
TL;DR
This paper presents a model explaining how star-forming galaxies accrete gas from hot coronae via cloud ablation and mixing, accounting for observed HI halos and galaxy evolution, including the quenching of star formation after mergers.
Contribution
It introduces a cloud-corona interaction model that successfully fits HI halo observations across different galaxies and explains galaxy quenching mechanisms post-merger.
Findings
Model fits HI halo data for multiple galaxies.
Parameter values are consistent with hydrodynamical simulations.
Galaxy quenching can result from loss of cool gas discs after mergers.
Abstract
Cosmology requires at least half of the baryons in the Universe to be in the intergalactic medium, much of which is believed to form hot coronae around galaxies. Star-forming galaxies must be accreting from their coronae. HI observations of external galaxies show that they have HI halos associated with star formation. These halos are naturally modelled as ensembles of clouds driven up by supernova bubbles. These models can fit the data successfully only if clouds exchange mass and momentum with the corona. As a cloud orbits, it is ablated and forms a turbulent wake where cold high-metallicity gas mixes with hot coronal gas causing the prompt cooling of the latter. As a consequence the total mass of HI increases. This model has recently been used to model the Leiden-Argentina-Bonn survey of Galactic HI. The values of the model's parameters that are required to model NGC 891, NGC 2403 and…
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