Simulações de ram pressure em aglomerados de galáxias

• Ano de defesa: 2022
• Autor(a) principal: Grinberg, Caroline Aparecida Fernandes de Oliveira
• Tipo de documento: Dissertação
• Tipo de acesso: Acesso aberto
• Idioma: por
• Instituição de defesa: Universidade Tecnológica Federal do Paraná; Curitiba; Brasil; Programa de Pós-Graduação em Física e Astronomia; UTFPR
• Palavras-chave em Português: Galáxias - Aglomerados; Estrelas - Formação; Métodos de simulação; Astrofísica; Pressão; Potencial gravitacional; Galaxies - Clusters; Stars - Formation; Simulation methods; Astrophysics; Pressure; Gravitational potential; CNPQ::CIENCIAS EXATAS E DA TERRA::ASTRONOMIA; Física
• Link de acesso: http://repositorio.utfpr.edu.br/jspui/handle/1/30206

Numerical simulations are an excellent tool to study astrophysical phenomena, considering the huge scales of time and space in which they occur. Ram pressure is an effect that galaxies crossing the intracluster medium (ICM) experience, causing the removal of the galaxy’s gas, i.e. ram pressure stripping (RPS), and in more intense cases, a gas tail forms behind it, characterizing the só-called “jellyfish galaxy”, in which most or all of the gas is removed. Exploring such effects can help us understand certain galaxy evolution processes. Using the GADGET-2 and GADGET-3 codes, we ran hydrodynamical -body simulations of a galaxy moving face-on or edge-on towards the center of a galaxy cluster, including star formation in some cases, with the aim of analyzing the effects of ram pressure in each scenario. Regarding these simulations, we characterize properties of the tail of the jellyfish galaxy, such as length and mass, investigate correlations between different variables related to the phenomenon, represent the position of the particles in a phase space, and verify characteristics of the star formation in the gas tail. We found similar gas masses in the tails of galaxies moving face-on to those moving edge-on, and this value is lower in galaxies with star formation. We identified strong correlations between the ram pressure and the gas density, for both face-on and edge-on cases, which is significant from an observational point of view, since the density can be obtained more easily than the gas velocity of the ICM gas, necessary to measure the ram pressure. We conclude that the variation between the face-on and edge-on cases leads to differences in the shape of the tail of jellyfish galaxies, which does not significantly affect the mass of gas removed. We also conclude that some of the removed gas converts to stars in the tail, só star-forming galaxies have less tail gas mass.