Galaxy outflows without supernovae

Abstract

High surface density, rapidly star-forming galaxies are observed to have ≈ 50 – 100 km s − 1 line of sight velocity dispersions, which are much higher than expected from supernova driving alone, but may arise from large-scale gravitational instabilities. Using three-dimensional simulations of local regions of the interstellar medium, we explore the impact of high velocity dispersions that arise from these disk instabilities. Parametrizing disks by their surface densities and epicyclic frequencies, we conduct a series of simulations that probe a broad range of conditions. Turbulence is driven purely horizontally and on large scales, neglecting any energy input from supernovae. We fi nd that such motions lead to strong global out fl ows in the highly compact disks that were common at high redshifts, but weak or negligible mass loss in the more diffuse disks that are prevalent today. Substantial out fl ows are generated if the one-dimensional horizontal velocity dispersion exceeds ≈ 35 km s − 1 ,as occurs in the dense disks that have star-formation rate ( SFR ) densities above ≈ 0.1 M e yr − 1 kpc − 2 . These out fl ows are triggered by a thermal runaway, arising from the inef fi cient cooling of hot material coupled with successive heating from turbulent driving. Thus, even in the absence of stellar feedback, a critical value of the SFR density for out fl ow generation can arise due to a turbulent heating instability. This suggests that in strongly self-gravitating disks, out fl ows may be enhanced by, but need not caused by, energy input from supernovae.