We investigate the effects of neutrino-nucleus interactions (the v-process) on the production of iron-peak elements in Population III core-collapse supernovae. The v-process and the following proton and neutron capture reactions produce odd-Z iron-peak elements in the complete and incomplete Si-burning region. This reaction sequence enhances the abundances of Sc, Mn, and Co in the supernova ejecta. Supernova explosion models of 15 and 25 solar mass stars with the v-process reproduce well the average Mn/Fe ratio observed in extremely metal-poor halo stars. In order to reproduce the observed Mn/Fe ratio, the total neutrino energy in the supernovae should be (3-9) × 10~(53) ergs. Stronger neutrino irradiation and other production sites are necessary to reproduce the observed Sc/Fe and Co/Fe ratios, although these ratios increase by the v-process.
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