  We propose the Wind of Fast Rotating Massive Stars scenario to explain the
origin of the abundance anomalies observed in globular clusters. We compute and
present models of fast rotating stars with initial masses between 20 and 120
Msun for an initial metallicity Z=0.0005 ([Fe/H]=-1.5). We discuss the
nucleosynthesis in the H-burning core of these objects and present the chemical
composition of their ejecta. We consider the impact of uncertainties in the
relevant nuclear reaction rates. Fast rotating stars reach the critical
velocity at the beginning of their evolution and remain near the critical limit
during the rest of the main sequence and part of the He-burning phase. As a
consequence they lose large amounts of material through a mechanical wind which
probably leads to the formation of a slow outflowing disk. The material in this
slow wind is enriched in H-burning products and presents abundance patterns
similar to the chemical anomalies observed in globular cluster stars. In
particular, the C, N, O, Na and Li variations are well reproduced by our model.
However the rate of the 24Mg(p,gamma) has to be increased by a factor 1000
around 50 MK in order to reproduce the whole amplitude of the observed Mg-Al
anticorrelation. We discuss how the long-lived low-mass stars currently
observed in globular clusters could have formed out of the slow wind material
ejected by massive stars.
