Building the Galilean moons system via pebble accretion and migration: A primordial resonant chain
Autor(a) principal: | |
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Data de Publicação: | 2021 |
Outros Autores: | , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.1093/mnras/stab986 http://hdl.handle.net/11449/206474 |
Resumo: | The origins of the Galilean satellites - namely Io, Europa, Ganymede, and Callisto - is not fully understood yet. Here we use N-body numerical simulations to study the formation of Galilean satellites in a gaseous circumplanetary disc around Jupiter. Our model includes the effects of pebble accretion, gas-driven migration, and gas tidal damping and drag. Satellitesimals in our simulations first grow via pebble accretion and start to migrate inwards. When they reach the trap at the disc inner edge, scattering events and collisions take place promoting additional growth. Growing satellites eventually reach a multiresonant configuration anchored at the disc inner edge. Our results show that an integrated pebble flux of ≥2 × 10-3 MJ results in the formation of satellites with masses typically larger than those of the Galilean satellites. Our best match to the masses of the Galilean satellites is produced in simulations where the integrated pebble flux is ∼10-3 MJ. These simulations typically produce between three and five satellites. In our best analogues, adjacent satellite pairs are all locked in 2:1 mean motion resonances. However, they have also moderately eccentric orbits (~0.1), unlike the current real satellites. We propose that the Galilean satellites system is a primordial resonant chain, similar to exoplanet systems as TRAPPIST-1, Kepler-223, and TOI-178. Callisto was probably in resonance with Ganymede in the past but left this configuration - without breaking the Laplacian resonance - via divergent migration due to tidal planet-satellite interactions. These same effects further damped the orbital eccentricities of these satellites down to their current values (~0.001). Our results support the hypothesis that Io and Europa were born with water-ice rich compositions and lost all/most of their water afterwards. Firmer constraints on the primordial compositions of the Galilean satellites are crucial to distinguish formation models. |
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Building the Galilean moons system via pebble accretion and migration: A primordial resonant chainPlanet-disc interactionsPlanets and satellites: dynamical evolution and stabilityPlanets and satellites: formationPlanets and satellites: individual: Galilean moonsProtoplanetary discsThe origins of the Galilean satellites - namely Io, Europa, Ganymede, and Callisto - is not fully understood yet. Here we use N-body numerical simulations to study the formation of Galilean satellites in a gaseous circumplanetary disc around Jupiter. Our model includes the effects of pebble accretion, gas-driven migration, and gas tidal damping and drag. Satellitesimals in our simulations first grow via pebble accretion and start to migrate inwards. When they reach the trap at the disc inner edge, scattering events and collisions take place promoting additional growth. Growing satellites eventually reach a multiresonant configuration anchored at the disc inner edge. Our results show that an integrated pebble flux of ≥2 × 10-3 MJ results in the formation of satellites with masses typically larger than those of the Galilean satellites. Our best match to the masses of the Galilean satellites is produced in simulations where the integrated pebble flux is ∼10-3 MJ. These simulations typically produce between three and five satellites. In our best analogues, adjacent satellite pairs are all locked in 2:1 mean motion resonances. However, they have also moderately eccentric orbits (~0.1), unlike the current real satellites. We propose that the Galilean satellites system is a primordial resonant chain, similar to exoplanet systems as TRAPPIST-1, Kepler-223, and TOI-178. Callisto was probably in resonance with Ganymede in the past but left this configuration - without breaking the Laplacian resonance - via divergent migration due to tidal planet-satellite interactions. These same effects further damped the orbital eccentricities of these satellites down to their current values (~0.001). Our results support the hypothesis that Io and Europa were born with water-ice rich compositions and lost all/most of their water afterwards. Firmer constraints on the primordial compositions of the Galilean satellites are crucial to distinguish formation models.Grupo de Dinâmica Orbital and Planetologia The University of São Paulo State-UNESP, Av. Ariberto Pereira da Cunha, 333Department of Earth Environmental and Planetary Sciences Rice University, MS 126Grupo de Dinâmica Orbital and Planetologia The University of São Paulo State-UNESP, Av. Ariberto Pereira da Cunha, 333Universidade Estadual Paulista (Unesp)Rice UniversityMadeira, Gustavo [UNESP]Izidoro, André [UNESP]Giuliatti Winter, Silvia M. [UNESP]2021-06-25T10:32:35Z2021-06-25T10:32:35Z2021-06-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/article1854-1872http://dx.doi.org/10.1093/mnras/stab986Monthly Notices of the Royal Astronomical Society, v. 504, n. 2, p. 1854-1872, 2021.1365-29660035-8711http://hdl.handle.net/11449/20647410.1093/mnras/stab9862-s2.0-85107790978Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengMonthly Notices of the Royal Astronomical Societyinfo:eu-repo/semantics/openAccess2021-10-23T05:55:16Zoai:repositorio.unesp.br:11449/206474Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462021-10-23T05:55:16Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
Building the Galilean moons system via pebble accretion and migration: A primordial resonant chain |
title |
Building the Galilean moons system via pebble accretion and migration: A primordial resonant chain |
spellingShingle |
Building the Galilean moons system via pebble accretion and migration: A primordial resonant chain Madeira, Gustavo [UNESP] Planet-disc interactions Planets and satellites: dynamical evolution and stability Planets and satellites: formation Planets and satellites: individual: Galilean moons Protoplanetary discs |
title_short |
Building the Galilean moons system via pebble accretion and migration: A primordial resonant chain |
title_full |
Building the Galilean moons system via pebble accretion and migration: A primordial resonant chain |
title_fullStr |
Building the Galilean moons system via pebble accretion and migration: A primordial resonant chain |
title_full_unstemmed |
Building the Galilean moons system via pebble accretion and migration: A primordial resonant chain |
title_sort |
Building the Galilean moons system via pebble accretion and migration: A primordial resonant chain |
author |
Madeira, Gustavo [UNESP] |
author_facet |
Madeira, Gustavo [UNESP] Izidoro, André [UNESP] Giuliatti Winter, Silvia M. [UNESP] |
author_role |
author |
author2 |
Izidoro, André [UNESP] Giuliatti Winter, Silvia M. [UNESP] |
author2_role |
author author |
dc.contributor.none.fl_str_mv |
Universidade Estadual Paulista (Unesp) Rice University |
dc.contributor.author.fl_str_mv |
Madeira, Gustavo [UNESP] Izidoro, André [UNESP] Giuliatti Winter, Silvia M. [UNESP] |
dc.subject.por.fl_str_mv |
Planet-disc interactions Planets and satellites: dynamical evolution and stability Planets and satellites: formation Planets and satellites: individual: Galilean moons Protoplanetary discs |
topic |
Planet-disc interactions Planets and satellites: dynamical evolution and stability Planets and satellites: formation Planets and satellites: individual: Galilean moons Protoplanetary discs |
description |
The origins of the Galilean satellites - namely Io, Europa, Ganymede, and Callisto - is not fully understood yet. Here we use N-body numerical simulations to study the formation of Galilean satellites in a gaseous circumplanetary disc around Jupiter. Our model includes the effects of pebble accretion, gas-driven migration, and gas tidal damping and drag. Satellitesimals in our simulations first grow via pebble accretion and start to migrate inwards. When they reach the trap at the disc inner edge, scattering events and collisions take place promoting additional growth. Growing satellites eventually reach a multiresonant configuration anchored at the disc inner edge. Our results show that an integrated pebble flux of ≥2 × 10-3 MJ results in the formation of satellites with masses typically larger than those of the Galilean satellites. Our best match to the masses of the Galilean satellites is produced in simulations where the integrated pebble flux is ∼10-3 MJ. These simulations typically produce between three and five satellites. In our best analogues, adjacent satellite pairs are all locked in 2:1 mean motion resonances. However, they have also moderately eccentric orbits (~0.1), unlike the current real satellites. We propose that the Galilean satellites system is a primordial resonant chain, similar to exoplanet systems as TRAPPIST-1, Kepler-223, and TOI-178. Callisto was probably in resonance with Ganymede in the past but left this configuration - without breaking the Laplacian resonance - via divergent migration due to tidal planet-satellite interactions. These same effects further damped the orbital eccentricities of these satellites down to their current values (~0.001). Our results support the hypothesis that Io and Europa were born with water-ice rich compositions and lost all/most of their water afterwards. Firmer constraints on the primordial compositions of the Galilean satellites are crucial to distinguish formation models. |
publishDate |
2021 |
dc.date.none.fl_str_mv |
2021-06-25T10:32:35Z 2021-06-25T10:32:35Z 2021-06-01 |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/article |
format |
article |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://dx.doi.org/10.1093/mnras/stab986 Monthly Notices of the Royal Astronomical Society, v. 504, n. 2, p. 1854-1872, 2021. 1365-2966 0035-8711 http://hdl.handle.net/11449/206474 10.1093/mnras/stab986 2-s2.0-85107790978 |
url |
http://dx.doi.org/10.1093/mnras/stab986 http://hdl.handle.net/11449/206474 |
identifier_str_mv |
Monthly Notices of the Royal Astronomical Society, v. 504, n. 2, p. 1854-1872, 2021. 1365-2966 0035-8711 10.1093/mnras/stab986 2-s2.0-85107790978 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
Monthly Notices of the Royal Astronomical Society |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.format.none.fl_str_mv |
1854-1872 |
dc.source.none.fl_str_mv |
Scopus reponame:Repositório Institucional da UNESP instname:Universidade Estadual Paulista (UNESP) instacron:UNESP |
instname_str |
Universidade Estadual Paulista (UNESP) |
instacron_str |
UNESP |
institution |
UNESP |
reponame_str |
Repositório Institucional da UNESP |
collection |
Repositório Institucional da UNESP |
repository.name.fl_str_mv |
Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP) |
repository.mail.fl_str_mv |
|
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1799965007168929792 |