General Relativistic Extension of Exponential Radius Evolution Near the Eddington Limit.pdf

This work introduces a surface-based photogravitational framework that unifies radiation and gravity through the parameter Φ = L / (M g), evaluated near the Eddington limit. By relying exclusively on observable surface quantities, the method avoids dependence on interior stellar models, while remaining compatible with stellar evolution codes such as MESA. The framework incorporates opacity effects (including OPAL tables), relativistic corrections, and dynamical processes such as mass loss and stellar winds. The principal result is a corrected exponential radius law, applicable to compact stars near the Eddington boundary. As Φ approaches its critical value in strong-field conditions, the framework reveals deeper geometric connections to horizon thermodynamics, and suggests a potential conceptual bridge to quantum gravity. Thus, it offers both a practical diagnostic for stellar structure and a unifying theoretical framework spanning classical and relativistic regimes.