Dynamical evolution of stable, regular and charged compact stars in f(R,ϕ) gravity

In this paper, we investigate the behavior of compact stars in [Formula: see text] gravity in the presence of charge and anisotropic matter configuration, where [Formula: see text] and [Formula: see text] represent the Ricci scalar and scalar field potential, respectively. We consider the spherically symmetric spacetime for investigation of stellar objects. For our current analysis, we consider Bardeen spacetime as a exterior geometry to find the unknown constants. A comprehensive analysis is performed for twelve distinct 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]. We analyze the physical properties such as energy density, pressure components, equations of state (EoS) parameters, and the measure of anisotropy. Furthermore, we examine the energy conditions, stability criteria, adiabatic index, mass function, compactness factor, and surface redshift. The graphical analysis of the Tolman–Oppenheimer–Volkoff (TOV) equation confirms that the anisotropic stellar configuration is in hydrostatic equilibrium. Our results demonstrate that the proposed [Formula: see text] model is physically viable, stable, and singularity-free.