Abstract This study explores the role of f (R, T) gravity in modeling massive pulsars, with particular attention to potential contributions from dark matter effects. We consider a static, spherically symmetric spacetime and derive the modified Einstein field equations for the specific functional form f (R, T) = R + 2 T f (R, T) = R + 2 ξ T, where ξ denotes the matter-geometry coupling constant. The matter distribution is modeled using a modified Chaplygin equation of state (EoS) to relate the energy density and radial pressure. To observe the physical relevance and viability of the model, two well-known pulsars: PSR~J0348+0432 P S R J 0348 + 0432 and PSR ~J0030+0451 P S R J 0030 + 0451 are used. Our analysis demonstrates that for coupling values ξ = - - 0. 1, - - 0. 2, - - 0. 3, the central densities range from 3. 43 10^15\, g~cm^-3 3. 43 × 10 15 g cm - 3 to 3. 98 10^15\, g~cm^-3 3. 98 × 10 15 g cm - 3, while the surface densities remain near 1. 98 10^15\, g~cm^-3 1. 98 × 10 15 g cm - 3. The central pressure pₑ (0) 3. 5 10^34 \, dyne~cm^-2 p r
Mardan et al. (Wed,) studied this question.