Structural and physical properties of singularity-free dark energy compact star generated by Durgapal–Bannerji potential

This study investigates the structural and physical properties of dark energy compact star within the framework of General Relativity. By incorporating variations in the dark energy parameter ([Formula: see text]) and the dark anisotropy parameter ([Formula: see text]), we analyze their effects on key physical characteristics, including metric potentials, density and pressure distributions, mass–radius relationships, and stability criteria. The results reveal that dark energy influences gravitational binding, total mass and compactness. Stability analysis confirms that the model satisfies causality conditions, remains hydrostatically balanced, and meets the Harrison–Zeldovich–Novikov criterion. Additionally, the modified Tolman–Oppenheimer–Volkoff equation ensures equilibrium under the interplay of gravitational, hydrostatic, and dark energy forces. These findings suggests the viability of dark energy compact stars as stable astrophysical objects, providing insights into their structural behavior and potential observational signatures. We have calculated mass–radius relation and moment of inertia for Her X-1, LMC X-4, PSR J1614-2230 and GW190814. In particular the radius and moment of inertia of LMC X-4 fall in the range [11.81–12.89] km and [1.11[Formula: see text]] [Formula: see text].