Fluxo de material para o disco circumplanetário necessário para a formação de satélites de planetas gigantes
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Data
2022-05-09
Autores
Santos, Julio Cesar Monteiro dos
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Universidade Estadual Paulista (Unesp)
Resumo
O sistema de satélites galileanos tem uma arquitetura similar a do Sistema Solar, entre as similaridades está o fato dos satélites apresentarem órbitas quase circulares e coplanares com o plano equatorial de Júpiter. Uma outra característica dos galileanos é que esses apresentam densidade decrescente conforme se afastam do planeta, ou seja, o mais denso é o satélite mais próximo ao planeta enquanto o menos denso é o mais distante (Lunine e Stevenson, 1982). Existem modelos de formação dos satélites galileanos equivalentes aos da formação dos planetas, todavia na escala do disco circumplanetário. Neste trabalho de dissertação de mestrado são considerados dois modelos principais que descrevem a formação desses satélites através do disco circumplanetário. O modelo de Massa Mínima para a Sub-Nébula (MMSN) (Lunine e Stevenson, 1982) sugere que os satélites galileanos se formaram em um disco circumplanetário ao redor de Júpiter durante o último estágio de formação do planeta. Nessa fase o disco não recebe mais material e pode ser aproximado por um disco circumplanetário não-turbulento, sem a formação de vortexes, com baixa possibilidade de aglomeração de material em zonas especificas no disco ou transporte descontínuo durante a formação dos satélites. Por outro lado, o segundo modelo (Canup e Ward, 2002) sugere um outro tipo de disco circumplanetário: o disco possui inicialmente pouca massa em gás e poeira e vai crescendo em massa adquirindo material oriundo do disco circunstelar. Neste trabalho é estudada a formação de sistemas de satélites sob as considerações do modelo MMSN e também do modelo do Disco com Déficit de Gás. São realizadas simulações numéricas hidrodinâmicas com o objetivo de se obter informações que caracterizam o disco de gás em volta do planeta. As simulações são feitas utilizando o código hidrodinâmico FARGO 3D (Benitez-Llambay e Masset, 2016), entretanto esse tipo de código traz consigo dificuldades como a resolução necessária para obter informações com precisão devido a simplicidade se seu integrador de N-corpos do tipo Rung-Kutta. Assim, para se obter resultados mais rápidos são utilizadas as simulações hidrodinâmicas para entender o comportamento do disco de gás ao redor do planeta e então essas informações são usadas no pacote de integração numérica de N-corpos REBOUND. Portanto, foram realizadas simulações numéricas com o uso do REBOUND (Rein e Liu, 2012) adaptando o código para estudar o crescimento dos satélites durante a fase colisional. Durante as simulações, são explorados parâmetros como a distribuição radial e a massa dos sólidos no disco, a densidade da nuvem de gás e a proporção de massa e gás do disco, como também a posição da linha de gelo ao longo do disco, considerando as informações obtidas através das simulações hidrodinâmicas. Isso é feito para elucidar em comparação com o modelo de Déficit de Gás a relevância do fluxo de matéria durante a formação dos satélites.
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
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
Descrição
Palavras-chave
Formação de Satélites, Integração Numérica, Satélites Galileanos, Satellites formation, Galilean Satellites., Numeric integration, Satélites - Órbitas, Integração numérica, Sistema solar