  Most numerical simulations of galaxy formation and evolution are unable to
properly resolve the turbulent cascade at or below the resolution scale and
turbulence models are required to capture the motion of eddies on those
unresolved scales. In this study, we investigate the impact of turbulent metal
diffusion models on multiphase outflows originating from dwarf galaxies
($M_{\rm halo} \sim 10^{10} - 10^{11}$ M$_\odot$). We use our state-of-the-art
numerical model for the formation of single stars and non-equilibrium cooling
and hydrogen chemistry. Our simulations are carried out at a mass resolution of
$\sim$1 M$_{\odot}$, where the individual supernova explosions are resolved in
terms of hot-phase generation and momentum input. We find that mass, energy,
and metal loading factors are only weakly affected by the inclusion of a metal
diffusion model. The metal enrichment factor at low altitude above the galactic
disk is higher by around 20 per cent when the metal diffusion model is
included. Specifically, we find more efficient cooling in the cold interstellar
medium, as higher amounts of metals are kept in the cold dense phase. The most
striking effect of the metal diffusion model is that, without metal diffusion,
there is more rapid cooling in the hot phase and a reduced sound speed by a
factor of two. Specifically, we find that the hot phase is more metal enriched
in the case without metal diffusion leading to more rapid (over) cooling of
that phase which is consistent with the higher sound speed we find in the runs
with metal diffusion.
