  This review discusses the physics of the formation of planetary nebulae
around low mass WR stars, or [WR] stars. It especially focuses on the
differences which can be expected due to the different character of the fast
winds from these [WR] stars. Their fast winds are more massive and are highly H
deficient and metal enriched compared to the winds of normal central stars of
planetary nebulae. This is expected to lead to faster expansion velocities for
the nebulae and a longer momentum-driven phase in the evolution of the
wind-driven bubble, leading to more turbulent nebulae. The observational
evidence also shows that the process which produces the [WR] stars is unlikely
to influence the onset of aspherical mass loss, something which can be used as
a test for models for aspherical mass loss from AGB and post-AGB stars. Finally
it is shown that the nebular characteristics rule out a very late He shell
flash as the origin of most [WR] stars.
