This talk will discuss solutions for optically thick, super-Eddington stellar winds, induced by an assumed steady energy addition at a near-surface heating radius of a luminous, massive star. The analysis unifies previous super-Eddington wind models that either: (1) assumed a direct radiative flux-driving without accounting for the advection of radiative enthalpy that can become important in such an optically thick flow; or (2) assumed that such super-Eddington outflows are adiabatic, neglecting the effects of the diffusive radiative flux. By solving the coupled differential equations for radiative diffusion and wind momentum, we obtain general solutions that effectively bridge the behaviors of these limiting models. The results give simple scaling relations for the wind terminal speed to surface escape speed, and show that for all allowed steady solutions, the observed luminosity exceeds the Eddington luminosity. Such super-Eddington wind solutions have potential applicability for modeling phases of eruptive mass loss from massive stars, classical novae, and the remnants of stellar mergers.