Abstract
In this paper, we have studied the spatially homogeneous and anisotropic Bianchi type-III cosmological model in the presence of pressureless matter and Holographic dark energy within the framework of f(R,T) gravity. We have constructed a cosmological model with an appropriate choice of function f(T). Field equations are solved using the relation between the metric potentials A=Cn and using a simple power-law form of a metric potential C=tn. The main objective behind this paper is to explore some physically significant discussions on the evolution of the universe. It is observed that the Hubble parameter H, scalar expansion θ and shear scalar σ diverge at the initial epoch while they approach zero for a large value of time and the anisotropic parameter Am is constant. The negative value of the deceleration parameter indicates the present acceleration of the universe.
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