Revisiting Wolf-Rayet Masses Through the Photogravitational Parameter Φ

This study introduces an observation anchored mass diagnostic for Wolf Rayet (WR) stars using the photogravitational parameter Φ ≡ L/(Mg). Calibration on 12 WR+O binaries with dynamical masses yields subtype dependent scaling factors, validated to about 9% RMS accuracy. Applying the method to 30 apparently single WRs (15 Galactic, 15 in the LMC, parameters adjusted to a common τ=20 reference) reveals a consistent 43% median mass discrepancy compared to evolutionary tracks, with uncertainties of 25 to 35% from Monte Carlo propagation. The deficit appears across metallicities and subtypes, including WO stars with T* > 200 kK. These results point to revised mass loss prescriptions, super Eddington envelope inflation, and binary driven formation channels, with implications for black hole masses, supernova energetics, and galactic chemical enrichment. The method provides model independent constraints suited to upcoming large WR spectroscopic surveys.