On the dust abundance gradients in late-type galaxies: II. Analytical
  models as evidence for massive interstellar dust growth in SINGS galaxies
  We use simple analytical models of the build up of the dust component and
compare these with radial dust distributions derived from observations of SINGS
galaxies. The observations show that dust gradients are indeed typically
steeper than the corresponding metallicity gradients and our models indicate
very little dust destruction, but significant dust growth in the ISM for most
of these galaxies. Hence, we conclude that there is evidence for significant
non-stellar dust production, and little evidence for dust destruction due to
SNe shock waves. We find that dust is reprocessed rather than destroyed by
shocks from SNe. Finally, we argue that dust abundances derived using standard
methods may be overestimated, since even very 'generous' estimates of the
metallicity results in dust-to-metals ratios above unity in several cases, if
the dust abundances given in the literature are taken at face value.
