Cosmic evolution in the background of R (1 + αQ) gravity

Abstract

In this paper, we discuss the cosmic evolution in a modified theory involving non-minimal interaction of geometry and matter, labeled as [Formula: see text] gravity, where [Formula: see text] is the non-minimal interaction term. First, we develop the dynamical [Formula: see text] field equations for Friedmann–Lemaitre–Robertson–Walker (FLRW) spacetime and then by using divergence of these equations, we explore its interesting outcome of non-conserved energy–momentum tensor (EMT). The presence of geometry matter coupling in such theories results in non-geodesic test particles motion and hence causes an additional force orthogonal to four-velocity of these particles. By taking these interesting features into account along with a particular choice of Lagrangian [Formula: see text], we explore the resulting expression of energy density. Further, the free model parameters are constrained using energy condition bounds where it is concluded that these values of free parameters are compatible with the recent data.

Isotropic exact solutions via Noether symmetries in f(R, T, R μ ν T μ ν ) gravity

“…The fractional densities meet with Planck limitations whereas the consistency disturbs as time passes due to the dominance of matter fractional density. Zubair et al [31] investigated cosmic evolution using particular f (R, Q) model and power-law Hubble parameter without using Noether Symmetry approach. They constructed model constraints that refer to ΛCDM limit and explain current accelerated expansion.…”