  A series of fast rotating models at very low metallicity (Z=1e-8) was
computed in order to explain the surface abundances observed at the surface of
CEMP stars, in particular for nitrogen. The main results are the following:
  - Strong mixing occurs during He--burning and leads to important primary
nitrogen production.
  - Important mass loss takes place in the RSG stage for the most massive
models. The 85 solar mass model loses about three quarter of its initial mass,
becomes a WO star and could produce a GRB.
  - The CNO elements of HE1327-2326 could have been produced in massive
rotating stars and ejected by their stellar winds.
