FRIEDMANN–ROBERTSON–WALKER BRANE COSMOLOGICAL EQUATIONS FROM THE FIVE-DIMENSIONAL BULk (A)dS BLACK HOLE

Abstract

In the first part of this work we review the equations of motion for the brane presented in Friedmann-Robertson-Walker (FRW) form, when bulk is 5-dimensional (A)dS Black Hole. The spacelike (timelike) FRW brane equations are considered from the point of view of their representation in the form similar to 2-dimensional CFT entropy, so-called Cardy-Verlinde (CV) formula. The following 5-dimensional gravities are reviewed: Einstein, Einstein-Maxwell and Einstein with brane quantum corrections. The second part of the work is devoted to study FRW brane equations and their representation in CV form, brane induced matter and brane cosmology in Einstein-Gauss-Bonnet (GB) gravity. In particular, we focus on the inflationary brane cosmology. The energy conditions for brane matter are also analyzed. We show that for some values of GB coupling constant (bulk is AdS BH) the brane matter is not CFT. Its energy density and pressure are not always positive. The appearence of logarithmic corrections in brane cosmology is discussed.

Pilgrim dark energy in f(T,T G ) cosmology

“…2006bNojiri at al. ,2006cCognola et al 2006aCognola et al ,2006bNojiri and Odintsov 2005a,2005b,2005c,2006dNojiri et al 2005aNojiri et al ,2005bNojiri et al 2002;Cvetic at al. 2002;Noji et al 2009;Nojiri and Odintsov 2008;Nojiri and Odintsov 2003 ).…”

Energy conditions in modified f(G) gravity

“…There has been an interested results found on the exploration of dark source terms on the dynamical evolution of stellar systems in Einstein-Λ [26], f (R) [27], f (R, T ) [28] (T is the trace of energy momentum tensor) and f (R, T, R µν T µν ) gravity [29]. Among MGTs, available in the literature, the one is Gauss Bonnet (GB) gravity which has received great attraction [30][31][32][33][34][35][36][37][38][39][40] and is named as f (G) gravity, where…”

“…The equation of motion for this gravity is required to be coupled with some scalar field or f (G) must be some arbitrary function of G. This MGT could help out in the study of inflationary era, transition of acceleration from deceleration regimes, passing tests induced by solar system experiments and crossing phantom divide line for different viable f (G) models [32,33]. It is also seen that the GB gravity is less constrained than f (R) gravity [34].…”

Phase space of generalized Gauss-Bonnet dark energy

“…Other aspects of modified GB gravity, such as the possibility of describing the inflationary era, transition from deceleration phase to acceleration phase, crossing the phantom-divide-line, and passing the solar system test have been discussed in [9]. The natural generalization of action (3) is the generalized Gauss-Bonnet dark energy, which have been introduced in [7,10] :…”