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We investigate the evolution of dust that formed at Population III supernova(SN) explosions and its processing through the collisions with the reverseshocks resulting from the interaction of the SN ejecta with the ambient medium.In particular, we investigate the transport of the shocked dust within the SNremnant (SNR), and its effect on the chemical composition, the sizedistribution, and the total mass of dust surviving in SNR. We find that theevolution of the reverse shock, and hence its effect on the processing of thedust depends on the thickness of the envelope retained by the progenitor star.Furthermore, the transport and survival of the dust grains depend on theirinitial radius, a_{ini}, and composition: For Type II SNRs expanding into theinterstellar medium (ISM) with a density of n_{H,0}=1 cm^{-3}, small grainswith a_{ini} < ~ 0.05 micron are completely destroyed by sputtering in thepostshock flow, while grains with a_{ini}= 0.05--0.2 micron are trapped intothe dense shell behind the forward shock. Very large grains of a_{ini} > ~ 0.2micron are ejected into the ISM without decreasing their sizes significantly.We find that the total mass fraction of dust that is destroyed by the reverseshock ranges from 0.2 to 1.0, depending on the energy of the explosion and thedensity of the ambient ISM. The results of our calculations have significantimpact on the abundance pattern of subsequent generation of stars that form inthe dense shell of primordial SNRs.

Evolution of Dust in Primordial Supernova Remnants: Can Dust Grains Formed in the Ejecta Survive and be Injected into the Early Interstellar Medium?