A four parameters quark star in quadratic [formula omitted]action

Abstract

In this collaborative work, we model charged compact objects within the framework of f(Q) gravity. We assume a quadratic form for the metricity function cast as f(Q)=Q+aQ2 where a can be thought of as a ‘switch’, regaining the classical general relativity limit when it vanishes. In order to close the system of governing equations, we adopt the Krori–Barua ansatz for the metric functions and the MIT bag model equation of state (EOS) determines the evolution of the electric field. The resulting models are singularity-free and describe physically realizable stellar structures such as neutron stars. We demonstrate that the physical attributes of our models are sensitive to four parameters, namely, the EOS, metricity, and charge parameters together with the bag constant. We observe that an increase in the quadratic contribution culminates in a decrease of the density, radial pressure, electric field, and sound speeds while ωr,ωt, anisotropy, and pt increase. The novelty in our work centers on a possible mechanism of increasing the anisotropy of the stellar interior without resorting to exotic fluids or anisotropisation via gravitational decoupling. The robustness of our models can account for observed mass–radius relations of well-known compact stars such as PSR J1614-2230, PSR J1903+6620, Cen X-3 and LMC X-4 and the secondary component of GW190814 event.