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