Energy conditions in $$f(\mathcal {G},T)$$ f ( G , T ) gravity

Abstract

The aim of this paper is to introduce a new modified gravity theory named f (G, T ) gravity (G and T are the Gauss-Bonnet invariant and trace of the energy-momentum tensor, respectively) and investigate energy conditions for two reconstructed models in the context of FRW universe. We formulate general field equations, divergence of energymomentum tensor, equation of motion for test particles as well as corresponding energy conditions. The massive test particles follow non-geodesic lines of geometry due to the presence of an extra force. We express the energy conditions in terms of cosmological parameters like the deceleration, jerk, and snap parameters. The reconstruction technique is applied to this theory using de Sitter and power-law cosmological solutions. We analyze the energy bounds and obtain feasible constraints on the free parameters.

Anisotropic Universe inf(G,T)Gravity

“…The field equations can be obtained by varying the action equation (1) with respect to the metric tensor [20] …”

“…This seems to be an issue with some other higher order derivatives theories as well that include higher order terms of energy-momentum tensor. However, to deal with the issue, one can put some constraints to (4) to obtain standard conservation equation [20]. Here we take the spatially homogeneous, anisotropic, LRS Bianchi type space-time…”

“…After inserting the value of GB invariant (20) reduces to differential equations with three unknowns , , and . It would be worthwhile to mention here that many solutions 4 Advances in High Energy Physics can be found using (20).…”

“…Thus, to save ( ) theories, one may include (G) terms. A theory with a similar idea has been recently proposed named as (G, ) gravity [20]. Some interesting work has been done in the recent past using modified GB theories.…”

“…In the context of (G, ) gravity, Sharif and Ikram proved that the massive test particles followed nongeodesic lines of geometry due to the presence of extra force and examined the energy conditions for flat FRW universe [20]. The same authors [31] used reconstruction techniques to reproduce the cosmic evolution corresponding to de Sitter universe, power 2 Advances in High Energy Physics law solutions, and phantom/nonphantom eras in this theory.…”