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The calculations for the evolution of dust within Population III supernova remnants (SNRs) are presented, based on the models of dust formed in the unmixed ejecta of Type II SNe. We show that once dust grains collide with the reverse shock penetrating into the ejecta, their fates strongly depend on the initial radius aini. For SNRs expanding into the interstellar medium (ISM) with nH,0 = 1 cm−3, grains of aini 0.2 μm are injected into the ISM without being eroded significantly. The total mass of surviving dust is 0.01 to 0.8 M⊙ for nH,0 = 10 to 0.1 cm−3. We also investigate the influence of the piled‐up dust on the elemental abundances of the second‐generation stars formed in the dense shell of Population III SNRs. The comparison of the calculated elemental abundances with those observed in hyper‐metal‐poor (HMP) and ultra‐metal‐poor (U...

Evolution of Dust in Primordial Supernova Remnants and Its Influence on the Elemental Composition of Hyper-Metal-Poor Stars