Simulação da formação da estrutura em "teia" da matéria escura

Abstract

The universe has always been a matter of curiosity and study. For thousands of years the desire to understand its origin and functioning has been with us, and this curiosity has often generated imaginative ideas of cosmology. It was long believed that the Universe was static, that is, ir remainsat rest at larges scales, later theories emerged that it would be expanding but that expansion would be slowing due to the gravitational pull of all the matter contained therein. The theory currently accepted is that the universe in accelerated expansion. It was possible to observe the increase of the recession velocity of galaxies as a function of their distance. The most accepted hypothesis for the cause of the expansion of the universe is the dark energy, a small energy density present in all space generating a negative pressure. On the other hand, the visible matter is not enough to explain a series of observed phenomena, such as the rotational velocity profile of a large number of galaxies and also the evolution of the distribution of matter in the universe that we observe today. The most accepted hypothesis currently capable of explaining this data is dark matter, which interacts very weakly with baryonic matter, in the simplest case, only by gravitational interaction. Although dark matter and dark energy have not been detected directly, one can explore their influence on the formation of the universe through numerical simulations. Thus, what we intend with this work is to delve into the theme of the formation of the large scale structures of the universe through the study of the theoretical basis and the realization of a numerical simulation of the evolution of dark matter governed only by gravitational interaction, from it’s almost homogeneous initial distribution until the appearance of the web-shaped structure. This evolution takes place in an expanding space. For these simulations an open software package dedicated for this purpose and publicly available will be used. The numerical technique used will be that of N-bodies