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This talk reviews three inputs important to neutrino-induced nucleosynthesisin a supernova: 1) "standard" properties of the supernova neutrino flux, 2)effects of phenomena like neutrino oscillations on that flux, and 3) nuclearstructure issues in estimating cross sections for neutrino-nucleusinteractions. The resulting possibilities for neutrino-induced nucleosynthesis-- the neutrino-process -- in massive stars are discussed. This includes tworelatively recent extensions of neutrino-process calculations to heaviernuclei, one focused on understanding the origin of 138La and 180Ta and thesecond on the effects following r-process freezeout. From calculations of theneutrino post-processing of the r-process distribution, limits can be placed onthe neutrino fluence after freezeout and thus on the dynamic timescale for theexpansion of the "hot bubble."Comment: 17 pages, 5 figures, talked presented at "The r-process: The  Astrophysical Origin of the Heavy Elements...

SUPERNOVA NEUTRINO-NUCLEUS PHYSICS AND THE R-PROCESS