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Although galactic winds play a critical role in regulating galaxy formation,hydrodynamic cosmological simulations do not resolve the scales that govern theinteraction between winds and the ambient circumgalactic medium (CGM). Weimplement the Physically Evolved Wind (PhEW) model of Huang et al. (2020) inthe GIZMO hydrodynamics code and perform test cosmological simulations withdifferent choices of model parameters and numerical resolution. PhEW adopts anexplicit subgrid model that treats each wind particle as a collection of cloudsthat exchange mass, metals, and momentum with their surroundings and evaporateby conduction and hydrodynamic instabilities as calibrated on much higherresolution cloud scale simulations. In contrast to a conventional windalgorithm, we find that PhEW results are robust to numerical resolution andimplementation details because the small scale interactions are defined by themodel itself. Compared to conventional wind simulations with the sameresolution, our PhEW simulations produce similar galaxy stellar mass functionsat $z\geq 1$ but are in better agreement with low-redshift observations at $M_*< 10^{11}M_\odot$ because PhEW particles shed mass to the CGM before escapinglow mass halos. PhEW radically alters the CGM metal distribution because PhEWparticles disperse metals to the ambient medium as their clouds dissipate,producing a CGM metallicity distribution that is skewed but unimodal and issimilar between cold and hot gas. While the temperature distributions andradial profiles of gaseous halos are similar in simulations with PhEW andconventional winds, these changes in metal distribution will affect theirpredicted UV/X-ray properties in absorption and emission.

A New Model For Including Galactic Winds in Simulations of Galaxy Formation II: Implementation of PhEW in Cosmological Simulations