Construction of Physically Viable Charged Stellar Structures admitting Scalar-Curvature Corrections

In this paper, we investigate charged, anisotropic compact-star configurations in [Formula: see text] gravity, where [Formula: see text] and [Formula: see text] are the Ricci scalar and scalar field, respectively. We adopt the Finch–Skea metric to reconstruct stellar interiors, with Reissner–Nordström-type metric values imposed at the surface rather than obtained from a full exterior integration. The model [Formula: see text], scalar-field ansatz [Formula: see text], and potential [Formula: see text] are implemented numerically using Mathematica. We examine twelve compact stellar candidates: [Formula: see text], [Formula: see text], [Formula: see text], [Formula: see text], [Formula: see text], [Formula: see text], [Formula: see text], [Formula: see text], [Formula: see text], [Formula: see text], [Formula: see text], and [Formula: see text]. The analysis covers metric potentials, energy density, pressure components, pressure-to-density ratios, anisotropy, energy conditions, sound-speed and adiabatic-index diagnostics, the interior mass function, compactness and redshift diagnostics, and the modified Tolman–Oppenheimer–Volkoff equation. The reported profiles satisfy the examined local diagnostic inequalities and force-balance condition over the evaluated stellar interiors. These checks do not establish full coupled perturbative stability or a self-consistent exterior solution. The prescribed masses and radii are inputs to individual reconstructions, not predictions of a common-EoS mass–radius sequence or a maximum supported mass. The results illustrate an interior modeling approach whose scalar-field regularity, full junction conditions, exterior contributions to gravitational mass, and coupled stability require further investigation.