Chemical evolution of galaxies: emerging dust and the different gas
  phases in a new multiphase code
  Dust plays an important role in the evolution of a galaxy, since it is one of
the main ingredients for efficient star formation. Dust grains are also a
sink/source of metals when they are created/destroyed, and, therefore, a
self-consistent treatment is key in order to correctly model chemical
evolution. In this work, we discuss the implementation of dust physics into our
current multiphase model, which also follows the evolution of atomic, ionised
and molecular gas. Our goal is to model the conversion rates among the
different phases of the interstellar medium, including the creation, growth and
destruction of dust, based on physical principles rather than phenomenological
recipes inasmuch as possible. We first present the updated set of differential
equations and then discuss the results. We calibrate our model against
observations of the Milky Way Galaxy and compare its predictions with extant
data. Our results are broadly consistent with the observed data for
intermediate and high metallicities, but the models tend to produce more dust
than observed in the low metallicity regime.
