Speaker
Description
We present the Hybrid Relativistic-Newtonian Approximation (HRNA), a novel and computationally efficient framework designed to simulate the dynamics of self-gravitating systems orbiting within a fixed, curved background spacetime. The HRNA operates at the intersection of two physical regimes: the global motion follows exact general relativistic geodesics in a black hole metric, while the internal self-gravity interaction is resolved using localized Newtonian dynamics.
We formalize the asymptotic consistency of this framework by executing rigorous validation benchmarks under constant relativistic boosts in Minkowski spacetime. Furthermore, we apply the HRNA framework to simulate the tidal separation of binary star systems interacting with a Schwarzschild supermassive black hole. By comparing our results directly against traditional Post-Newtonian (PN) approximations, we demonstrate that the HRNA naturally captures strong-field relativistic effects without the computational complexity or high-order expansion breakdowns typical of PN methods.
These deep-encounter regimes carry profound astrophysical significance, as they drive tidal disruption events and represent a unified mechanism that simultaneously ejects hypervelocity stars out of the galaxy and captures their partners into tightly bound orbits, forming populations like the S-star cluster surrounding Sagittarius A*.