Modeling Dust in Galaxy Evolution Simulations

Dust grains play a fundamental role in galaxies, influencing both their evolution and observability. As a result, incorporating dust physics into galaxy evolution simulations is essential. This is a challenging task due to the finite resolution of such simulations and the uncertainties on dust grain formation in stellar envelopes and their evolution in the Interstellar Medium (ISM). This report reviews some of the most commonly used techniques for modeling dust in galaxy evolution simulations, with a particular emphasis on developments from the past $\sim$10 years in both hydrodynamic and semi-analytic approaches. Key findings from these simulations are presented, discussed, and compared to the most recent available observations. These include the dust-to-gas vs metallicity relation, the abundance of dust within and outside galaxies, and predictions on the relative importance of various processes affecting dust. The analysis presented here highlights significant achievements as well as the limitations in our current modeling of dust evolution in galaxies.