Interacting viscous dark energy in a Bianchi type-III universe

Abstract

In this paper we study the evolution of the equation of state of viscous dark energy in the scope of Bianchi type III space-time. We consider the case when the dark energy is minimally coupled to the perfect fluid as well as direct interaction with it. The viscosity and the interaction between the two fluids are parameterized by constants ζ0 and σ respectively. We have made a detailed investigation on the cosmological implications of this parametrization. To differentiate between different dark energy models, we have performed a geometrical diagnostic by using the statefinder pair {s, r}.PACS numbers: 98.80.Es, 98.80-k, 95.36.+x Key words: Bianchi type-III models, dark energy, statefinderRecently the dissipative DE models in which the negative pressure, responsible for the current acceleration, is an effective bulk viscous pressure have been proposed in order to avoid the occurrence of the big rip (McInnes

Constraining Bianchi type I universe with type Ia supernova and H(z) data

“…Very recently Authors of Ref [21] have studied some DE models in the scope of LTB spaceime. There are increasing interest in the study of dark energy models in the scope of anisotropic Bianchi spacetimes (for example see [22,23,24,25,26,26,27,28] also see [29,30] for recent review). Recently, we have studied viscous dark energy in the scope of Bianchi type V spacetime [31].…”