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We study the dust evolution in the supernova remnant Cassiopeia A. We followthe processing of dust grains that formed in the Type II-b supernova bymodelling the sputtering of grains. The dust is located in dense ejecta clumpscrossed by the reverse shock. Further sputtering in the inter-clump medium oncethe clumps are disrupted by the reverse shock is investigated. The dustevolution in the dense ejecta clumps of Type II-P supernovae and their remnantsis also studied. We study oxygen-rich clumps that describe the ejecta oxygencore, and carbon-rich clumps that correspond to the outermost carbon-richejecta zone. We consider the dust components formed in the supernova, severalreverse shock velocities and inter-clump gas temperatures, and derive dustgrain size distributions and masses as a function of time. We find thatnon-thermal sputtering in clumps is important and accounts for reducing thegrain population by ~ 40% to 80% in mass, depending on the clump gasover-density and the grain type and size. A Type II-b supernova forms smallgrains that are sputtered within clumps and in the inter-clump medium. For CasA, silicate grains do not survive thermal sputtering in the inter-clump medium.Our derived masses of currently processed silicate, alumina and carbon grainsin Cas A agree well with values derived from observations. Grains produced byType II-P supernovae better survive the remnant phase. For dense ejecta clumps,dust survival efficiencies range between 42% and 98% in mass. For the SN1987Amodel, the derived surviving dust mass is in the range ~ 0.06-0.13 Msolar. Thistype of dense supernovae may efficiently provide galaxies with dust.Specifically, silicate grains over 0.1 micron and other grains over 0,05 micronsurvive thermal sputtering in the remnant. Therefore, pre-solar grains ofsupernova origin possibly form in the dense ejecta clumps of Type II-Psupernovae.

Molecules and dust in Cassiopeia A: II - Dust sputtering and diagnosis of dust survival in supernova remnants