Anisotropic Quark Stars in Modified $f(R,T)$ Gravity utilizing Tolman V potential

Alternative gravity theory is currently an incredibly significant technique for addressing some enduring experimental difficulties, such as the universe's dark region. They may also be employed in celestial cosmology, producing results that are a stage beyond those found using Einstein's General Relativity. In this study, we examine the characteristics of anisotropic spherically symmetric stellar structures in the context of modified $f(R,T)$ gravity. In order to explain the distinctive characteristics of compact objects, we investigate how the fluid distribution in the star model is affected by the MIT bag model equation of state. By using Tolman V metric potentials, we establish the field equations, and by employing the experimental data of the three observed stars, we identify the values of unknown parameters. By using a realistic $f(R,T)$ model, we investigate the effect of the energy density, anisotropic factor, transversal and radial pressure within the cores of the aforementioned stars for a particular amount of the Bag constant. Further, we examine the stability of the cosmic structure and the physical validity of our suggested model via equilibrium conditions, energy, and causality parameters. To conclude, the physical conditions are fulfilled by our model, and the magnitude of the Bag constant agrees with the experimental data, demonstrating the model's feasibility.