Simulating Metal Mixing of Both Common and Rare Enrichment Sources in a
  Low Mass Dwarf Galaxy
  One-zone models constructed to match observed stellar abundance patterns have
been used extensively to constrain the sites of nucleosynthesis with
sophisticated libraries of stellar evolution and stellar yields. The metal
mixing included in these models is usually highly simplified, although it is
likely to be a significant driver of abundance evolution. In this work we use
high-resolution hydrodynamics simulations to investigate how metals from
individual enrichment events with varying source energies $E_{\rm ej}$ mix
throughout the multi-phase interstellar medium (ISM) of a low-mass ($M_{\rm
gas}=2\times 10^{6}$~M$_{\odot}$), low-metallicity, isolated dwarf galaxy.
These events correspond to the characteristic energies of both common and
exotic astrophysical sites of nucleosynthesis, including: asymptotic giant
branch winds ($E_{\rm ej}\sim$10$^{46}$~erg), neutron star-neutron star mergers
($E_{\rm ej}\sim$10$^{49}$~erg), supernovae ($E_{\rm ej}\sim$10$^{51}$~erg),
and hypernovae ($E_{\rm ej}\sim$10$^{52}$~erg). We find the mixing timescales
for individual enrichment sources in our dwarf galaxy to be long
(100~Myr--1~Gyr), with a clear trend of increasing homogeneity for the more
energetic events. Given these timescales, we conclude that the spatial
distribution and frequency of events are important drivers of abundance
homogeneity on large scales; rare, low $E_{\rm ej}$ events should be
characterized by particularly broad abundance distributions. The source energy
$E_{\rm ej}$ also correlates with the fraction of metals ejected in galactic
winds, ranging anywhere from 60\% at the lowest energy to 95\% for hypernovae.
We conclude by examining how the radial position, local ISM density, and global
star formation rate influence these results.
