Dissipative Gravitation Model: A Non-Linear Spatial Tension Approach to the N-Body Problem

This paper presents the theoretical foundation and computational validation of an alternative approach to the N-body problem and classical orbital dynamics. The Dissipative Gravitation Model (DGM) proposes that the vacuum of spacetime does not constitute an inert stage, but rather a dynamic medium characterized by a variable tension acting as a macroscopic thermodynamic regulator. By introducing a non-linear, velocity-dependent spatial drag, the model mitigates the chaotic instabilities intrinsic to the classical 3-body problem in an idealized vacuum, demonstrating how orbits naturally decay, dissipate energy into the medium (analogous to gravitational wave attenuation), and stabilize towards the system's geometric barycenter. Furthermore, an empirical validation pipeline based on high-precision astrometric data obtained via Very Long Baseline Interferometry (VLBI/IVS) and the Gaia satellite (ESA) is presented, predicting a hydrodynamic refraction asymmetry of approximately 29.14 µas at the solar limb due to the vortical motion of spacetime.