DARK ENERGY COSMOLOGICAL MODEL FOR BIANCHI TYPE III SPACE-TIME WITH PERFECT FLUID

B Mishra,P.K Sahoo,Ch.B Siddarth Varma

doi:10.12732/ijpam.v99i1.9

Abstract

In this paper, the problem of diagonal Bianchi type III space-time is investigated in scale invariant theory with dark energy. The matter field is considered in the form of perfect fluid. The field equations for scale invariant theory has been solved by applying a variation law for generalized Hubble's parameter (Nuovo Cimento B 74:182, 1983). The gauge function depends on time coordinate only (Dirac gauge). The cosmological model is constructed, its physical and kinematical properties are discussed.

Highlights

Soleheim (1966) was the first to indicate that the universe is presently in a state of accelerated expansion
Approaches to account for the late time cosmic acceleration fall into two representative categories: one is to introduce dark energy (DE) in the right hand side of the Einstein equation in the framework of general relativity (Kamionkowski 2009; Amendola and Tsujikawa 2010, Kunz 2012)
Motivated with the work of Nojiri and Odintsov (2011), We have considered the scale invariant theory in dark energy, which theory necessarily includes an arbitrary gauge function

Summary

Introduction

Soleheim (1966) was the first to indicate that the universe is presently in a state of accelerated expansion. Holman and Naidu (2005)observed that their model is consistent with the most recent SNIa data, the WMAP results as well as the constraints coming from measurements of the power spectrum They considered both, the case where the dark fluid is smooth Motivated with the work of Nojiri and Odintsov (2011), We have considered the scale invariant theory in dark energy, which theory necessarily includes an arbitrary gauge function. Bianchi type III space-time with dark energy has not been considered, so far, in the scale invariant theory of gravitation. In this paper, we have constructed the Bianchi type III cosmological model with dark energy in scale invariant theory.

Metric and Field Equations

C β44 β β42 β2

Solutions of the Field Equations

Some Physical and Kinematical Properties of the Model

Findings

Conclusions