  We propose and apply a new classification for the CEMP-no stars, which are
"carbon-enhanced metal-poor" stars with no overabundance of s-elements and with
[Fe/H] generally inferior or equal to -2.5. This classification is based on the
changes in abundances for the elements and isotopes involved in the CNO, Ne-Na,
and Mg-Al nuclear cycles. These abundances change very much owing to successive
back and forth mixing motions between the He- and H-burning regions in massive
stars (the "source stars" responsible for the chemical enrichment of the
CEMP-no stars). The wide variety of the ratios [C/Fe], 12C/13C, [N/Fe], [O/Fe],
[Na/Fe], [Mg/Fe], [Al/Fe], [Sr/Fe], and [Ba/Fe], which are the main
characteristics making the CEMP-no and low s stars so peculiar, is described
well in terms of the proposed nucleosynthetic classification. We note that the
[(C+N+O)/Fe] ratios significantly increase for lower values of [Fe/H]. The
classification of CEMP-no stars and the behavior of [(C+N+O)/Fe] support the
presence, in the first stellar generations of the Galaxy, of fast-rotating
massive stars experiencing strong mixing and mass loss (spinstars). This result
has an impact on the early chemical and spectral evolution of the Galaxy.
