  The material used to form the CEMP-no stars presents signatures of material
processed by the CNO cycle and by He-burning from a previous stellar generation
called the source stars. In order to reproduce the relative abundance ratios
like for instance C/N or $^{12}$C/$^{13}$C, some mixing between the two burning
regions must have occured in the source stars and only the outer layers of the
stars, with modest amount coming from the CO core, must have been expelled
either through stellar winds or at the time of the (faint) supernova event.
With new models at low metallicity including rotational mixing, we shall
discuss how the variety of abundances observed for CEMP-no stars can be
reproduced.
