Density dependent B- parameter model of relativistic strange stars in the framework of f(R, T) gravity

We investigate a spherically symmetric, isotropic model of strange stars in the context of modified gravity, considering the functional form f ( R , T ) = R + 2 β T , where R is the Ricci scalar, T the trace of the energy-momentum tensor, and β a coupling constant. To obtain the gravitational field equations, a Tolman-IV type potential is employed for the metric component g rr . The stellar matter distribution is described by the MIT bag model equation of state, p = 1 3 ( ρ − 4 B ) , with the bag constant B treated as density-dependent. The energy per baryon E B is evaluated as a function of the energy density ρ within the star. The physical features of compact star candidates such as 4U 1820-30 and LMC X-4 are examined under this framework. The stellar surface is determined from the vanishing pressure condition, while solutions of the Tolman-Oppenheimer-Volkoff equation predict a maximum mass of 3.6 M ⊙ for β = 2.55 , consistent with causality. For the secondary object in G W 230529 − 181500 , with a mass of 3.6 M ⊙ , the model predicts a radius of 12.96 km. Stability and energy condition analyses confirm the model’s applicability to the high-mass regime of strange stars.