Bulk viscosity, interaction and the viability of phantom solutions

TL;DR

This paper investigates a bulk viscosity cosmological model with dark matter and dark energy, including interactions, finding constraints that favor quintessence over phantom solutions and aligning with observational data.

Contribution

It introduces a detailed analysis of bulk viscosity effects and interactions in dark matter and dark energy, deriving bounds that restrict late-time phantom solutions and favor quintessence.

Findings

Bounds on bulk viscosity compatible with matter-dominated era

Late-time phantom solutions are eliminated by constraints

Interaction parameter bounds align with observational data

Abstract

We study the dynamics of a bulk viscosity model in the Eckart approach for a spatially flat Friedmann-Robertson-Walker (FRW) universe. We have included radiation and dark energy, assumed as perfect fluids, and dark matter treated as an imperfect fluid having bulk viscosity. We also introduce an interaction term between the dark matter and dark energy components. Considering that the bulk viscosity is proportional to the dark matter energy density and imposing a complete cosmological dynamics, we find bounds on the bulk viscosity in order to reproduce a matter-dominated era (MDE). This constraint is independent of the interaction term. Some late time phantom solutions are mathematically possible. However, the constraint imposed by a MDE restricts the interaction parameter, in the phantom solutions, to a region consistent with a null value, eliminating the possibility of late time stable solutions with $w<-1$. From the different cases that we study, the only possible scenario, with bulk viscosity and interaction term, belongs to the quintessence region. In this latter case, we find bounds on the interaction parameter compatible with latest observational data.