Dust evolution in population III supernova remnants

We present the results of calculations for the evolution of dust within Population III supernova remnants (SNRs), focusing on the dust formed in the unmixed ejecta of Type II SNe. We show that once dust grains inside the He core encounter the reverse shock, they are subject to different fates depending on their initial sizes a(ini). For SNRs expanding into the interstellar medium (ISM) with n(H,0) = 1 cm(-3), grains of a(ini) < 0.05 mu m are trapped in the hot gas and are completely destroyed; grains of a(ini) = 0.05-0.2 mu m are trapped in the dense shell behind the forward shock with the final sizes of 0.001-0.1 mu m; grains of a(ini) > 0.2 mu m are injected into the ISM without significant destruction. The total mass of surviving dust is 0.01 to 0.8 M-circle dot and is higher for the lower ISM gas density. We also investigate the elemental abundances of the second-generation stars that form in the dense shell of Population III SNRs, based on the elemental composition of dust piled up in the shell. The comparison of those results with the observations of hyper-metal poor (HMP) stars indicates that the transport of dust segregated from metal-rich gas within a SNR can be responsible for the abundance patterns of Mg and Si in HMP stars.