Cosmography in $f(Q,T)$ gravity with the specific $H(z)$

TL;DR

This paper investigates the cosmological implications of $f(Q,T)$ gravity using a specific $H(z)$ parameterization, analyzing how it models the universe's expansion, energy content, and large-scale structure evolution.

Contribution

It introduces a detailed analysis of $f(Q,T)$ gravity with a specific $H(z)$ form, highlighting its ability to describe cosmic dynamics and evolution.

Findings

Accurately models energy density and pressure evolution.

Provides insights into cosmic acceleration and deceleration phases.

Explores large-scale structure development within the modified gravity framework.

Abstract

The dynamics of perfect fluid as a source in the context of modified gravity, specifically $f(Q,T)$ gravity, are examined within the Friedmann-Lema\^itre-Robertson-Walker (FLRW) cosmological model. This gravity is a generic function of the non-metricity scalar $Q$ and its trace $T$. We investigate the characteristics of the derived cosmological model using a parameterized form of Hubble's parameter, $H(z) = H_0\left[\Omega_{0m}(1+z)^3 + (1-\Omega_{0m})\right]^{\frac{1}{2}}$ (Mahmood et al. Int. J. Geom. Methods Mod. Phys., https://doi.org/10.1142/S0219887824502049). Our examination reveals how physical parameters such as energy density, pressure, and the equation of state parameter, among others, in our model accurately describe the physical behavior of the cosmos. Furthermore, we explore the kinematic parameters in our model, which provide valuable insights into the cosmos's expansion history, including its acceleration, deceleration, and the evolution of its large-scale structure. By exploring these aspects, we gain a deeper understanding of the cosmos's dynamics and evolution within the context of modified gravity.