  Mass loss through stellar winds plays a dominant role in the evolution of
massive stars. Very massive stars (VMSs, $> 100 M_{\odot}$) display Wolf-Rayet
spectral morphologies (WNh) whilst on the main-sequence. Bestenlehner (2020)
extended the elegant and widely used stellar wind theory by Castor, Abbott &
Klein (1975) from the optically thin (O star) to the optically thick
main-sequence (WNh) wind regime. The new mass-loss description is able to
explain the empirical mass-loss dependence on the Eddington parameter and is
suitable for incorporation into stellar evolution models for massive and very
massive stars. The prescription can be calibrated with the transition mass-loss
rate defined in Vink & Gr\"afener (2012). Based on the stellar sample presented
in Bestenlehner et al. (2014) we derive a mass-loss recipe for the Large
Magellanic Cloud using the new theoretical mass-loss prescription of
Bestenlehner (2020).
