Friedmann model with viscous cosmology in modified f(R,T)f(R,T) gravity theory


In this paper, we introduce bulk viscosity in the formalism of modified gravity theory in which the gravitational action contains a general function f(R,T)f(R,T), where RR and TT denote the curvature scalar and the trace of the energy-momentum tensor, respectively within the framework of a flat Friedmann-Robertson-Walker model. As an equation of state for prefect fluid, we take p=(γ1)ρp=(\gamma-1)\rho, where 0γ20 \leq \gamma \leq 2 and viscous term as a bulk viscosity due to isotropic model, of the form ζ=ζ0+ζ1H\zeta =\zeta_{0}+\zeta_{1}H, where ζ0\zeta_{0} and ζ1\zeta_{1} are constants, and HH is the Hubble parameter. The exact non-singular solutions to the corresponding field equations are obtained with non- viscous and viscous fluids, respectively by assuming a simplest particular model of the form of f(R,T)=R+2f(T)f(R,T) = R+2f(T), where f(T)=αTf(T)=\alpha T ( α\alpha is a constant). A big-rip singularity is also observed for γ<0\gamma<0 at a finite value of cosmic time under certain constraints. We study all possible scenarios with the possible positive and negative ranges of α\alpha to analyze the expansion history of the universe. It is observed that the universe accelerates or exhibits transition from decelerated phase to accelerated phase under certain constraints of ζ0\zeta_0 and ζ1\zeta_1. We compare the viscous models with the non-viscous one through the graph plotted between scale factor and cosmic time and find that bulk viscosity plays the major role in the expansion of the universe. A similar graph is plotted for deceleration parameter with non-viscous and viscous fluids and find a transition from decelerated to accelerated phase with some form of bulk viscosity.Comment: 19 pages, 3 figures, the whole paper has been revised to improve the quality of paper. Some references added. arXiv admin note: text overlap with arXiv:1307.4262 by other author

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