Interacting Two-Fluid Viscous Dark Energy Models In Non-Flat Universe

Abstract

We study the evolution of the dark energy parameter within the scope of a spatially non-flat and isotropic Friedmann-Robertson-Walker (FRW) model filled with barotropic fluid and bulk viscous stresses. We have obtained cosmological solutions which exhibit without a big rip singularity. It is concluded that in both non-interacting and interacting cases non-flat open universe crosses the phantom region. We find that during the evolution of the universe, the equation of state (EoS) for dark energy ${\omega }_D$ changes from ${\omega }_D^{eff}<-1$ to ${\omega }_D^{eff}>-1$, which is consistent with recent observations.

10 Pages, 4 Figures

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Cited by in corpus (6)

• Two-fluid atmosphere from decelerating to accelerating FRW dark energy models
• Two-Fluid Dark Energy Models in Bianchi Type-III Universe with Variable Deceleration Parameter
• Phantom Instability of Viscous Dark Energy in Anisotropic Space-Time
• Interacting Viscous Dark Energy in Bianchi Type-I Universe
• An Interacting Scenario for Dark Energy in Bianchi Type-I Universe
• Interacting Viscous Dark Energy in Bianchi Type-III Universe