  During the first 20 seconds of its life, the enormous neutrino luminosity of
a neutron star drives appreciable mass loss from its surface. This
neutrino-driven wind has been previously identified as a likely site for the
r-process. Qian & Woosley (1996) have derived, both analytically and
numerically, the physical conditions relevant for heavy element synthesis in
the wind. These conditions include the entropy (S), the electron fraction (Ye),
the dynamic time scale, and the mass loss rate. Here we explore the
implications of these conditions for nucleosynthesis. We find that the standard
wind models derived in that paper are inadequate to make the r-process, though
they do produce some rare species above the iron group. We further determine
the general restrictions on the entropy, the electron fraction, and the dynamic
time scale that are required to make the r-process. In particular, we derive
from nuclear reaction network calculations the conditions required to give a
sufficient neutron-to-seed ratio for production of the platinum peak. These
conditions range from Ye = 0.2 and S < 100 per baryon for reasonable dynamic
time scales of 0.001-0.1 s, to Ye = 0.4-0.495 and S > 400 per baryon for a
dynamic time scale of 0.1 s. These conditions are also derived analytically to
illustrate the physics determining the neutron-to-seed ratio.
