Charged Compact Stars within the Modified Rastall f(ℚ,𝒯 ) Gravity

This manuscript investigates the viability and stability of charged anisotropic compact star configurations within the framework of modified Rastall [Formula: see text] gravity, where [Formula: see text] and [Formula: see text] denote the non-metricity scalar and the trace of the energy-momentum tensor, respectively. The metric components are generated through the Karmarkar condition, which provides a geometrically consistent embedding relation between the metric potentials. The modified field equations are formulated in terms of an analytical function [Formula: see text], and two representative scenarios are explored. First, a hybrid form of [Formula: see text] combined with a linear phenomenological EoS to determine [Formula: see text]. Second, the same hybrid form of [Formula: see text] is retained, while [Formula: see text] is chosen in logarithmic form. The main objective is to examine how the model parameters influence the regularity, viability, and stability of the resulting exact solution configurations. A representative compact star mass radius scale, motivated by PSR J1614-2230, is used only for boundary matching and parameter calibration. The results show that, within the selected parameter range, the obtained effective configurations satisfy the standard regularity, energy condition, causality, compactness, redshift, and equilibrium requirements expected from phenomenological compact star models.