  We discuss various neutrino-nucleus interactions in connection with the
supernova r-process nucleosynthesis, which possibly occurs in the
neutrino-driven wind of a young neutron star. These interactions include
absorptions of electron neutrinos and antineutrinos on free nucleons,
electron-neutrino captures on neutron-rich nuclei, and neutral-current
interactions of heavy-flavor neutrinos with alpha particles and neutron-rich
nuclei. We describe how these interactions can affect the r-process
nucleosynthesis and discuss the implications of their effects for the physical
conditions leading to a successful supernova r-process. We conclude that a low
electron fraction and/or a short dynamic time scale may be required to give the
sufficient neutron-to-seed ratio for an r-process in the neutrino-driven wind.
In the case of a short dynamic time scale, the wind has to be contained during
the r-process. Possible mechanisms which can give a low electron fraction or
contain the wind are discussed.
