn and 0.01 for Jupiter, due to the increase in the perturbation on the disc. The behaviour of planets whose mass is larger than M<SUB>c</SUB> is similar to the one of type II migrators in gaseous discs. Our results suggest that, in a minimum mass, solar planetesimals disc, type I migrations occur for masses smaller than M<SUB>c</SUB>, whereas for this mass value it could be a transition zone between the two types of migration.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
description We have performed N-body numerical simulations of the exchange of angular momentum between a massive planet and a 3D Keplerian disc of planetesimals. Our interest is directed at the study of the classical analytical expressions of the lineal theory of density waves, as representative of the dynamical friction in discs 'dominated by the planet' and the orbital migration of the planets with regard to this effect. By means of a numerical integration of the equations of motion, we have carried out a set of numerical experiments with a large number of particles (N ≥ 10 000), and planets with the mass of Jupiter, Saturn and one core mass of the giant planets in the Solar system (M<SUB>c</SUB> = 10M⊕). The torque, measured in a phase in which a 'steady forcing' is clearly measurable, yields inward migration in a minimum-mass solar disc (∑ ∼ 10 g cm<SUP>-2</SUP> ), with a characteristic drift time of ∼ a few 10<SUP>6</SUP> yr. The planets predate the disc, but the orbital decay rate is not sufficient to allow accretion in a time-scale relevant to the formation of giant planets. We found reductions of the measured torque on the planet, with respect to the linear theory, by a factor of 0.38 for M<SUB>c</SUB>, 0.04 for Saturn and 0.01 for Jupiter, due to the increase in the perturbation on the disc. The behaviour of planets whose mass is larger than M<SUB>c</SUB> is similar to the one of type II migrators in gaseous discs. Our results suggest that, in a minimum mass, solar planetesimals disc, type I migrations occur for masses smaller than M<SUB>c</SUB>, whereas for this mass value it could be a transition zone between the two types of migration.
publishDate 2002
dc.date.none.fl_str_mv 2002
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
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info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/84600
url http://sedici.unlp.edu.ar/handle/10915/84600
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0035-8711
info:eu-repo/semantics/altIdentifier/doi/10.1046/j.1365-8711.2002.05477.x
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
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repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
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