Thermal instabilities in cooling galactic coronae: fuelling star formation in galactic discs

TL;DR

This study uses an improved SPH simulation to show that cold gas accretion in galaxies occurs via filament fragmentation driven by physical instabilities, not through numerical artifacts, significantly impacting galaxy formation models.

Contribution

The paper demonstrates that improved SPHS simulations eliminate artificial cold clumps, revealing a physical filament fragmentation process that fuels star formation in galactic discs.

Findings

Cold gas condenses along filaments formed at supernova bubble intersections.

Filaments break into bound clumps that form stars, driven by overdensity instabilities.

Classic SPH simulations produce numerical artifacts, not physical cold clumps.

Abstract

We investigate the means by which cold gas can accrete onto Milky Way mass galaxies from a hot corona of gas, using a new smoothed particle hydrodynamics code, 'SPHS'. We find that the 'cold clumps' seen in many classic SPH simulations in the literature are not present in our SPHS simulations. Instead, cold gas condenses from the halo along filaments that form at the intersection of supernovae-driven bubbles from previous phases of star formation. This positive feedback feeds cold gas to the galactic disc directly, fuelling further star formation. The resulting galaxies in the SPH and SPHS simulations differ greatly in their morphology, gas phase diagrams, and stellar content. We show that the classic SPH cold clumps owe to a numerical thermal instability caused by an inability for cold gas to mix in the hot halo. The improved treatment of mixing in SPHS suppresses this instability leading to a dramatically different physical outcome. In our highest resolution SPHS simulation, we find that the cold filaments break up into bound clumps that form stars. The filaments are overdense by a factor of 10-100 compared to the surrounding gas, suggesting that the fragmentation results from a physical non-linear instability driven by the overdensity. This 'fragmenting filament' mode of disc growth has important implications for galaxy formation, in particular the role of star formation in bringing cold gas into disc galaxies.