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We investigate the nucleosynthesis in the neutrino-driven winds blown offfrom a $3M_\odot$ massive proto-neutron star (mPNS) temporarily formed duringthe collapse of a $100M_\odot$ star. Such mPNSs would be formed in hypernovae.We construct steady and spherically symmetric wind solutions. We set largeneutrino luminosities of $\sim 10^{53}\ {\rm erg\ s^{-1}}$ and average energiesof electron neutrinos and antineutrinos in the ranges of$\epsilon_{\nu_e}=9-16\ {\rm MeV}$ and $\epsilon_{\bar{\nu}_e}=11-18\ {\rmMeV}$ based on a recent numerical relativity simulation. The wind solutionsindicate much shorter temperature-decrease timescale than that of the windsfrom ordinary PNSs and, depending on $\epsilon_\nu$, the winds can be bothneutron-rich and proton-rich. In the neutron-rich wind, the $r$-process occursand the abundance distribution of a fiducial wind model of the mPNS gives anapproximate agreement with the abundance pattern of metal-poor weak $r$ starHD~122563, although the third-peak elements are produced only when the$\bar{\nu}_e$ energy is much larger than the $\nu_e$ energy. In the proton-richwind, the strong $\nu p$-process occurs and $A>100$ nuclides are synthesized.The synthesized nuclei can be neutron-rich in some cases because the largeneutrino luminosity of the mPNS supplies a sufficient amount of neutrons.

Nucleosynthesis in neutrino-driven winds in hypernovae