1995A&A...299..503K

We present a grid of helium-carbon models for Wolf-Rayet (WR) stars of the carbon sequence (WC) with β_ C_=0.2 (carbon mass fraction), thus extending our previously released grid with β_C=0.6 to a different chemical composition. The WR model atmospheres are based on the so-called standard assumptions. The calculations account for non-LTE radiation transfer in spherically expanding atmospheres. Helium and carbon are represented by detailed model atoms, especially concerning the ions CIII and CIV. Using the model grids 25 Galactic WC stars of intermediate subtype (WC5 to WC8) are analyzed. Subsequently we perform fine analyses by calculating several individual models for each of the program stars. Temperatures, radii, mass-loss rates and terminal velocities are determined together with the carbon to helium ratio. The analyzed WC stars are found to form two groups, which can be distinguished by the strength of their emission lines. Stars with weak lines (WC-w) have effective temperatures close to 50kK and their winds are relatively thin, forming the continuous spectrum in regions with small expansion velocities. WC stars with strong lines (WC-s) have higher effective temperatures (60 to 100kK, referring to the core radius) and thick winds. Thus there is a strong analogy to the distribution of the early-type WN stars (WNE-w and WNE-s, respectively). For the WC stars we determine luminosities between 10^4.7 and 10^5.5L_☉ and mass-loss rates from 10^–4.8 to 10^–3.9M☉/yr. The carbon mass fraction varies from 0.2 to 0.6. No correlation is found between the carbon abundance and any of the stellar parameters (e.g. temperature, luminosity) or the spectral subtype. The evolution of WR stars is discussed by comparing the results of our analyses with evolutionary tracks.