Dinâmica secular no cinturão principal de asteroides
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Data
2017-02-24
Autores
Huaman Espinoza, Mariela [UNESP]
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Universidade Estadual Paulista (Unesp)
Resumo
Nesta tese, nós introduzimos uma nova métrica no domínio dos elementos próprios, nas cores obtidas pela survey SDSS-MOC4 e nos albedos geométricos do WISE, com o objetivo de obter um método para determinar uma família dinâmica e o halo. Assim determinamos a família de Vesta que se caracteriza por seus membros estarem associados a material basáltico. Ela está localizada no cinturão interno e nas últimas décadas foram identificados vários objetos fora da região dinâmica da família. Realizamos uma revisão dos conhecimentos atuais sobre candidatos fotométricos de tipo V e consideramos as hipóteses de possíveis fontes originárias de material basáltico localizados no cinturão central e externo. Nosso primeiro objetivo foi estudar a evolução dinâmica induzida pelo efeito Yarkovsky nos clones dos candidatos fotométricos. De acordo com nossas investigações, nós verificamos que alguns candidatos fotométricos de tipo V foram encontrados na ressonância secular não linear g + g5 − 2g6 nas regiões central e externo do cinturão de asteroides, mostrando-se como um mecanismo eficaz na dinâmica local. Porém, nosso segundo objetivo foi realizar o estudo das principais ressonâncias seculares não lineares obtendo uma população de asteroides susceptíveis aos efeitos destas ressonâncias ao longo do cinturão de asteroides. Como um terceiro objetivo, nós estudamos como estas regiões ressonantes podem influir na evolução dinâmica das famílias de asteroides. Em geral, nossos resultados mostraram que as ressonâncias seculares não lineares de tipo g podem ser eficazes na formação de famílias que são cruzadas por este tipo de ressonância e podem aumentar o fluxo de asteroides e NEOS enquanto se encontram próximas a fortes ressonâncias de movimento médio. Como esperado, o efeito a longo prazo sobre as inclinações de asteroides deste tipo de ressonâncias é negligenciável.
In this thesis we introduced a new metric in the domain of proper elements, SDSS-MOC4 colours, WISE geometric albedo, in order to better identify dynamical families and halos. Thus we determine the family of Vesta, which is characterized by its members very associated with basaltic material. It is located in the inner main belt and in the last decades were identified several objects outside the dynamic region of the family. We review the current knowledge of V-type photometric candidates, and we considered the hypotheses of possible sources for the basaltic material located in the central and outer Main-Belt. Was studied the Yarkovsky effect-induced dynamical evolution of clones of all photometric candidates. In our research we have observed that some V-type photometric candidates were found in the regions of the central and outer main belt, at the nonlinear secular resonances g + g5 − 2g6 , which shown to be affecting the dynamical evolution. However our second objective was to study the main nonlinear secular resonances obtaining a population of asteroids most likely to be affected by these resonances along the main belt. We question how these resonant regions can influence the dynamic evolution of asteroid families. This was studied as a third objective and our selection was in accordance with the locations of asteroids with respect to the main nonlinear resonant regions. Overall, our results show that g type resonances can be effective in shaping families that are crossed by this of resonances, and can increase the flux of asteroids and NEOS in nearby powerful mean-motion resonances. As expected, the long-term effect on asteroid inclinations of this type of resonances is essentially negligible.
In this thesis we introduced a new metric in the domain of proper elements, SDSS-MOC4 colours, WISE geometric albedo, in order to better identify dynamical families and halos. Thus we determine the family of Vesta, which is characterized by its members very associated with basaltic material. It is located in the inner main belt and in the last decades were identified several objects outside the dynamic region of the family. We review the current knowledge of V-type photometric candidates, and we considered the hypotheses of possible sources for the basaltic material located in the central and outer Main-Belt. Was studied the Yarkovsky effect-induced dynamical evolution of clones of all photometric candidates. In our research we have observed that some V-type photometric candidates were found in the regions of the central and outer main belt, at the nonlinear secular resonances g + g5 − 2g6 , which shown to be affecting the dynamical evolution. However our second objective was to study the main nonlinear secular resonances obtaining a population of asteroids most likely to be affected by these resonances along the main belt. We question how these resonant regions can influence the dynamic evolution of asteroid families. This was studied as a third objective and our selection was in accordance with the locations of asteroids with respect to the main nonlinear resonant regions. Overall, our results show that g type resonances can be effective in shaping families that are crossed by this of resonances, and can increase the flux of asteroids and NEOS in nearby powerful mean-motion resonances. As expected, the long-term effect on asteroid inclinations of this type of resonances is essentially negligible.
Descrição
Palavras-chave
Asteroides de tipo-V, Ressonâncias seculares não lineares, V-type asteroids, Non-linear secular resonances