Late-time acceleration in f(Q) gravity: Analysis and constraints in an anisotropic background

Constraining Parameters for the Accelerating Models in Symmetric Teleparallel Gravity

“…( 24), H 0 +1 > 0 and the signature of γ will not have any effect on its expanding behaviour. For = 1, we can obtain [33] and we consider > −1 to avoid the singularity as well as to maintain positiveness of H(z). Using the scale factor and redshift relation, a = 1 1+z , Eq.…”

“…The behavior of the dynamical parameters of f (Q) gravity constrained by the scale factor and model parameters was studied in Refs. [31][32][33]). Maurya et al [34] investigated the gravitationally decoupled anisotropic solutions for the strange stars in the framework of gravity by utilizing the CGD technique.…”

A model-independent method with phantom divide line crossing in Weyl-type f(Q,T) gravity

“…As SNe Ia measurements and other astronomical observations suggest that the cosmos is accelerating, a timedependent deceleration parameter is necessary to explain the transition from deceleration expansion in the past to accelerating expansion in the present. In line with this idea, different parametrizations have argued that deceleration parameter is time-dependent in order to examine various cosmological difficulties [42][43][44][45][46][47][48][49][50][51][52][53]. Motivated by the preceding debate, we use a generalization form of the deceleration parameter proposed in Eq.…”

Anisotropic Universe in $f(Q,T)$ gravity, a novel study

“…One must relax the assumption of FLRW geometry from the very start and investigate the transition from an anisotropic and inhomogeneous state to the observed level of homogeneity and isotropy. A number of recent articles in several modified gravity theories can be cited [55][56][57][58][59][60] for a diverse field of investigation in the background of anisotropic Bianchi type Universe models. In the present discussion we consider a special type of Bianchi Universe, the locally rotationally symmetric (LRS) Bianchi type-I model to denote the anisotropic state of the Universe, given by the metric in the Cartesian coordinates…”