| Abstract : | The large-scale structure of the universe on a scale of less than 100 Mpc consists of a network of overdense and underdense regions. Studying their evolution, which depends on the initial conditions and dark energy, can be useful in constraining the cosmological parameters. Underdensities, or cosmic voids, especially provide reliable testing grounds for large-scale structure formation, cosmological parameters, and dark energy. In our study, the evolution of an isolated spherical void in a homogeneous, expanding background universe is studied for different models of dark energy. We assumed the initial density profile to be an inverse top-hat density profile and the density contrast corresponding to shell crossing is set to δ = −0.8. We first analyze the void evolution for an Einstein-de Sitter cosmology and later repeat the analysis by including an additional dark energy component in the acceleration equation. We chose two models of dark energy, the Chaplygin gas, and the generalized Chaplygin gas, which are described as perfect fluids filling the universe. We present our progress and discuss our theoretical analysis of the void evolution, plots, numerical analyses, and future work. |
