Shaping planetary nebulae: is it different for [WR] stars?

This review discusses the physics of the formation of planetary nebulae aro und low mass WR stars, or [WR] stars. It especially focuses on the differen ces 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 d eficient and metal enriched compared to the winds of normal central stars o f planetary nebulae. This is expected to lead to faster expansion velocitie s for the nebulae and a longer momentum-driven phase in the evolution of th e wind-driven bubble, leading to more turbulent nebulae. The observational evidence also shows that the process which produces the [WR] stars is unlik ely 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 st ars. Finally it is shown that the nebular characteristics rule out a very l ate He shell flash as the origin of most [WR] stars.