%0 Generic %1 thompson2014subeddington %A Thompson, Todd A. %A Krumholz, Mark R. %D 2014 %K coupling eddington outflow radiative %T Sub-Eddington Star-Forming Regions are Super-Eddington: Momentum Driven Outflows from Supersonic Turbulence %U http://arxiv.org/abs/1411.1769 %X We show that the turbulent gas in the star-forming regions of galaxies is unstable to wind formation via momentum deposition by radiation pressure or other momentum sources like supernova explosions, even if the system is below the average Eddington limit. This conclusion follows from the fact that the critical momentum injection rate per unit mass for unbinding gas from a self-gravitating system is proportional to the gas surface density and that a turbulent medium presents a broad distribution of column densities to the sources. For an average Eddington ratio of <Gamma> = 0.1 and for turbulent Mach numbers greater than 30, we find that ~1% of the gas is ejected per dynamical timescale at velocities larger than the local escape velocity. Because of the lognormal shape of the surface density distribution, the mass loss rate is highly sensitive to the average Eddington ratio, reaching 20-40% of the gas mass per dynamical time for <Gamma> = 1. Implications for the efficiency of star formation in giant molecular clouds are highlighted. Uncertainties are discussed.

@misc{thompson2014subeddington, abstract = {We show that the turbulent gas in the star-forming regions of galaxies is unstable to wind formation via momentum deposition by radiation pressure or other momentum sources like supernova explosions, even if the system is below the average Eddington limit. This conclusion follows from the fact that the critical momentum injection rate per unit mass for unbinding gas from a self-gravitating system is proportional to the gas surface density and that a turbulent medium presents a broad distribution of column densities to the sources. For an average Eddington ratio of <Gamma> = 0.1 and for turbulent Mach numbers greater than 30, we find that ~1% of the gas is ejected per dynamical timescale at velocities larger than the local escape velocity. Because of the lognormal shape of the surface density distribution, the mass loss rate is highly sensitive to the average Eddington ratio, reaching 20-40% of the gas mass per dynamical time for <Gamma> = 1. Implications for the efficiency of star formation in giant molecular clouds are highlighted. Uncertainties are discussed.}, added-at = {2014-11-10T10:15:20.000+0100}, author = {Thompson, Todd A. and Krumholz, Mark R.}, biburl = {https://www.bibsonomy.org/bibtex/2449d5288beb8100158b7b819aff8090c/miki}, description = {[1411.1769] Sub-Eddington Star-Forming Regions are Super-Eddington: Momentum Driven Outflows from Supersonic Turbulence}, interhash = {ad6cefb3f42ee34a00a38bc23b79dadb}, intrahash = {449d5288beb8100158b7b819aff8090c}, keywords = {coupling eddington outflow radiative}, note = {cite arxiv:1411.1769Comment: 9 pages, 5 figures. Submitted. Comments welcome}, timestamp = {2014-11-10T10:15:20.000+0100}, title = {Sub-Eddington Star-Forming Regions are Super-Eddington: Momentum Driven Outflows from Supersonic Turbulence}, url = {http://arxiv.org/abs/1411.1769}, year = 2014 }