Most general exact solution for charged compact star model in extended symmetric teleparallel gravity using two step-method

This article investigates the physical properties and stability of an isotropic compact star in F(Q,T) gravity, where T denotes the trace of the energy-momentum tensor and Q represents the nonmetricity scalar. In the present study, the impact of F(Q,T) gravity on the stability and structure of compact stars is investigated, considering a perfect fluid distribution and adopting the functional form F(Q,T)=ξ1Q+ξ2T. The field equations are solved using the two-step method proposed by Gupta and Jasim [Astrophys. Space Sci. 283 (2003) 337], along with the Buchdahl ansatz given by eφ=ϒ(1+ϵr2)ϒ+ϵr2. To investigate the physical properties of the LMC X-4 compact star, a static spherically symmetric metric is employed in the interior region, while a Reissner-Nordstrom exterior metric is adopted for the exterior region. In the interior region of the proposed stellar object, we analyze the behaviour of the spacetime metric functions (eφ and eϑ), energy density (ρ), pressure (P), charge (q), ratio of pressure to density (Ω) and the energy conditions. The equilibrium state of the star is analysed using the Tolman-Oppenheimer-Volkoff (TOV) equation, expressed as FG+FH+F(Q,T)+FQ=0. To assess the stability of the configuration, we examine the adiabatic index (Γ), the causality condition, regularity conditions, the well-behaved condition and the stability against convection criterion.