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