An interacting and non-interacting two-fluid scenario for dark energy in FRW universe with constant deceleration parameter

Abstract

In this paper we study the evolution of the dark energy parameter within the scope of a spatially homogeneous and isotropic FRW universe filled with barotropic fluid and dark energy. The scale factor is considered as a power law function of time which yields a constant deceleration parameter. We consider the case when the dark energy is minimally coupled to the perfect fluid as well as direct interaction with it. The cosmic jerk parameter in our derived models is consistent with the recent data of astrophysical observations. It is concluded that in non-interacting case, all the three open, close and flat universes cross the phantom region whereas in interacting case only open and flat universes cross the phantom region. We find that during the evolution of the universe, the equation of state (EoS) for dark energy ω D changes from ω D > −1 to ω D < −1, which is consistent with recent observations. A. Pradhan ( )

An Interacting and Non-interacting Two-Fluid Dark Energy Models in FRW Universe with Time Dependent Deceleration Parameter

“…So a number of viable models for dark energy have been constructed. These scenarios include, quintessence [24,25], chameleon [26], K-essence [27,28], which is based on earlier work of K-inflation [29], modified gravity [30][31][32][33][34][35][36], tachyon [37] arising in string theory [38], quintessential inflation [39], Chaplygin gas as well as generalized Chaplygin gas [40][41][42][43][44][45][46], cosmological nuclear energy [47], equation of state (EoS) parameter [48][49][50][51][52][53][54][55], braneworld [56,57] and interacting dark energy models [58][59][60][61][62]. Therefore some form of dark energy whose fractional energy density is about DE = 0.70 must exist in the Universe to drive this acceleration.…”

Accelerating Dark Energy Models in Bianchi Type-v Spacetime

“…This ansatz generalized the one proposed by Amirhashchi et al [52]. In literature it is common to use a constant deceleration parameter [37,38,41,53,21,22] as it duly gives a power law for metric function or corresponding quantity. The motivation to choose such time dependent DP is behind the fact that the universe is accelerated expansion at present as observed in recent observations of Type Ia supernova [1]− [4] and CMB anisotropies [54]− [56] and decelerated expansion in the past.…”

FRW dark energy cosmological model with hybrid expansion law

“…These observations were based on the combination of cosmological datasets coming from CMB anisotropies, luminosity distances of high redshift type Ia supernovae and galaxy clustering. Recently, Amirhashchi et al [29,30], Pradhan et al [31], Saha et al [32], Pradhan [33] and Kumar [34] have made study on FRW based dark energy model in which they considered an interacting and non-interacting two type of fluids, one for barotropic matter and other for dark energy.…”