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 Mₘax = 2. 25 M☉, canonical radius R₁. 4 = 12. 0 km, tidal deformability Λ₁. 4 = 177, gravitational redshift zₛurf = 0. 235, peak sound speed cₛ² = c²/3 at 3n₀, and the NS cooling dichotomy threshold at Mc = 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 εₑff = 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