Accelerating dark energy models in bianchi Type-V space-time

TL;DR

This paper presents new exact solutions for dark energy in Bianchi type-V space-time, showing how different models can describe the universe's transition from deceleration to acceleration and align with observational data.

Contribution

It introduces specific exact solutions with a chosen scale factor that models the universe's transition from deceleration to acceleration, including quintessence and phantom scenarios.

Findings

Models reproduce current and future universe evolution.

Quintessence and phantom models approach isotropy at late times.

Cosmic jerk parameter aligns with recent astrophysical observations.

Abstract

Some new exact solutions of Einstein's field equations in a spatially homogeneous and anisotropic Bianchi type-V space-time with minimally interaction of perfect fluid and dark energy components have been obtained. To prevail the deterministic solution we choose the scale factor $a(t) = \sqrt{t^{n}e^{t}}$, which yields a time dependent deceleration parameter (DP), representing a model which generates a transition of the universe from the early decelerating phase to the recent accelerating phase. We find that for $n \geq 1$, the quintessence model is reproducible with present and expected future evolution of the universe. The other models (for $n < 1$), we observe the phantom scenario. The quintessence as well as phantom models approach to isotropy at late time. For different values of $n$, we can generate a class of physically viable DE models. The cosmic jerk parameter in our descended model is also found to be in good concordance with the recent data of astrophysical observations under appropriate condition. The physical and geometric properties of spatially homogeneous and anisotropic cosmological models are discussed.