Randall-Sundrum Model in the Presence of a Brane Bulk Viscosity

TL;DR

This paper investigates how bulk viscosity in the cosmic fluid affects the dynamics of a Randall-Sundrum brane universe, deriving modified Friedmann equations and analyzing their solutions in different cosmological regimes.

Contribution

It derives the five-dimensional Friedmann and energy conservation equations with bulk viscosity on a Randall-Sundrum brane, exploring their implications in various cosmological scenarios.

Findings

Viscous effects can be significant at the Planck time.

Derived equations applicable in low-energy, matter-dominated, and radiation-dominated regimes.

Numerical estimates suggest bulk viscosity influences early universe dynamics.

Abstract

The presence of a bulk viscosity for the cosmic fluid on a single Randall-Sundrum brane is considered. The spatial curvature is assumed to be zero. The five-dimensional Friedmann equation is derived, together with the energy conservation equation for the viscous fluid. These governing equations are solved for some special cases: (i) in the low-energy limit when the matter energy density is small compared with brane tension; (ii) for a matter-dominated universe, and (iii) for a radiation-dominated universe. Rough numerical estimates, for the extreme case when the universe is at its Planck time, indicate that the viscous effect can be significant.