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Relativistic modeling demonstrates stable supermassive neutron stars exceeding standard mass limits in modified gravity, indicating potential candidates in the lower mass gap.
This work presents a model of highly massive neutron stars within the f(R, T) gravity framework by investigating the combined effects of anisotropy, electric charge, and matter-geometry coupling on their equilibrium and stability in Karmarkar spacetime. Employing a generalized Chaplygin gas equation of state, the modified Einstein field equations yield the corresponding Tolman-Oppenheimer-Volkoff equation. The resulting Mass-Radius relation predicts the existence of supermassive neutron stars, PSR J0614-3329 and PSR J0437-4715, with masses of 3.23M ⊙ and 3.18M ⊙ and radii of 8.33 km and 8.40 km, respectively, exceeding the general relativistic mass limit while remaining consistent with current astrophysical observations.
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Bhattacharya et al. (2026) studied this question.
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