Abstract
This paper deals with the bulk viscous Bianchi type-V cosmological model with an exponential scale factor in Lyra geometry based on f(R, T) gravity, by considering a time dependent displacement field. To determine the nature and physical properties of the model, we considered Harko et al. (Harko et al., Phys. Rev. D, 2011, 84, 024020) [proposed the linear form f(R, T) = f1(R) + f2(T)], in which the barotropic equation of state for pressure, density, and bulk viscous pressure is proportional to energy density. The kinematical properties of the model are also discussed in the presence of bulk viscosity. Evolution of energy conditions is also studied and examined the behaviour of that in examined in order to explain the late-time cosmic acceleration.
Highlights
As evidenced by various observational data from Garnavich (Garnavich et al, 1998a; Garnavich et al, 1998b), Riess (Riess et al, 1998) and Perlmutter (Perlmutter et al, 1997; Perlmutter et al, 1999) the expansion of the universe is accelerating
A completely spatially homogeneous and anisotropic Bianchi type-V cosmological model has been discussed in the presence of a bulk viscous fluid based on Lyra geometry, with an exponential form of scale factor
We employed a barotropic equation of state for pressure and energy density to determine the nature and deterministic solution of the highly non linear differential equation
Summary
As evidenced by various observational data from Garnavich (Garnavich et al, 1998a; Garnavich et al, 1998b), Riess (Riess et al, 1998) and Perlmutter (Perlmutter et al, 1997; Perlmutter et al, 1999) the expansion of the universe is accelerating. In a recent cosmological model, f(R) gravity has become a more attractive theory to represent the behaviour of the expansion of the universe, known as f(R, T) gravity, where the matter Lagrangian is given by an arbitrary function of the Ricci scalar R and the trace of the energy momentum tensor T. In which R~, T, and Lm respectively denote the function of Ricci scalar R, the trace of the stress tensor, and the Lagrangian density of matter, where the stress- energy tensor of the matter is defined as Such that its trace is given by T = gijTij Consider that the matter Lagrangian Lm depends only on the metric tensor components gij and does not depend on its derivatives, it reduces to gijLm. by varying the action S in Eq 2 with respect to metric tensor gij, the gravitational field equations of f(R~, T) gravity are obtained as fR~. The displacement vector field is φi (0, 0, 0, β(t)) and h (8πμ−cμ2c2) is taken as unity
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