models of Hillier & Miller (1998) and Gräfener et al. (2002), as well as characteristic abundances, known from spectral synthesis modelling, and evolutionary models. We then vary the metal abundance $Z$, such that we may study the effects of a different host galaxy environment on .

In reality, both stellar structure and evolution are expected to be $Z$ dependent as well, however we do not take this into account at this stage (but see Sect. \[s\_impl\]). The crucial point here is that if  Fe dominates the mass loss of WR stars, mass loss is anticipated to be $Z$-dependent, and the precise chemical enrichment will be less relevant. However, if it turns out that lighter elements, such as the intermediate mass element carbon set the mass loss for WR stars, mass loss is not expected to be dependent on the chemical environment after all.

Although we do not attempt to reproduce a most realistic WR wind model [*per se*]{}, we do aim to construct a representative model. This is no trivial task for the optically thick winds of WR stars. In particular, the effective temperatures of WR stars are not well defined, since the radius is strongly wavelength dependent (e.g. Schmutz 