Revisiting Wolf-Rayet Masses Through the Photogravitational Parameter Φ

This work introduces a surface-anchored mass diagnostic for Wolf-Rayet (WR) stars using the photogravitational parameter Φ = L/(Mg), which combines bolometric luminosity, mass, and surface gravity into a single observable. We calibrate subtype-dependent scale factors on 12 WR+O binaries with dynamical masses, achieving 9% RMS accuracy via leave-one-out cross-validation. Applied to 10 isolated WR stars with internally consistent atmospheric parameters, the method yields photogravitational masses 42% below evolutionary track predictions (median), with 25-35% uncertainties from Monte Carlo error propagation (N=10⁴). The systematic offset suggests enhanced mass loss near the Eddington limit, envelope inflation, and/or binary interaction histories among apparently single WR stars. The framework provides a falsifiable, observation-based mass scale for ~60 Galactic WR objects lacking dynamical constraints, with direct implications for supernova progenitor masses and gravitational wave source populations.本研究提出了一种针对沃尔夫-拉叶星（Wolf-Rayet, WR）的表面锚定质量诊断方法，该方法采用光引力参数Φ = L/(Mg)，将热光度、质量与表面重力整合为单一可观测量。我们基于12颗拥有动力学质量的WR+O双星系统校准了与子类型相关的标度因子，通过留一交叉验证实现了9%的均方根（RMS）精度。将该方法应用于10颗大气参数内部一致的孤立WR星，所得光引力质量较演化轨道预言值低42%（中位数），其不确定性由蒙特卡洛误差传播（Monte Carlo error propagation）估算，范围为25%~35%（N=10⁴）。这一系统性偏移表明，看似孤立的WR星可能存在爱丁顿极限（Eddington limit）附近的质量损失增强、包层膨胀，或双星相互作用历史。该框架为约60个缺乏动力学约束的银河系WR天体提供了可证伪的、基于观测的质量标尺，其结果对超新星前身星（supernova progenitor）质量以及引力波源种群的研究具有直接参考意义。