  We discuss general relativistic effects in the steady-state neutrino-driven
``wind'' which may arise from nascent neutron stars. In particular, we
generalize previous analytic estimates of the entropy per baryon $S$, the mass
outflow rate $\dot M$, and the dynamical expansion time scale $\tau_{dyn}$. We
show that $S$ increases and $\tau_{dyn}$ decreases with increasing values of
the mass-to-radius ratio describing the supernova core. Both of these trends
indicate that a more compact core will lead to a higher number of neutrons per
iron peak seed nucleus. Such an enhancement in the neutron-to-seed ratio may be
required for successful r-process nucleosynthesis in neutrino-heated supernova
ejecta.
