Gravitational Collapse Beyond the Neutron-Star Limit: Can Standard-Model Matter Produce a Finite High-Density Core?

Abstract

We refine the mathematical formulation of the Słowik hypothesis within classical general relativity coupled to Standard-Model thermodynamics. The central question remains unchanged: whether gravitational collapse of a configuration of mass ≈ 2.8 M⊙ beyond the maximum stable neutron-star mass can drive baryonic matter through dense-QCD and electroweak regimes, and whether the resulting stress-energy can support a finite, nonsingular core. We present the Misner–Sharp relativistic hydrodynamic system, the TOV equilibrium sequence, beta-equilibrium conditions, a timescale hierarchy, and an explicit energy-density budget for the electroweak temperature. The Newtonian matching scale R_E ≡ GMm_N/E is retained solely as a heuristic diagnostic. Numerical evaluation shows that a sphere of radius equal to any of the heuristic R_E values, if thermalized at the electroweak crossover temperature T_EW ≃ 159.5 ± 1.5 GeV, would contain a mass of order 10^4–10^6 M⊙, far exceeding the total mass budget. This energy-budget obstruction implies that macroscopic, thermally equilibrated electroweak regions at the heuristic radii are not attainable within a 2.8 M⊙ object. Consequently, within the minimal classical framework, a regular finite core supported solely by Standard-Model stress-energy has not been demonstrated and remains subject to the classical singularity-theorem obstruction. The original hierarchy intuition of the hypothesis is preserved as a physical question whose resolution lies beyond the present minimal model.