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Stratification in WR envelopes as seen in HeII lines

Using literature data on lines widths we show that the HeII emission lines originate in different regions of the Wolf-Rayet envelope. It is concluded that because of variations of lines widths within one series of an ion the Ionization Potential vs. FWHM velocity diagrams can not be used for quantitative analysis of WR stars. Another physical quantity such as line optical depth should be used. For simplicity we use n u (principal quantum number of upper level) or EP-excitation energy of the upper level in (u-l) transition. The correlation is strongest with n u , indicating the importance of optical depth effects on the line formation region