Stability of Power Law cosmological model in f(Q) gravity

Abstract

In the present study, we have described the accelerated cosmological models of the universe in f(Q) gravity. In f(Q) gravity, the gravitational field equations are modified by a function of the non-metricity tensor, which characterizes the deviation of the affine connection from the metric compatibility condition. We have considered two different forms of f(Q) gravity as f(Q) = \beta + \alpha \, Q^{(n+1)} and f(Q) = \beta \, Q + \alpha \, Q^{n} to explain the dynamics of the expanding universe. We have discussed the dynamics of the universe through graphical representation by considering the power law ( $a = k t^m$). The free parameters of {\color{red}the} models are fitted {\color{red}with} the latest observational data set of {\color{red} Observational Hubble Data} (OHD), consisting of 57 points, using statistical analysis based on the MCMC method. The best-fitted values for the model’s parameter are estimated as H_0 = 67.3 \pm 1.1, m = 1.0213 \pm 0.0071, and k = 65.4 \pm 1.1. The parameters of the derived model, like energy density, isotropic pressure, EoS parameter, and jerk parameter, are discussed. We have described the energy conditions to explain the viability of the considered models. We have also verified the stability of the derived model through perturbation analysis.