Building the Galilean moons system via pebble accretion and migration: a primordial resonant chain

Autor(es)

Madeira, Gustavo ^[1] ; Izidoro, Andre ^{[2, 1]} ; Giuliatti Winter, Silvia M. ^[1]

Afiliação do(s) autor(es)

^[1] Univ Sao Paulo State, UNESP, Grp Dinam Orbital & Planetol, Av Ariberto Pereira da Cunha 333, BR-12516410 Guaratingueta, SP - Brazil

^[2] Rice Univ, Dept Earth Environm & Planetary Sci, MS 126, Houston, MS 77005 - USA

• Tipo de documento: Artigo Científico
• Fonte: Monthly Notices of the Royal Astronomical Society; v. 504, n. 2, p. 1854-1872, JUN 2021.
• Citações Web of Science: 0

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 x 10(-3) M-J 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 similar to 10(-3) M-J. 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 (similar to 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 (similar to 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. (AU)

• Processo FAPESP: 13/07375-0 - CeMEAI - Centro de Ciências Matemáticas Aplicadas à Indústria
• Beneficiário: José Alberto Cuminato
• Modalidade de apoio: Auxílio à Pesquisa - Centros de Pesquisa, Inovação e Difusão - CEPIDs
• Processo FAPESP: 16/12686-2 - Formação e dinâmica planetária: do Sistema Solar a exoplanetas
• Beneficiário: André Izidoro Ferreira da Costa
• Modalidade de apoio: Auxílio à Pesquisa - Jovens Pesquisadores
• Processo FAPESP: 16/19556-7 - Formação e Dinâmica Planetária: do Sistema Solar a Exoplanetas
• Beneficiário: André Izidoro Ferreira da Costa
• Modalidade de apoio: Bolsas no Brasil - Jovens Pesquisadores
• Processo FAPESP: 18/23568-6 - Cenários para a formação dos arcos de Netuno e dos grandes satélites dos gigantes gasosos
• Beneficiário: Gustavo Oliveira Madeira
• Modalidade de apoio: Bolsas no Brasil - Doutorado
• Processo FAPESP: 16/24561-0 - A relevância dos pequenos corpos em dinâmica orbital
• Beneficiário: Othon Cabo Winter
• Modalidade de apoio: Auxílio à Pesquisa - Temático