Physical causes of energy-density inhomogenization and stability of energy-density homogeneity in relativistic self--gravitating fluids

TL;DR

This paper investigates the physical factors leading to energy-density inhomogeneities in self-gravitating fluids and examines how these inhomogeneities evolve from initially uniform distributions, highlighting the roles of the Weyl tensor, pressure anisotropy, and dissipation.

Contribution

It identifies the key physical factors responsible for energy-density inhomogeneities and analyzes their evolution in various scenarios, including dissipative processes and non-local effects.

Findings

Energy-density inhomogeneities are linked to Weyl tensor and pressure anisotropy.

Dissipative fluxes and relaxational processes influence inhomogeneity development.

Different cases show how initial homogeneity can evolve into inhomogeneity.

Abstract

We identify the factors responsible for the appearance of energy-density inhomogeneities in a self-gravitating fluid, and describe the evolution of those factors from an initially homogeneous distribution. It is shown that a specific combination of the Weyl tensor and/or local anisotropy of pressure and/or dissipative fluxes entails the formation of energy-density inhomogeneities. Different cases are analyzed in detail and in the particular case of dissipative fluids, the role of relaxational processes as well as non-local effects are brought out.