Inhomogeneous anisotropic cosmology

Quintessence inhomogeneous cosmology

The Einstein–Klein–Gordon field equations are solved in a inhomogeneous shear–free universe containing a material fluid, a self–interacting scalar field, a variable cosmological term, and a heat flux. A quintessence– dominated scenario arises with a power–law accelerated expansion compatible with the currently observed homogeneous universe.

Anisotropic and Inhomogeneous Cosmologies

Cosmology with inhomogeneous magnetic fields

We review spacetime dynamics in the presence of large-scale electromagnetic fields and then consider the effects of the magnetic component on perturbations to a spatially homogeneous and isotropic universe. Using covariant techniques, we refine and extend earlier work and provide the magnetohydrodynamic equations that describe inhomogeneous magnetic cosmologies in full general relativity. Speci...

Asymptotic isotropization in inhomogeneous cosmology

In this paper we investigate asymptotic isotropization. We derive the asymptotic dynamics of spatially inhomogeneous cosmological models with a perfect fluid matter source and a positive cosmological constant near the de Sitter equilibrium state at late times, and near the flat FL equilibrium state at early times. Our results show that there exists an open set of solutions approaching the de Si...

Anisotropic ’hairs’ in string cosmology

In most models, inflation is driven by the potential energy of a scalar field. This has similar effects as adding vacuum energy or, equivalently, a positive cosmological constant. For these models Wald [1] proved a cosmic no hair theorem, which implies that an initial shear is inflated away [2]. A couple of years ago, a new mechanism of inflation has been proposed, where inflation is due to the...