Signatures of non-metricity on dynamical analysis of isotropic cosmological models

The characteristics of compact stars are examined in this study utilizing the Kohler-Chao-Tikekar and Tolman IV spacetime models. This study is framed within the f ( Q ) gravity, a geometric theory of gravity where spacetime curvature is describe by the non-metricity, Q . The governing equations for the star’s interior, whose fluid composition is modeled by the perfect matter, are derived initially for a quadratic gravity model, which is predicated on a static, spherically symmetric spacetime. Considering both spacetimes separately results in two different new solutions. We apply boundary conditions at the star’s surface, necessitating continuity with the known Schwarzschild exterior line element, in order to identify the unknowns in our solutions. A thorough set of physical acceptance standards is then discussed in relation to the developed models to guarantee that the stellar models accurately depict compact objects. Using the well-constrained compact stars, such as LMC X-4 and Her X-1, as benchmark candidates, we perform a graphical analysis to verify the parameter space of our models in order to ground our theory in observation. Our findings show that, within a certain range of parameters, both stellar solutions are physically feasible. This work ultimately improves our knowledge of compact star interiors within symmetric teleparallel gravity by offering a solid theoretical framework and significant avenues for further research in this area.