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The reverse shock in the ejecta of core-collapse supernovae is potentiallyable to destroy newly formed dust material. In order to determine dust survivalrates, we have performed a set of hydrodynamic simulations using the grid-basedcode AstroBEAR in order to model a shock wave interacting with clumpy supernovaejecta. Dust motions and destruction rates were computed using our newlydeveloped external, post-processing code Paperboats, which includes gas drag,grain charging, sputtering and grain-grain collisions. We have determined dustdestruction rates for the oxygen-rich supernova remnant Cassiopeia A as afunction 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 ifthe initial grain size distribution is narrow with radii around ~10 - 50 nm forhigh gas densities, or with radii around ~0.5 - 1.5 ${\mu}$m for low and mediumgas densities. Silicate grains with initial radii around 10 - 30 nm showsurvival rates of up to 40 % for medium and high density contrasts, whilesilicate material with micron sized distributions is mostly destroyed. For bothmaterials, the surviving dust mass is rearranged into a new size distributionthat can be approximated by two components: a power-law distribution of smallgrains and a log-normal distribution of grains having the same size range asthe initial distribution. Our results show that grain-grain collisions andsputtering are synergistic and that grain-grain collisions can play a crucialrole in determining the surviving dust budget in supernova remnants.

Dust survival rates in clumps passing through the Cas A reverse shock I: results for a range of clump densities