Later, small anisotropies gradually grew and condensed the homogeneous universe into stars, galaxies and larger structures.
2.
WMAP indicates ( Figure 1 ) a smooth, homogeneous universe with density anisotropies of 10 parts per million.
3.
Prior to structure formation, e . g ., Friedmann cosmology solutions to general relativity describe a homogeneous universe.
4.
In a homogeneous universe that contrast just doesn't exist . ( The universe actually could still collapse into a singularity.
5.
Before this epoch, the evolution of the universe could be understood through linear cosmological perturbation theory : that is, all structures could be understood as small deviations from a perfect homogeneous universe.
6.
Guth's original formulation was problematic, as there was no consistent way to bring an end to the inflationary epoch and end up with the hot, isotropic, homogeneous universe observed today.
7.
The evolution of the scale factor is a dynamical question, determined by the equations of general relativity, which are presented in the case of a locally isotropic, locally homogeneous universe by the Friedmann equations.
8.
The original proposal of inflation is, the exponentially growing phase ends via the nucleation of Coleman-de Luccia bubbles with a low vacuum energy, these bubbles collide and thermalize, leaving a homogeneous universe with high temperature.
मोबाइल