0 Assigned ID: 759 ----- Attempting Submission 1 (Fri Apr 11 20:11:29 GMT 2014) ----- Observations indicate that galactic winds are ubiquitous, and must carry substantial fractions of the total metals produced by star formation into the circumgalactic medium and perhaps beyond. UV spectroscopy with HST is now beginning to provide an accounting for these metals in local galaxies, but theoretical models for how metal-bearing winds are launched are primitive at best. The primary limitation of simulations at present is resolution: the process of entrainment and mixing between hot, metal-rich supernova ejecta and cool, metal-poor interstellar medium is simply too small-scale to be resolved in cosmological simulations. We propose to clarify the picture by running very high resolution simulations of isolated dwarf galaxies that resolve supernova bubbles and the adiabatic-radaitive transitions they undergo, thereby avoiding the resolution problem and the numerous ad-hoc tricks simulators have used to get around it. Our simulations will make direct, a priori predictions for the absorption spectra produced by various ions in the circumgalactic media of dwarf galaxies, which can be tested against and used to help interpret the forthcoming COS dwarfs survey. We will make our simulation and analysis code public, along with a library of synthetic spectra. QUASAR ABSORPTION LINES AND IGM Default Medium false false false false true SUPPORTED