The problem of neutrino-driven winds from a protoneutron star is revisited with particular attention to: 1) the injection region where the mass outflow increases to its steady state value, and 2) the effect of boundary conditions from the shock wave. Our results reproduce one-dimensional hydrodynamic calculations at the 10% level. By constructing the relevant conditions for nucleosynthesis from the properties of matter in the wind, we are able to quantitatively connect the canonical protoneutron star observables such as mass, radius, and neutrino luminosity to the production of nuclei near the r-process peak at A=130.