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We show that the turbulent gas in the star-forming regions of galaxies isunstable to wind formation via momentum deposition by radiation pressure orother momentum sources like supernova explosions, even if the system is belowthe average Eddington limit. This conclusion follows from the fact that thecritical momentum injection rate per unit mass for unbinding gas from aself-gravitating system is proportional to the gas surface density and that aturbulent medium presents a broad distribution of column densities to thesources. For an average Eddington ratio of <Gamma>~0.1 and for turbulent Machnumbers >30, we find that ~1% of the gas is ejected per dynamical timescale atvelocities larger than the local escape velocity. Because of the lognormalshape of the surface density distribution, the mass loss rate is highlysensitive to the average Eddington ratio, reaching 20-40% of the gas mass perdynamical time for <Gamma>=1. Using this model we find a large scatter in themass-loading factor for star-forming galaxies, ranging from 0.001-10, but withsignificant uncertainties. Implications for the efficiency of star formation ingiant molecular clouds are highlighted. For radiation pressure feedback alone,we find an increasing star formation efficiency as a function of initial gassurface density. Uncertainties are discussed.

Sub-Eddington Star-Forming Regions are Super-Eddington: Momentum Driven Outflows from Supersonic Turbulence