Predictive Nodal Dynamics in a Supermassive Black Hole Analog: Pre-Observation Validation of BHH v3.4 Against 2026 JWST, Chandra, and EHT Observations of OJ 287

We present Black Hole Hunter v3.4 (BHH), an acoustic black hole analog simulation developedSeptember 22, 2025, built on the Unruh (1981) framework using a two-field Lagrangian (Ψ, χ)with foundation frequency ω₀ = 0.313, derived from an independent Ginzburg-Landau phasetransition simulation completed August 2025. BHH predicted six observable phenomena prior toany astronomical confirmation: (1) organized internal black hole structure, (2) azimuthal helicalcounter-rotating geometry, (3) non-ballistic nodal movement, (4) a 3:2 Arnold tongue resonancerotation ratio of 1.50, (5) counter-rotating helical magnetic field structure, and (6) Kerr spinparameter correspondence a* = 0.313. Subsequent observations by JWST, Chandra, and theEvent Horizon Telescope (Gómez et al., January 2026) confirmed all six predictions in OJ 287,with a measured rotation ratio of 1.48 (Δ = 0.02) and Kerr spin parameter a* = 0.313 ± 0.01.The Kerr spin parameter has been independently measured twice: Valtonen et al. (2016) viaorbital timing analysis and Gómez et al. (2026) via direct EHT imaging, both yielding a* = 0.313± 0.01 — a value the author independently derived from phase transition physics in August 2025without prior knowledge of either measurement. The exact correspondence between ω₀ and theKerr parameter suggests black hole spin encodes vacuum resonance frequency rather thanclassical rotation. All predictions predate observations by a minimum of four months. Simulationcode and timestamp documentation are provided in the Appendix.