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

Revision III develops a refined mathematical formulation of the Słowik hypothesis concerning gravitational collapse beyond the neutron-star stability limit. The study examines whether Standard-Model matter in a collapsing ≈2.8-solar-mass configuration can access dense-QCD and electroweak regimes and whether such physics can support a finite high-density core. The analysis is formulated within classical general relativity and Standard-Model thermodynamics using the TOV and Misner–Sharp frameworks, composition and beta-equilibrium conditions, causal dense-matter equations of state, characteristic timescale comparisons, curvature regularity conditions, and an explicit electroweak energy-density budget. The resulting calculation shows that the heuristic gravitational energy-matching radii cannot represent macroscopic thermally equilibrated electroweak regions within the available stellar-mass budget. No nonsingular finite core or discrete four-layer structure is derived within the minimal framework. The work therefore preserves the original hierarchy hypothesis as a well-defined physical question while clearly identifying the limits imposed by classical GR and Standard-Model matter.