The Neutron Star: Its Layered 4-D Rotor Structure and Transition into a Black Hole
Abstract
Neutron stars have long been modeled as three-dimensional spheres of degenerate nuclear matter held up by quantum pressure, yet this picture leaves major questions unanswered: how magnetars sustain fields exceeding 10¹¹ T for millennia, why rotational glitches occur in discrete quanta, and why gravitational-wave data imply stronger central compactness than nuclear equations of state predict. In earlier work, subatomic particles were described as four-dimensional (4-D) curvature rotorslocalized standing patterns of torsion whose internal rotation projects as spin, charge, and magnetic moment. Here we extend that geometry to stellar scale. A neutron star is modeled as a two-radius system: a compact torsion core (r_core R_curv) containing phase-locked 4-D rotation, surrounded ≪ by a macroscopic curvature envelope (R_curv ≈ 10-13 km) that defines the observed photosphere. Between these radii lie three previously unrecognized regions-the shear membrane, torsionpressure gradient zone, and torsion halo-each with distinct physical roles. This layered structure reproduces magnetar stability, quantized glitches, and low tidal deformability, while predicting subtle polarization and redshift anomalies. A stability analysis shows that collapse to a black hole occurs when the torsional pressure P_torsion ≈ ρ Ω₄² r_core² / κ falls below the gravitational pressure P_g ≈ G M² / R_curv⁴. The "black-hole boundary" thus marks the loss of 4-D phase coherence, not merely a density threshold. This…
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