Quintessence Cosmology with an Effective Λ -Term in Lyra Manifold

Abstract

In this paper, we study quintessence cosmology with an effective Λ-term in Lyra manifold. We consider three different models by choosing variable Λ depend on time, the Hubble parameter and the energy density of dark matter and dark energy. Dark energy assumed as quintessence which interacts with the dark matter. By using numerical analysis we investigate behavior of cosmological parameters in three different models and compare our results with observational data. Statefinder diagnostic is also performed for all models.

Exact Cosmological Models with Yang–Mills Fields on Lyra Manifold

“…It is useful to mention that the conservation equation for YM field, T k i;k = 0, for EMT of YM field in form (21), namely ρg + 3H(ρ g + p g ) = 0, (22) where H = ȧ/a is the Hubble parameter, is satisfied identically by our solution (21). As can be seen, the reason of such satisfaction of the continuity equation in the case k = 0 is nothing more than the equality of ρ g and p g to zero according to (21).…”

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...…”

Toy Models of Universe with an Effective VaryingΛ-Term in Lyra Manifold

“…But such theories with different forms of modifications still should pass experimental tests, because they contain ghosts, finite-time future singularities e.t.c, which is the base of other theoretical problems. One of the well studied Dark Energy models is a quintessence model [35]- [43], which is a scalar field model described by a field φ and V (φ) potential and it is the simplest scalar-field scenario without having theoretical problems such as the appearance of ghosts and Laplacian instabilities. Energy density and pressure of quintessence DE given as…”