Cosmological nonlinear structure formation in full general relativity

Understand

We perform numerical evolutions of cosmological scenarios using a standard general relativistic code in spherical symmetry.

• We concentrate on two different situations: initial matter distributions that are homogeneous and isotropic, and perturbations to those that respect the spherical symmetry.
• As matter models we consider the case of a pressureless perfect fluid, i.e.
• dust, and the case of a real massive scalar field oscillating around the minimum of the potential.