The role of dust destruction and dust growth in the evolution of the
  interstellar medium
  We use Milky Way-like chemodynamical simulations with a new treatment for
dust destruction and growth to investigate how these two processes affect the
properties of the interstellar medium in galaxies. We focus on the role of two
specific parameters: f_des (a new parameter that determines the fraction of
dust destroyed in a single gas particle surrounding supernova) and C_s (the
probability that a metal atom or ion sticks to the dust grain after colliding,
i.e., the sticking coefficient) in regulating the amount and distribution of
dust, cold gas and metals in galaxies. We find that simulated galaxies with low
f_des and/or high C_s values produce not only more dust, but they also have a
shallower correlation between dust surface density and total gas surface
density, and a steeper correlation between dust-to-gas ratio and metallicity.
Only for values of f_des between 0.01 and 0.02, and of C_s between 0.5 and 1
our simulations produce an average slope of the dust-to-gas ratio versus
metallicity relation consistent with observations. f_des values correspond to a
range of a total fraction of dust destroyed by a single supernova between 0.42
and 0.44. Lastly, we compare predictions of several simulations (with different
star formation recipes, gas fractions, central metallicities, and metallicity
gradients) to the spatially resolved M101 galaxy, and conclude that metallicity
is the primary driver of the spatial distribution of dust, while dust-to-gas
ratio controls the cold gas distribution, as it regulates the
atomic-to-molecular hydrogen conversion rate.
