Dynamical Simulation of Neutron Star Hydrostatic Equilibrium via Axiomatic Physical Homeostasis

This paper presents a novel computational model for simulating Neutron Star dynamics using theAxiomatic Physical Homeostasis (APH) framework. Utilizing the Wave-Particle Transport Simulation(WTS) engine, we model the stellar interior as a continuous fluid governed by a geometric “Stiffness”parameter (β) rather than traditional particle-based degeneracy pressure. We demonstrate that thisphenomenological approach spontaneously reproduces key astrophysical observables: stable hydro-static equilibrium, accretion disk formation, polar jet alignment via geometric torsion, and “glitch”events analogous to starquakes. The simulation provides a real-time, numerically stable laboratoryfor testing the emergent properties of high-density matter under the APH geometric constraints.