Interacting ghost dark energy models with variableGand Λ

Abstract

In this paper we consider several phenomenological models of variable Λ. Model of a flat Universe with variable Λ and G is accepted. It is well known, that varying G and Λ gives rise to modified field equations and modified conservation laws, which gives rise to many different manipulations and assumptions in literature. We will consider two component fluid, which parameters will enter to Λ. Interaction between fluids with energy densities ρ1 and ρ2 assumed as Q = 3Hb(ρ1 + ρ2). We have numerical analyze of important cosmological parameters like EoS parameter of the composed fluid and deceleration parameter q of the model. *

Chaotic universe model

“…In order to obtain the coupling interaction equation we follow belove theoretical procedure. Based on the Friedman-Robertson-Walker metric, the interaction between dark matter and dark energy can be given as follows:where Q is arbitrary coupling function and subscript stands for a generic dark energy model to be specified 23–41 . The conservation equations are subject to the Friedman constraint…”

Reconstructing QCD ghost f(R,T) models

“…They fitted this model with observational data including SNeIa, BAO, BBN, the Hubble parameter data and found that the modified GDE model, without having the two fundamental cosmological puzzles, like the ΛCDM fit the astronomical data very well. Sadeghi et al (2013) discussed the flat universe model with varying G and Λ in the presence of modified GDE model (31). In (Karami et al 2013b), modified GDE scalar field models has been discussed in FRW universe with both interaction and viscosity.…”

Stability and interacting f(T, T ) gravity with modified Chaplygin gas

“…In order to describe dark energy model, numerous studies have been performed in isotropic space-time such as scalar fields (quintessence, phantom, tachyon and etc.) [6][7][8][9][10][11][12][13][14][15][16][17][18][19][20][21][22][23], modified gravity models [24][25][26][27][28][29][30][31], holographic models [32][33][34][35][36][37][38][39][40], interacting models [41][42][43][44][45][46][47][48][49][50][51][52], bouncing model [53][54][55...…”