The Role of Stellar Feedback in the Chemical Evolution of a Low Mass
  Dwarf Galaxy
  We investigate how each aspect of a multi-channel stellar feedback model
drives the chemodynamical evolution of a low-mass, isolated dwarf galaxy using
a suite of high-resolution simulations. Our model follows individual star
particles sampled randomly from an adopted initial mass function, considering
independently feedback from: supernovae; stellar radiation causing
photoelectric heating of dust grains, ionization and associated heating,
Lyman-Werner (LW) dissociation of H$_2$, and radiation pressure; and winds from
massive main sequence (neglecting their energy input) and asymptotic giant
branch (AGB) stars. Radiative transfer is done by ray tracing. We consider the
effects each of these processes have on regulating the star formation rate,
global properties, multi-phase interstellar medium (ISM), and driving of
galactic winds. We follow individual metal species from distinct
nucleosynthetic enrichment channels (AGB winds, massive star stellar winds,
core collapse and Type Ia supernovae) and pay particular attention to how these
feedback processes regulate metal mixing in the ISM, the metal content of
outflows, and the stellar abundance patterns in our galaxy. We find that---for
a low-metallicity, low-mass dwarf galaxy ---stellar radiation, particularly
ionizing radiation and LW radiation, are important sources of stellar feedback
whose effects dominate over photoelectric heating and HI radiation pressure.
However, feedback is coupled non-linearly, and the inclusion or exclusion of
each process produces non-negligible effects. We find strong variations with:
the star formation history; the ejection fractions of metals, mass, and energy;
and the distribution of elements from different nucleosynthetic sources in both
the gas and stars.
