Formação coorbital com a terra e origem de theia
Carregando...
Arquivos
Data
2012-09-28
Autores
Luiz, André Amarante [UNESP]
Título da Revista
ISSN da Revista
Título de Volume
Editor
Universidade Estadual Paulista (Unesp)
Resumo
A hipótese atualmente mais aceita da origem da Lua, é a de ela ter se formado a partir de restos gerados por uma grande colisão entre a proto-Terra e um proto-planeta de tamanho similar a Marte, conhecido como Theia. Simulações mostraram que pode-se reproduzir a falta de ferro na Lua, as massas da Terra e Lua, e o momento angular atual do sistema Terra-Lua. Para tal, a colisão deve ter ocorrido de modo peculiar. Assim sendo, foi proposto que os corpos Terra e Theia seriam coorbitais, de modo que a velocidade de impacto seria baixa. Tendo isto em vista, em nosso trabalho nos propusemos a estudar o processo de acresção de massa, como um possível mecanismo de formação de planetas coorbitais à Terra. O trabalho se divide em duas partes principais. Em um primeiro momento tentamos reproduzir o cenário da teoria descrita no primeiro parágrafo, ou seja, estudamos a possibilidade de formação de um corpo com massa 𝑀D similar à de Marte e que seja coorbital com a Terra. Os presentes resultados das simulações numéricas mostram ser improvável a formação de um corpo com massa 𝑀D e que seja coorbital com a Terra. Na segunda parte do trabalho estudamos a possibilidade de formação de Theia e da proto-Terra seguindo um perfil de densidades. Os resultados das simulações numéricas do modelo não levaram à formação de corpos com massas 1,0 𝑀C e 1,0 𝑀D, mas houve a formação de corpos de massa menor (t 0,6𝑀C). Isso mostrou que o modelo adotado é promissor, e então, ajustes de parâmetros e inserção de planetas similares a Júpiter e Saturno no sistema foram implementados. Os resultados dessas últimas simulações mostraram ser possível a formação da Terra e de Theia, mas com velocidades relativas de colisão 2 vezes maior do que a esperada (¤ 4km/s)
The most accepted hypothesis of the origin of the Moon, she is to have formed from debris generated by a major collision between the proto-Earth and a proto-planet of si-milar size to Mars, known as Theia. Simulations showed one can reproduce the lack of iron in the Moon, the masses of the Earth and Moon, and the angular momentum of the current Earth-Moon system. To this end, the collision must have occurred in a particular way. Therefore, it was proposed that the bodies would be sharing the same orbit, i.e., Earth and Theia would coorbitals, so that the impact velocity and impact would be low subtle. In view of this, in our work we set out to study the process of mass accretion as a possible mechanism for the formation of planets coorbitals to Earth. The work is divided into two major parts. At first we tried to reproduce the scenario of the theory described in the first paragraph, ie, we study the possibility of forming a body with mass 𝑀D similar to that of Mars and the Earth is coorbital. The present results of numerical simulations show that it is unlikely the formation of a body with mass 𝑀D and is coorbital with Earth. In the second part of the paper we study the possibility of formation of Theia and proto-Earth following a density profile. The results of numerical simulations of the model did not lead to the formation of bodies with masses 1.0 𝑀C e 1.0 𝑀D, but there was the formation of bodies of mass smaller (t 0.6𝑀C). This showed that the model is promising, and then, parameter settings and insertion of planets similar to Jupiter and Saturn in the system were implemented. The results of these simulations showed latest possible formation of earth and Theia, but with relative rates of collision 2 times higher than expected (¤ 4km/s)
The most accepted hypothesis of the origin of the Moon, she is to have formed from debris generated by a major collision between the proto-Earth and a proto-planet of si-milar size to Mars, known as Theia. Simulations showed one can reproduce the lack of iron in the Moon, the masses of the Earth and Moon, and the angular momentum of the current Earth-Moon system. To this end, the collision must have occurred in a particular way. Therefore, it was proposed that the bodies would be sharing the same orbit, i.e., Earth and Theia would coorbitals, so that the impact velocity and impact would be low subtle. In view of this, in our work we set out to study the process of mass accretion as a possible mechanism for the formation of planets coorbitals to Earth. The work is divided into two major parts. At first we tried to reproduce the scenario of the theory described in the first paragraph, ie, we study the possibility of forming a body with mass 𝑀D similar to that of Mars and the Earth is coorbital. The present results of numerical simulations show that it is unlikely the formation of a body with mass 𝑀D and is coorbital with Earth. In the second part of the paper we study the possibility of formation of Theia and proto-Earth following a density profile. The results of numerical simulations of the model did not lead to the formation of bodies with masses 1.0 𝑀C e 1.0 𝑀D, but there was the formation of bodies of mass smaller (t 0.6𝑀C). This showed that the model is promising, and then, parameter settings and insertion of planets similar to Jupiter and Saturn in the system were implemented. The results of these simulations showed latest possible formation of earth and Theia, but with relative rates of collision 2 times higher than expected (¤ 4km/s)
Descrição
Palavras-chave
Astronomia, Lua, Mecânica celeste, Astronomy
Como citar
LUIZ, André Amarante. Formação coorbital com a terra e origem de theia. 2012. 80 p. Dissertação (mestrado) – Universidade Estadual Paulista, Faculdade de Engenharia de Guaratinguetá, 2012.