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Classical Wolf-Rayet (WR) stars are at a crucial evolutionary stage forconstraining the fates of massive stars. The feedback of these hot,hydrogen-depleted stars dominates their surrounding by tremendous injections ofionizing radiation and kinetic energy. The strength of a WR wind decides theeventual mass of its remnant, likely a massive black hole. However, despitetheir major influence and importance for gravitational wave detectionstatistics, WR winds are particularly poorly understood. In this paper, weintroduce the first set of hydrodynamically consistent stellar atmospheremodels for classical WR stars of both the carbon (C) and nitrogen (N) sequence,i.e. WC and WN stars, as a function of stellar luminosity-to-mass ratio (orEddington Gamma), and metallicity. We demonstrate the inapplicability of theCAK wind theory for classical WR stars and confirm earlier findings that theirwinds are launched at the (hot) iron (Fe) opacity peak. For $\log Z/Z_\odot >-2$, Fe is also the main accelerator throughout the wind. Contrasting previousclaims of a sharp lower mass-loss limit for WR stars, we obtain a smoothtransition to optically thin winds. Furthermore, we find a strong dependence ofthe mass-loss rates on Eddington-$\Gamma$, both at solar and sub-solarmetallicity. Increases in WC carbon and oxygen abundances turn out to slightlyreduce the predicted mass-loss rates. Calculations at subsolar metallicitiesindicate that below the metallicity of the SMC, WR mass-loss rates decreasemuch faster than previously assumed, potentially allowing for high black holemasses even in the local universe.

Driving classical Wolf-Rayet winds: A {\Gamma}- and Z-dependent mass-loss