  The reverse shock in the ejecta of core-collapse supernovae is potentially
able to destroy newly formed dust material. In order to determine dust survival
rates, we have performed a set of hydrodynamic simulations using the grid-based
code AstroBEAR in order to model a shock wave interacting with clumpy supernova
ejecta. Dust motions and destruction rates were computed using our newly
developed external, post-processing code Paperboats, which includes gas drag,
grain charging, sputtering and grain-grain collisions. We have determined dust
destruction rates for the oxygen-rich supernova remnant Cassiopeia A as a
function of initial grain sizes and clump gas density. We found that up to 30 %
of the carbon dust mass is able to survive the passage of the reverse shock if
the initial grain size distribution is narrow with radii around ~10 - 50 nm for
high gas densities, or with radii around ~0.5 - 1.5 ${\mu}$m for low and medium
gas densities. Silicate grains with initial radii around 10 - 30 nm show
survival rates of up to 40 % for medium and high density contrasts, while
silicate material with micron sized distributions is mostly destroyed. For both
materials, the surviving dust mass is rearranged into a new size distribution
that can be approximated by two components: a power-law distribution of small
grains and a log-normal distribution of grains having the same size range as
the initial distribution. Our results show that grain-grain collisions and
sputtering are synergistic and that grain-grain collisions can play a crucial
role in determining the surviving dust budget in supernova remnants.
