  Neutrino-driven winds are thought to accompany the Kelvin-Helmholtz cooling
phase of nascent protoneutron stars in the first seconds after a core-collapse
supernova. These outflows are a likely candidate as the astrophysical site for
rapid neutron-capture nucleosynthesis (the r-process). In this chapter we
review the physics of protoneutron star winds and assess their potential as a
site for the production of the heavy r-process nuclides. We show that spherical
transonic protoneutron star winds do not produce robust $r$-process
nucleosynthesis for `canonical' neutron stars with gravitational masses of 1.4
M_sun and coordinate radii of 10 km. We further speculate on and review some
aspects of neutrino-driven winds from protoneutron stars with strong magnetic
fields.
