Abstract
A number of central stars of planetary nebulae (CSPN) show emission lines in their spectra. Among them about 50 have been classified as [Wolf-Rayet] type (Tylenda et al. 1993). In spite of the fact that these stars probably have masses below 1 M⊙ and luminosities < 104 L⊙ their spectra show emission bands very similar to those of much more massive and luminous Population I Wolf-Rayet stars. We present some preliminary results of an extensive investigation of the [WR]-type CSPN based on the spectroscopic survey described in the Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker et al. 1992).
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