Relativistic isotropic stellar model with Durgapal-V metric in f(R,T) gravity

The main aim of this paper is to obtain a relativistic non-singular model for static, spherically symmetric isotropic celestial compact stars in the [Formula: see text] gravity scenario. In this regard, we have considered the isotropic Durgapal-V metric ansatz [M. Durgapal, J. Phys. A[Formula: see text] Math. Gen. 15 (1982) 2637] to find the solutions of Einstein’s field equations in the framework of [Formula: see text] gravity. The obtained solutions are analyzed graphically for the compact star Cen X-3 with mass [Formula: see text] and radius [Formula: see text][Formula: see text]km [M. L. Rawls, J. A. Orosz, J. E. McClintock, M. A. P. Torres, C. D. Bailyn and M. M. Buxton, Astrophys. J. 730 (2011) 25] and numerically for 10 well-known different compact stars along with Cen X-3 corresponding to the different values of coupling constant [Formula: see text]. The reported solutions are singularity-free at the center of the stars, physically well-behaved, and support the physically stable matter configurations by satisfying all the energy conditions and EoS parameter [Formula: see text] (0, 1), causality condition, adiabatic index [Formula: see text]. We have also discussed hydrostatic equilibrium through the modified TOV equation to ensure the equilibrium position of the solutions representing matter distributions. Considering the several values of [Formula: see text] we have examined the impact of this parameter on the proposed solutions that help to make a fruitful comparison of modified [Formula: see text] gravity to the standard general relativity, and interestingly, we have found that the modified [Formula: see text] gravity supports long-term stable compact objects than the standard Einstein gravity. All the graphical and numerical results ensure that our reported model is under the physically admissible regime that indicates the acceptability of the model.