[WC] stars are H–deficient central stars of PN which can mimic the spectra of massive (Min∼50M⊙) Wolf-Rayet stars of the carbon sequence and can be modelled using the same techniques. Our model calculations for the [WC10] CPD–56° 8032 and He 2–113 are based on the iterative technique of Hillier (A&A 231 111 1990) which solves the transfer equation in the co-moving frame subject to statistical and radiative equilibrium, assuming an expanding, spherically-symmetric, homogeneous and time-independent atmosphere. In extended atmospheres the stellar radius (R∗) is defined as the inner boundary of the model atmosphere at τRoss=20, with the stellar temperature (T∗) defined by the usual Stefan-Boltzmann (T∗ = (L∗/4 π σ R2 ∗)1/4) relation. For a given mass loss rate (M), the density and velocity field (v(r) = V∞ (1 - R∗/r)β for the supersonic part) are related via the equation of continuity M = 4 π r2 ρ(r) v(r).