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| Author(s): |
Julio Cesar Monteiro dos Santos
Total Authors: 1
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| Document type: | Master's Dissertation |
| Press: | Guaratinguetá. 2022-06-20. |
| Institution: | Universidade Estadual Paulista (Unesp). Faculdade de Engenharia. Guaratinguetá |
| Defense date: | 2022-05-09 |
| Advisor: | Ernesto Vieira Neto |
| Abstract | |
The Galilean satellite system has an architecture similar to that of the Solar System, among the similarities is the fact that the satellites present almost circular and coplanar orbits with the equatorial plane of Jupiter, in addition the Galileans also present decreasing density as they move away from the planet, that is, the densest is the satellite closest to the planet while the least dense is the most distant (Lunine and Stevenson, 1982), as observed for terrestrial planets in the Solar System. There are models for the formation of Galilean satellites equivalent to the formation of planets, however on the scale of the circumplanetary disk. There are two main models that describe the formation of these satellites across the circumplanetary disk. The Minimum Mass Sub-Nebula (MMSN) model (Lunine and Stevenson, 1982) suggests that Galilean satellites form in a circumplanetary disk around Jupiter during the last stage of planet formation. At this stage, the disk does not receive any more material and can be approximated by a non-turbulent circumplanetary disk, without the formation of vortexes, with little possibility of agglomeration of material in specific zones in the disk or discontinuous transport during the formation of the satellites. The second model (Canup and Ward, 2002) suggests, on the other hand, another type of circumplanetary disk: the disk initially has little mass in gas and dust and then grows in mass acquiring material from the circumstellar disk. In this work, the formation of satellite systems is studied under the considerations of the MMSN model and the reproduction of the Disk with Gas Deficit model is also carried out. Hydrodynamic simulations are performed in order to obtain information that characterizes the gas disk around the planet. The simulations are performed using the FARGO 3D hydrodynamic code (Benitez-Llambay and Masset, 2016), however this type of code brings with it difficulties such as the resolution required to obtain information accurately due to the simplicity of its Rung-Kutta N-body type integrator. Thus, in order to obtain faster results, hydrodynamic simulations are used to understand the behavior of the gas disk around the planet and then this information is used in the REBOUND N-body package. Therefore, numerical simulations were performed using REBOUND (Rein and Liu, 2012) adapting the code to study the growth of satellites during the collision phase. During the simulations, parameters such as the radial distribution and the mass of the solids in the disk, the density of the gas cloud and the proportion of mass and gas of the disk, as well as the position of the ice line along the disk are explored considering the information obtained through hydrodynamic simulations. This is done to elucidate in comparison with the Gas Deficit model the relevance of the flow of matter during the formation of the satellites (AU) | |
| FAPESP's process: | 19/21857-3 - Flux of material to circumplanetary disk necessary for the formations of satellites in giant planets |
| Grantee: | Julio Cesar Monteiro dos Santos |
| Support Opportunities: | Scholarships in Brazil - Master |