An Interacting Scenario for Dark Energy in Bianchi Type-I Universe

TL;DR

This paper investigates the interaction between dark energy and dark matter within an anisotropic Bianchi type I universe, analyzing the evolution of the dark energy equation of state and constraining anisotropy using observational data.

Contribution

It derives the dark energy equation of state in both interacting and non-interacting scenarios in anisotropic spacetime and examines their future behavior with observational constraints.

Findings

Dark energy EoS varies from phantom to quintessence depending on anisotropy.

In interacting case, EoS remains in the quintessence region.

EoS tends to -1 at late times, resembling a cosmological constant.

Abstract

We study the interaction between dark energy (DE) and dark matter (DM) in the scope of anisotropic bianchi type I space-time. First we derive the general form of the dark energy equation of state parameter (EoS) in both non-interacting and interacting cases and then we examine it's future by applying a hyperbolic scale factor. It is shown that in non-interacting case, depending on the value of the anisotropy parameter $K$, the dark energy EoS parameter is varying from phantom to quintessence whereas in interacting case EoS parameter vary in quintessence region. However, in both cases the dark energy EoS parameter $\omega^{de}$, ultimately (i. e at $z=-1$) tends to the cosmological constant ($\omega^{de}=-1$). Moreover, we fixed the cosmological bound on the anisotropy parameter $K$ by using the recent observational data of Hubble parameter.