The physical drivers of gas turbulence in simulated disc galaxies

Abstract

ABSTRACT We use the eagle cosmological simulations to study the evolution of the vertical velocity dispersion of cold gas, σz, in central disc galaxies and its connection to stellar feedback, gravitational instabilities, cosmological gas accretion, and galaxy mergers. To isolate the impact of feedback, we analyse runs that turn off stellar and (or) active galactic nuclei feedback in addition to a run that includes both. The evolution of σz and its dependence on stellar mass and star formation rate in eagle are in good agreement with observations. Galaxies hosted by haloes of similar virial mass, $\rm M_{200}$, have similar σz values even in runs where feedback is absent. The prevalence of local instabilities in discs is uncorrelated with σz at low redshift and becomes only weakly correlated at high redshifts and in galaxies hosted by massive haloes. σz correlates most strongly with the specific gas accretion rate onto the disc as well as with the degree of misalignment between the inflowing gas and the disc’s rotation axis. These correlations are significant across all redshifts and halo masses, with misaligned accretion being the primary driver of high gas turbulence at redshifts z ≲ 1 and for halo masses $\rm M_{200} \lesssim 10^{11.5} {\rm M}_{\odot }$. Galaxy mergers increase σz, but because they are rare in our sample, they play only a minor role in its evolution. Our results suggest that the turbulence of cold gas in eagle discs results from a complex interplay of different physical processes whose relative importance depends on halo mass and redshift.