Study of thermal stability for different dark energy models

Abstract

In the present work, we have made an attempt to investigate the dark energy possibility from the thermodynamical point of view. For this purpose, we have studied thermodynamic stability of three popular dark energy models in the framework of an expanding, homogeneous, isotropic and spatially flat FRW Universe filled with dark energy and cold dark matter. The models considered in this work are Chevallier-Polarski-Linder (CPL) model, Generalized Chaplygin Gas (GCG) model and Modified Chaplygin Gas (MCG) model. By considering the cosmic components (dark energy and cold dark matter) as perfect fluid, we have examined the constraints imposed on the total equation of state parameter (wT ) of the dark fluid by thermodynamics and found that the phantom nature (wT < −1) is not thermodynamically stable. Our investigation indicates that the dark fluid models (CPL, GCG and MCG) are thermodynamically stable under some restrictions of the parameters of each model. PACS numbers: 98.80.Hw, 98.80.Jk, 98.80.Cq, 05.70.Ce.

Universe consisting of diffusive dark fluids: thermodynamics and stability analysis

“…Subsequently, Chakraborty and collaborators [35][36][37][38] in a series of works have shown the stability criteria for different type of dark fluids and have presented the stability conditions (in tabular form) for different ranges of the equa-tion of state parameter. The present work is an extension of the interacting dark fluid model.…”

Cosmic evolution and thermal stability of Barrow holographic dark energy in nonflat Friedmann-Robertson-Walker Universe

“…Further aspects are still to be considered: first, one could investigate how the present study interfaces with the results of [81], where it has been shown that some DE models, such as Chevallier-Polarski-Linder model, Generalized Chaplygin Gas and Modified Chaplygin Gas are thermodynamically stable for certain values of the model parameters. A potential path to explore is to see whether thermal stability for BHDE is achieved by considering different IR cutoffs and/or generalized interactions between the dark sectors of the cosmos.…”