Summary: The main aim of this paper is to obtain analytic relativistic anisotropic spherical solutions in \(f(R,T)\) scenario. To do so we use modified Durgapal-Fuloria metric potential and the pressure anisotropy condition is imposed in order to obtain the effective anisotropic factor \(\widetilde{\Delta}\). Besides, a notable and viable election on \(f(R,T)\) gravity formulation is taken. The choice of \(f(R,T)\) function modifies the matter sector only, including new ingredients to the physical parameters that characterize the model such as density, pressure, subliminal speeds of sound, surface redshift etc. We analyze all the physical and mathematical general requirements of the configuration taking \(M=1.04 M_\odot\) and varying \(\chi\) from \(- 0.1\) to 0.1. It is shown by the graphical procedure that \(\chi<0\) yields a more compact object in comparison when \(\chi \geq 0\) (where \(\chi=0.0\) corresponds to general relativity) and increases the value of the surface redshift. However, negative values of \(\chi\) introduce in the system an attractive anisotropic force (inward) and the configuration is completely unstable (corroborated employing Abreu’s criterion). Furthermore, the model in Einstein gravity theory presents cracking while for \(\chi>0\) the system is fully stable. The relationship between effective radial pressure \(\widetilde{p}_r\) and effective density \(\widetilde{\rho}\) is discussed and obtained. This is achieved by establishing the corresponding equation of state.