  This talk reviews three inputs important to neutrino-induced nucleosynthesis
in a supernova: 1) "standard" properties of the supernova neutrino flux, 2)
effects of phenomena like neutrino oscillations on that flux, and 3) nuclear
structure issues in estimating cross sections for neutrino-nucleus
interactions. The resulting possibilities for neutrino-induced nucleosynthesis
-- the neutrino-process -- in massive stars are discussed. This includes two
relatively recent extensions of neutrino-process calculations to heavier
nuclei, one focused on understanding the origin of 138La and 180Ta and the
second on the effects following r-process freezeout. From calculations of the
neutrino post-processing of the r-process distribution, limits can be placed on
the neutrino fluence after freezeout and thus on the dynamic timescale for the
expansion of the "hot bubble."
