  Some indirect observations, as the high fraction of Be stars at low
metallicity, or the necessity for massive stars to be important sources of
primary nitrogen, seem to indicate that very metal poor stars were fast
rotators. As a consequence of this fast rotation, these stars, contrarily to
current wisdom, might lose large amounts of mass during their lifetime. In this
paper, we review various mechanisms triggered by rotation which may induce
strong mass loss at very low metallicity. The most efficient process comes from
surface enrichments in CNO elements which then drive mass loss by stellar
winds. Due to this process, a fast rotating 60 M$_\odot$ with metallicities in
the range of $Z=10^{-8}$ and $10^{-5}$, can lose between 30 and 55% of its
initial mass. This rotationally wind ejected material participates to the
chemical evolution of the interstellar medium, enriching it exclusively in H-
and He-burning products. In particular, metal poor fast rotating stars may play
a key role for explaining the origin of the peculiar abundance pattern observed
at the surface of the extremely metal-poor C-rich stars, for explaining the
chemical inhomogeneities observed in globular clusters, and the presence of
stars in $\omega$ Cen with a very high helium content .
