This study investigates the characteristics of anisotropic spherically symmetric stellar structures in the context of modified $ f(R, T) $ gravity. The research uses the MIT bag model equation of state to explain the unique features of compact objects and examines how the fluid distribution in the star model is affected by this. By employing Tolman V metric potentials, the field equations are established, and the values of unknown parameters are identified using experimental data from observed stars. A realistic $ f(R, T) $ model is used to analyze the effects of energy density, anisotropic factor, transverse and radial pressure within the cores of these stars for a specific value of the Bag constant. The stability of the cosmic structure and the physical validity of the model are assessed using equilibrium conditions, energy, and causality parameters. The results show that the physical conditions are satisfied by the model, and the magnitude of the Bag constant aligns with experimental data, demonstrating the model's feasibility. Modified $ f(R, T) $ gravity is a theory that extends Einstein's general relativity by incorporating the trace of the energy-momentum tensor into the gravitational action. This theory has been used to explore the behavior of dark energy and dark matter, as well as to study the properties of compact stars. The study highlights the importance of modified gravity theories in addressing unresolved issues in cosmology and astrophysics. The research also emphasizes the role of the Bag constant in describing the properties of compact stars and the significance of the Tolman V metric potentials in deriving the field equations. The findings suggest that modified $ f(R, T) $ gravity can provide a more accurate description of the universe's structure and evolution, particularly in the context of high-gravity regimes such as those found in compact stars.This study investigates the characteristics of anisotropic spherically symmetric stellar structures in the context of modified $ f(R, T) $ gravity. The research uses the MIT bag model equation of state to explain the unique features of compact objects and examines how the fluid distribution in the star model is affected by this. By employing Tolman V metric potentials, the field equations are established, and the values of unknown parameters are identified using experimental data from observed stars. A realistic $ f(R, T) $ model is used to analyze the effects of energy density, anisotropic factor, transverse and radial pressure within the cores of these stars for a specific value of the Bag constant. The stability of the cosmic structure and the physical validity of the model are assessed using equilibrium conditions, energy, and causality parameters. The results show that the physical conditions are satisfied by the model, and the magnitude of the Bag constant aligns with experimental data, demonstrating the model's feasibility. Modified $ f(R, T) $ gravity is a theory that extends Einstein's general relativity by incorporating the trace of the energy-momentum tensor into the gravitational action. This theory has been used to explore the behavior of dark energy and dark matter, as well as to study the properties of compact stars. The study highlights the importance of modified gravity theories in addressing unresolved issues in cosmology and astrophysics. The research also emphasizes the role of the Bag constant in describing the properties of compact stars and the significance of the Tolman V metric potentials in deriving the field equations. The findings suggest that modified $ f(R, T) $ gravity can provide a more accurate description of the universe's structure and evolution, particularly in the context of high-gravity regimes such as those found in compact stars.