  Fast line-driven stellar winds play an important role in the evolution of
planetary nebulae. We provide global hot star wind models of central stars of
planetary nebulae. The models predict wind structure including the mass-loss
rates, terminal velocities, and emergent fluxes from basic stellar parameters.
We applied our wind code for parameters corresponding to evolutionary stages
between the asymptotic giant branch and white dwarf phases. We study the
influence of metallicity and wind inhomogeneities (clumping) on the wind
properties. Line-driven winds appear very early after the star leaves the
asymptotic giant branch (at the latest for $T_\rm{eff}\approx10\,$kK) and fade
away at the white dwarf cooling track (below $T_\rm{eff}=105\,$kK). Their
mass-loss rate mostly scales with the stellar luminosity and, consequently, the
mass-loss rate only varies slightly during the transition from the red to the
blue part of the Hertzsprung-Russell diagram. There are the following two
exceptions to the monotonic behavior: a bistability jump at around $20\,$kK,
where the mass-loss rate decreases by a factor of a few (during evolution) due
to a change in iron ionization, and an additional maximum at about
$T_\rm{eff}=40-50\,$kK. On the other hand, the terminal velocity increases from
about a few hundreds of $\rm{km}\,\rm{s}^{-1}$ to a few thousands of
$\rm{km}\,\rm{s}^{-1}$ during the transition as a result of stellar radius
decrease. The wind terminal velocity also significantly increases at the
bistability jump. Derived wind parameters reasonably agree with observations.
The effect of clumping is stronger at the hot side of the bistability jump than
at the cool side. Derived fits to wind parameters can be used in evolutionary
models and in studies of planetary nebula formation. A predicted bistability
jump in mass-loss rates can cause the appearance of an additional shell of
planetary nebula.
