Modeling dust evolution in the interstellar medium

The results of modeling dust evolution in the interstellar medium of the Galaxy are presented. We combine a chemical evolution model of the Galaxy with a model for dust evolution in the interstellar medium. To study dust growth in molecular clouds we develop a new model in which dust production is determined by characteristic growth timescales of dust species in molecular clouds. We study carbon, silicates, iron, and SiC dust species, discriminating between dust injected by asymptotic giant branch stars and supernovae, and dust grown in the interstellar medium. The observed abundance ratios of presolar dust grains formed in supernova ejecta and in asymptotic giant branch outflows require that for the ejecta from supernovae the fraction of refractory elements condensed into dust be quite small.