\begin{document}$3\,M_{\odot}$\end{document}, with compactness ratios of order \begin{document}$0.34$\end{document}, placing them within the mass range inferred for the secondary component of GW190814, whose nature remains observationally undetermined. The presence of charge reduces the central density at maximum mass by approximately \begin{document}$10\%$\end{document}–\begin{document}$15\%$\end{document} while satisfying causality requirements. Furthermore, comparisons with observational constraints from PSR J1614\begin{document}$-$\end{document}2230, J0348\begin{document}$+$\end{document}0432, J0740\begin{document}$+$\end{document}6620, J0952\begin{document}$-$\end{document}0607, and recent NICER radius measurements indicate that charged EMSG configurations remain consistent with current astrophysical bounds across a wide parameter space. These results demonstrate that moderate electric charge, combined with nonlinear matter-geometry coupling, can support quark stars that are significantly more massive than those predicted by general relativity, underscoring the potential observational relevance of charged compact objects in modified gravity and multimessenger astrophysics."> Energy–momentum–squared gravity: charged quark star solutions with unified interacting matter -
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