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In order to better understand the relationship between feedback and galacticchemical evolution, we have developed a new model for stellar feedback at gridresolutions of only a few parsecs in global disk simulations, using theadaptive mesh refinement hydrodynamics code Enzo. For the first time in galaxyscale simulations, we simulate detailed stellar feedback from individual starsincluding asymptotic giant branch winds, photoelectric heating, Lyman-Wernerradiation, ionizing radiation tracked through an adaptive ray-tracing radiativetransfer method, and core collapse and Type Ia supernovae. We furthermorefollow the star-by-star chemical yields using tracer fields for 15 metalspecies: C, N, O, Na, Mg, Si, S, Ca, Mn, Fe, Ni, As, Sr, Y, and Ba. We includethe yields ejected in massive stellar winds, but greatly reduce the winds'velocities due to computational constraints. We describe these methods indetail in this work and present the first results from 500~Myr of evolution ofan isolated dwarf galaxy with properties similar to a Local Group, low-massdwarf galaxy. We demonstrate that our physics and feedback model is capable ofproducing a dwarf galaxy whose evolution is consistent with observations inboth the Kennicutt-Schmidt relationship and extended Schmidt relationship.Effective feedback drives outflows with a greater metallicity than the ISM,leading to low metal retention fractions consistent with observations. Finally,we demonstrate that these simulations yield valuable information on thevariation in mixing behavior of individual metal species within the multi-phaseinterstellar medium.

Simulating an Isolated Dwarf Galaxy with Multi-Channel Feedback and Chemical Yields from Individual Stars