In this work, we develop a new class of compact stellar models by considering electrically charged anisotropic matter distributions coupled with a quintessence field under the zero gravitational complexity condition. The interior spacetime is obtained as an exact solution of the Einstein-Maxwell field equations with quintessence, where the anisotropy and charge contribute to the physical stability of the configuration. The relevant thermodynamical quantities, including the energy density, radial and tangential pressures, quintessence density, anisotropy factor, and equation of state parameters, are shown to be positive, finite, and monotonically decreasing functions of the radial coordinate. The model is further verified through the analysis of regularity, energy conditions, causality, and stability constraints, as well as the behavior of mass function, compactness, and surface redshift. The surface redshift is found to remain finite and within the admissible astrophysical bounds Formula: see text. As an application, we analyze the physical viability of the present framework for a set of well-known pulsars: PSR J0348+0432 (PSR–I), PSR J0740+6620 (PSR–II), PSR J1614–2230 (PSR–III), PSR J1903+0327 (PSR–IV), Cen X–3 (PSR–V), and SMC X–1. Our results indicate that the charged quintessence anisotropic models constructed under the zero GC condition are consistent with observational data of compact stars, thereby providing a physically acceptable description of realistic pulsar structures.
Khan et al. (Thu,) studied this question.