Abstract
This study reformulates f(T) and f(G) gravity for neutron stars using a modified Tolman–Oppenheimer–Volkoff equation. Reconstruction approaches have been developed in the polytropic gas model context assuming that the star’s density is a quadratic, linear, or exponential function of the radius r. Studies have been carried out on the behaviour of modified gravity theories reconstructed through analytical solutions and the assumption of some already valid forms. The evolution of the radial density of the neutron star has been studied in every instance. For f(T) gravity, it is determined that the density of the neutron star increases with radius, which is explainable as a result of accretion surrounding the neutron star. Additionally, as r→∞, the reconstructed models show asymptotic flatness. As a result, it has been hypothesised that the interior mass of the neutron star resembles an ideal fluid, which results in decreased viscosity and lessened internal resistance. This lowers the possibility of collapse for the neutron star.
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