Growth and evolution of satellites in a Jovian massive disc
| Autor: | E. Vieira Neto, Wilhelm Kley, R. A. Moraes |
|---|---|
| Přispěvatelé: | Universidade Estadual Paulista (Unesp), Universität Tübingen |
| Rok vydání: | 2017 |
| Předmět: |
010504 meteorology & atmospheric sciences
media_common.quotation_subject FOS: Physical sciences Minimum mass Astrophysics 01 natural sciences Jovian symbols.namesake Individual: (Galilean satellites) [Planets and satellites] Planet 0103 physical sciences Eccentricity (behavior) 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics 0105 earth and related environmental sciences media_common Earth and Planetary Astrophysics (astro-ph.EP) Physics Astronomy and Astrophysics Exoplanet Galilean moons Space and Planetary Science Physics::Space Physics symbols Terrestrial planet Satellite Astrophysics::Earth and Planetary Astrophysics formation [Planets and satellites] Astrophysics - Earth and Planetary Astrophysics |
| Zdroj: | Scopus Repositório Institucional da UNESP Universidade Estadual Paulista (UNESP) instacron:UNESP |
| ISSN: | 1365-2966 0035-8711 |
| DOI: | 10.1093/mnras/stx3268 |
| Popis: | The formation of satellite systems in circum-planetary discs is considered to be similar to the formation of rocky planets in a proto-planetary disc, especially Super-Earths. Thus, it is possible to use systems with large satellites to test formation theories that are also applicable to extrasolar planets. Furthermore, a better understanding of the origin of satellites might yield important information about the environment near the growing planet during the last stages of planet formation. In this work we investigate the formation and migration of the Jovian satellites through N-body simulations. We simulated a massive, static, low viscosity, circum-planetary disc in agreement with the minimum mass sub-nebula model prescriptions for its total mass. In hydrodynamic simulations we found no signs of gaps, therefore type II migration is not expected. Hence, we used analytic prescriptions for type I migration, eccentricity and inclination damping, and performed N-body simulations with damping forces added. Detailed parameter studies showed that the number of final satellites is strong influenced by the initial distribution of embryos, the disc temperature, and the initial gas density profile. For steeper initial density profiles it is possible to form systems with multiple satellites in resonance while a flatter profile favours the formation of satellites close to the region of the Galilean satellites. We show that the formation of massive satellites such as Ganymede and Callisto can be achieved for hotter discs with an aspect ratio of H/r ~ 0.15 for which the ice line was located around 30 R_J. 17 pages, 21 figures |
| Databáze: | OpenAIRE |
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