In the context of Energy-Momentum Squared Gravity (EMSG), a modified theory of gravity with nonlinear couplings between matter and geometry, we study the structure, stability, and physical viability of electrically charged polytropic compact stars. A relativistic polytropic equation of state with index (n=1) is used to simulate the star interior, and a systematic investigation of charge effects is made possible by assuming that the electric charge distribution is proportionate to the energy density. We examine the impact of the EMSG coupling parameter and the charge fraction on global stellar properties, including mass-radius relations, compactness, and charge profiles, by numerically solving the modified Tolman-Oppenheimer-Volkoff equations. Based on our findings, the maximum gravitational mass is greatly increased and equilibrium configurations are shifted toward larger radii when electric charge is included. Stable models surpass the observational 2 M ⊙ limit established by the heaviest precisely measured neutron stars while still being physically permissible. The robustness of the equilibrium sequences is confirmed by examining the stability of these configurations using the turning-point criterion applied along sequences of fixed total charge Q , following the approach of Arbañil and Malheiro 1 . Additionally, the radial behavior of the sound speed, which stays subluminal throughout the stellar interior for all parameter choices taken into consideration, is analyzed to confirm causality. All things considered, our results show that charged polytropic stars in EMSG are stable and viable compact objects, underscoring the joint influence of nonlinear matter corrections and electric charge in determining the characteristics of dense astrophysical systems outside of general relativity.
Dayanandan et al. (Wed,) studied this question.
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