is less well-established, we use it here, noting that the $\beta$-law model of Gräfener & Hamann (2005) shows a similar global energy budget as their self-consistent computation for the same parameters. This indicates that the global method may produce meaningful results (as for O stars). In any case, it is our philosophy to accept small errors in the mass-loss determination, as our goal is to explore a large parameter space, comprising a wide range of metallicities and mass-loss rates, and to establish the ${\mbox{$\dot{M}$}}(Z)$ scaling law that may already be retrieved from a differential study.

In the next two sections, we describe our method and assumptions. Our basic Wolf-Rayet wind models are presented in Sect. \[s\_massloss\], followed by a study of their mass-loss properties as a function of metal abundance. We make a distinction between the nitrogen-rich Wolf-Rayet stars (WN), which may still contain some hydrogen, but with helium present in large quantities, and the carbon rich WR stars (WC) that have converted a significant fraction of helium into carbon, thereby representing a later evolutionary phase. We discuss the implications of our findings in Sect. \[s\_impl\], and summarize in Sect. \[s\_concl\]

Method to calculate  with Monte Carlo {#s_method}
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The 