Interacting Models of Generalised Chaplygin Gas and Modified Chaplygin Gas with Barotropic Fluid

TL;DR

This paper explores two cosmological models with interacting generalized and modified Chaplygin gases and barotropic fluids, analyzing their effects on cosmic acceleration, key parameters, and observational consistency.

Contribution

It introduces explicit energy density functions for two interacting Chaplygin gas models and studies their impact on cosmic evolution and observational parameters.

Findings

Identified redshift for transition from deceleration to acceleration.

Compared effects of different interaction coefficients on cosmological parameters.

Analyzed dependence of cosmological evolution on dark energy and fluid parameters.

Abstract

In this letter we consider two different models of our present universe. We choose the models which are consisting different sets of two seperate fluids. The first one of each set tries to justify the late time acceleration and the second one is barotropic fluid. The former model considers our present time universe to be homogeneously filled up by Generalized Chaplygin Gas which is interacting with barotropic fluid. On the other hand, the latter model considers that the cosmic acceleration is generated by Modified Chaplygin Gas which is interacting with matter depicted by barotropic equation of state. For both the models, we consider the interaction term to vary proportionally with Hubble's parameter as well as with the exotic matter/dark energy's energy density. We find an explicit function form of the energy density of the cosmos which is found to depend on different cosmological parameters like scale factor, dark energy and barotropic fluid's EoS parameters and other constants like interacting constants etc. We draw curves of effective EoS-s, different cosmological parameters like deceleration parameter $q$, statefinder parameters $r$ and $s$ with repect to the redshift $z$ (for different values of dark energy and barotopic fluid parameters) and study them thoroughly. We compare two models as well as the nature of dependencies on these models' interaction coefficients. We point out the particular redshift for which the universe may transit from a deceleration to acceleration phase. We tally all these values with different observational data. Here we also analyse how this value of particular redshift does change for different values of interaction coefficients and different dark energy models.