Testing the Modified Ω-Model on the Hulse–Taylor Binary Pulsar (PSR B1913+16)

The Hulse–Taylor binary pulsar (PSR B1913+16) provides one of the most stringent tests of relativistic gravity. In the modified Ω-model, gravitational interactions emergefrom a dual-frequency spacetime curvature invariant, derived using torus geometry with a poloidal radius defined as r = c/f2, where c is the speed of light and f2 is the torsional frequency. We derive the effective invariant for a two-body system and postulate that the periastron precession per orbit is given by ∆ω = Ω/T, with appropriateeccentricity corrections. Using the well-measured parameters of PSR B1913+16, our analysis yields a predicted periastron precession rate of approximately 4.17◦/year, inexcellent agreement with the observed value of about 4.2◦/year. This result reinforces the robustness of the Ω-model in a strong-field regime.