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Mass loss is a very important aspect of the life of massive stars. Afterbriefly reviewing its importance, we discuss the impact of the recentlyproposed downward revision of mass loss rates due to clumping (difficulty toform Wolf-Rayet stars and production of critically rotating stars). Although asmall reduction might be allowed, large reduction factors around ten aredisfavoured.  We then discuss the possibility of significant mass loss at very lowmetallicity due to stars reaching break-up velocities and especially due to themetal enrichment of the surface of the star via rotational and convectivemixing. This significant mass loss may help the first very massive stars avoidthe fate of pair-creation supernova, the chemical signature of which is notobserved in extremely metal poor stars. The chemical composition of the verylow metallicity winds is very similar to that of the most metal poor star knownto date, HE1327-2326 and offer an interesting explanation for the origin of themetals in this star.  We also discuss the importance of mass loss in the context of long and softgamma-ray bursts and pair-creation supernovae. Finally, we would like to stressthat mass loss in cooler parts of the HR-diagram (luminous blue variable andyellow and red supergiant stages) are much more uncertain than in the hot part.More work needs to be done in these areas to better constrain the evolution ofthe most massive stars.

The impact of reduced mass loss rates on the evolution of massive stars