Viscous Dark Energy In Bianchi Type V Space-Time

TL;DR

This paper explores the effects of viscosity on dark energy within anisotropic Bianchi type V space-time, deriving equations, comparing models, and constraining parameters using observational Hubble data.

Contribution

It introduces a detailed analysis of viscous dark energy in Bianchi V space-time, including scalar field reconstructions and observational constraints.

Findings

Viscous dark energy affects the EoS parameter evolution.

Conditions for mapping Bianchi V to FRW are identified.

Bulk viscosity influences dark energy behavior and observational fits.

Abstract

We study the behavior of dark energy (DE) in the scope of anisotropic Bianchi type V (BV) space-time. First we derive Friedmann-Like Equations, then we compare the dark energy equation of state (EoS) parameter for viscous and non-viscous dark energy and make a correspondence between DE and quintessence and phantom descriptions of non-viscous and viscous dark energy and reconstruct the potential of these two scalar fields. The late time behavior of EoS parameter through a thermodynamical study has also been investigated. Finally, we investigate the conditions under which BV space-time can be mapped into the FRW and how the bulk viscose coefficient may affect dark energy EoS parameter of our $\omega\mbox{BV}$ Model with constraints from 28 Hubble parameter, $H(z)$, measurements at intermediate redshifts $0.07\leq z\leq 2.3$.