Compact stars are astronomical objects characterized by their high density and gravitational pull, resulting from the gravitational collapse of massive stellar cores. These extreme conditions lead to a state of matter that defies our everyday understanding, where quantum mechanical effects become significant. The Tolman-Oppenheimer-Volkoff (TOV) equations play a crucial role in describing the equilibrium structure of such compact stars. Formulated within the framework of general relativity, these equations provide insights into the interplay between gravity, pressure, and the properties of matter at such extreme densities. TOV equations offer a theoretical model that enables us to comprehend the balance between the crushing force of gravity and the outward pressure generated by particle interactions within the star's core. As a result, these equations are essential tools for studying the maximum mass a compact star can achieve before collapsing into a black hole, as well as predicting the radius and other properties of these enigmatic celestial objects.
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