Phantom Instability of Viscous Dark Energy in Anisotropic Space-Time

Abstract

Phantom dark energy is a proposal that explains the current observations that mildly favor the equation of state of dark energy ${\omega }^{de}$ crossing -1 at 68% confidence level. However, phantom fields are generally ruled out by ultraviolet quantum instabilities. To overcome this discrepancy, in this paper we propose a mechanism to show that how the presence of bulk viscosity in the cosmic fluid can temporarily drive the fluid into the phantom region ($\omega <-1$). As time is going on, phantom decays and ultimately ${\omega }^{de}$ approaches to -1. Then we show these quintessence and phantom descriptions of non-viscous and viscous dark energy and reconstruct the potential of these two scalar fields. Also a diagnostic for these models are performed by using the statefinder pairs $\{s,r\}$. All results are obtained in an anisotropic space-time which is a generalization of FLRW universe.

13 pages, 6 figures, Astrophysics and Space Science, 2013

References in corpus (6)

• Cosmology and the Fate of Dilatation Symmetry
• Interacting holographic generalized Chaplygin gas model
• Interacting Holographic Phantom
• Bianchi Type-I Anisotropic Dark Energy Models with Constant Deceleration Parameter
• The null energy condition and instability
• Viscous dark energy and generalized second law of thermodynamics

Cited by in corpus (5)

• Viscous Dark Energy In Bianchi Type V Space-Time
• Anisotropic cosmological models with two fluids
• An Interacting Scenario for Dark Energy in Bianchi Type-I Universe
• Interacting Viscous Dark Energy in Bianchi Type-III Universe
• Viscous effect in the late time evolution of phantom universe