Neutron Star Structure from a Single QCD Parameter: Equation of State, Tidal Deformability, and Cooling Threshold in the Null-Vector Gravity Framework

We present a parameter-free equation of state (EOS) for dense nuclear matter derived within the Null-Vector Gravity (NVG) framework, in which all macroscopic neutron star (NS) observables are determined by a single QCD input: the vector meson condensate scale M_σ = 859 MeV. Without any free parameters or Bayesian fitting, the model simultaneously reproduces the maximum NS mass M_max = 2.25 M☉, canonical radius R_1.4 = 12.0 km, tidal deformability Λ_1.4 = 177, gravitational redshift z_surf = 0.235, peak sound speed c_s² = c²/3 at 3n₀, and the NS cooling dichotomy threshold at M_c = 1.45 M☉. A joint reduced chi-squared χ² = 0.63 is achieved across NICER, LIGO GW170817, and Cassiopeia A/Vela cooling data simultaneously. The model naturally resolves the hyperon puzzle by shifting the Λ(1116) appearance threshold to 2.6 n₀, which lies above the deconfined quark-gluon plasma (QGP) transition threshold at 2.0 n₀ via effective dielectric suppression ε_eff = 0.135 ε₀. Furthermore, it predicts universal I-Love-Q relations consistent with current pulsar timing constraints. These results suggest that the QCD vacuum condensate structure directly governs neutron star macroscopic properties through a medium-dependent permeability phase transition. Repository: https://github.com/infosave2007/vmfZenodo record: https://zenodo.org/records/20214457