  Recent studies of massive O-type stars present clear evidences of
inhomogeneous and clumped winds. O-type (H-rich) central stars of planetary
nebulae (CSPNs) are in some ways the low mass-low luminosity analogous of those
massive stars. In this contribution, we present preliminary results of our
on-going multi-wavelength (FUV, UV and optical) study of the winds of Galactic
CSPNs. Particular emphasis will be given to the clumping factors derived by
means of optical lines (Halpha and HeII4686) and "classic" FUV (and UV) lines.
