Charged Weyssenhoff Compact-Star Models in Einstein–Cartan–Maxwell Theory

We obtain a new class of exact interior solutions describing static, spherically symmetric charged compact configurations in Einstein–Cartan theory. The matter source is modeled by a charged Weyssenhoff spinning fluid, so that intrinsic spin naturally generates spacetime torsion within the Einstein–Cartan framework. Using the Durgapal–Bannerji transformation together with suitable choices of the gravitational potential and anisotropy profile, the Einstein–Cartan–Maxwell field equations are reduced to a second-order master differential equation. The resulting equation is solved exactly in terms of hypergeometric functions, yielding a new family of charged anisotropic interior solutions. In the neutral and isotropic limit (Formula: see text), the model reduces to the well-known Vaidya–Tikekar spheroidal geometry. The parameter combination Formula: see text governs the departure from this limit, and non-zero values generate a broader family of charged anisotropic Einstein–Cartan–Maxwell configurations. The physical behaviour of the model is analyzed through the metric potentials, matter variables, anisotropy, electric field intensity, causality conditions, energy conditions, and stability criteria. The obtained solutions remain regular throughout the stellar interior and satisfy the standard physical acceptability requirements. The causality and stability conditions are fulfilled, all standard energy conditions are satisfied, and the interior spacetime matches smoothly with the exterior Reissner–Nordström solution through the standard junction conditions. The resulting configuration possesses physically acceptable values of compactness and surface redshift. The analysis shows that the combined effects of electric charge, anisotropy, and spin–torsion significantly influence the equilibrium structure of the configuration. In the present model, spin–torsion modifies the effective density and pressure variables through the Einstein–Cartan corrections, thereby affecting the internal equilibrium behaviour of the stellar matter distribution. The present class of solutions therefore provides a physically viable Einstein–Cartan–Maxwell extension of relativistic spheroidal compact-star models and may be relevant in the description of ultra-dense astrophysical systems where strong gravitational, electromagnetic, and spin effects coexist.