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The first generation of metal-free (Pop III) stars are crucial for theproduction of heavy elements in the earliest phase of structure formation.Their mass scale can be derived from the elemental abundance pattern ofextremely metal-poor (EMP) stars, which are assumed to inherit the abundancesof uniformly mixed supernova (SN) ejecta. If the expanding ejecta maintains itsinitial stratified structure, the elemental abundance pattern of EMP starsmight be different from that from uniform ejecta. In this work we performnumerical simulations of the metal enrichment from stratified ejecta for normalcore-collapse SNe (CCSNe) with a progenitor mass $25 \ {\rm M}_{\bigodot}$ andexplosion energies 0.7--10 B ($1 \ {\rm B} = 10^{51}$ erg). We find that SNshells fall back into the central minihalo in all models. In the recollapsingclouds, the abundance ratio ${\rm [M/Fe]}$ for stratified ejecta is differentfrom the one for uniform ejecta only within $\pm 0.4$ dex for any element M. Wealso find that, for the largest explosion energy (10 B), a neighboring halo isalso enriched. Only the outer layers containing Ca or lighter elements reachthe halo, where ${\rm [C/Fe]} = 1.49$. This means that C-enhanced metal-poor(CEMP) stars can form from the CCSN even with an average abundance ratio ${\rm[C/Fe]} = -0.65$.

Does the structure of Pop III supernova ejecta affect the elemental abundance of extremely metal-poor stars?