Viscous Dark Energy and Phantom Field in An Anisotropic Universe

Abstract

In this paper we have investigated the general form of viscous and non-viscous dark energy equation of state (EoS) parameter in the scope of anisotropic Bianchi type I space-time. We show that the presence of bulk viscosity causes transition of ${\omega }^{de}$ from quintessence to phantom but the phantom state is an unstable state (as expected) and EoS of DE tends to $-1$ at late time. Then we show this phantomic description of the viscous dark energy and reconstruct the potential of the phantom scalar field. It is found that bulk viscosity pushes the universe to a darker region. We have also shown that at late time $q\sim -{\Omega }^{de}$.

10 pages

References in corpus (5)

• Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation
• Cardy-Verlinde formula in FRW Universe with inhomogeneous generalized fluid and dynamical entropy bounds near the future singularity
• Viscous dark energy and generalized second law of thermodynamics
• Phantom Instability of Viscous Dark Energy in Anisotropic Space-Time
• Interacting Viscous Dark Energy in Bianchi Type-I Universe

Cited by in corpus (2)

• Viscous Dark Energy In Bianchi Type V Space-Time
• Israel-Stewart approach to viscous dissipative extended holographic Ricci dark energy dominated universe