  The most significant feature in the cosmic-ray (CR) nuclei spectra is the
spectral hardening at a few hundred GV. It is important to know whether the
hardening of different nuclei species is the same or not for constructing CR
sources and propagation models. In this work, we collect the recently released
AMS-02 CR nuclei spectra of primary species (proton, helium, carbon, oxygen,
neon, magnesium, silicon, and iron), secondary species (lithium, beryllium,
boron, and fluorine), and hybrid species (nitrogen, sodium, and aluminum) and
study the break positions and the spectral index differences (less and greater
than the break rigidity) of the spectral hardening quantitatively. The results
show us that the CR nuclei spectral hardening at a few hundred GV has hybrid
origins. In detail, the dominating factors of the spectral hardening for
primary and secondary CR nuclei species are different: the former comes from
the superposition of different kinds of CR sources, while the latter comes from
the propagation process. Both of these factors influence all kinds of CR nuclei
spectra, just with different weights.
