The mode of gas accretion onto star-forming galaxies
F. Marinacci, J. Binney, F. Fraternali, C. Nipoti, L. Ciotti, P., Londrillo

TL;DR
This paper investigates how star-forming galaxies acquire gas through a galactic fountain mechanism involving cloud-corona interactions, supported by hydrodynamical simulations, which may explain galaxy evolution and the transition from blue to red galaxies.
Contribution
It introduces hydrodynamical simulations demonstrating a critical ablation rate that leads to coronal gas condensation, providing a new insight into gas accretion processes in galaxies.
Findings
Hydrodynamical simulations confirm a critical ablation rate for gas condensation.
Trails of HI from clouds are detectable in the Galaxy but not in external galaxies.
The mechanism explains galaxy color evolution and the decline of cold infall over cosmic time.
Abstract
It is argued that galaxies like ours sustain their star formation by transferring gas from an extensive corona to the star-forming disc. The transfer is effected by the galactic fountain -- cool clouds that are shot up from the plane to kiloparsec heights above the plane. The Kelvin-Helmholtz instability strips gas from these clouds. If the pressure and the the metallicity of the corona are high enough, the stripped gas causes a similar mass of coronal gas to condense in the cloud's wake. Hydrodynamical simulations of cloud-corona interaction are presented. These confirm the existence of a critical ablation rate above which the corona is condensed, and imply that for the likely parameters of the Galactic corona this rate lies near the actual ablation rate of clouds. In external galaxies trails of HI behind individual clouds will not be detectable, although the integrated emission from…
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