  Based on the precise nuclei data released by AMS-02, we study the spectra
hardening of both the primary (proton, helium, carbon, oxygen, and the primary
component of nitrogen) and the secondary (anti-proton, lithium, beryllium,
boron and the secondary component of nitrogen) cosmic ray (CR) nuclei. With the
diffusion-reacceleration model, we consider two schemes to reproduce the
hardening in the spectra: (i) A high-rigidity break in primary source
injection; (ii) A high-rigidity break in diffusion coefficient. The global
fitting results show that both schemes could reproduce the spectra hardening in
current status. More precise multi-TV data (especially the data of secondary CR
species) is needed if one wants to distinguish these two schemes. In our global
fitting, each of the nuclei species is allocated an independent solar
modulation potential and a re-scale factor (which accounts for the isotopic
abundance for primary nuclei species and uncertainties of production cross
section or inhomogeneity of CR sources and propagation for secondary nuclei
species). The fitting values of these two parameter classes show us some hints
on some new directions in CR physics. All the fitted re-scale factors of
primary nuclei species have values that systematically smaller than 1.0, while
that of secondary nuclei species are systematically larger than 1.0. Moreover,
both the re-scale factor and solar modulation potential of beryllium have
values which are obviously different from other species. This might indicate
that beryllium has the specificity not only on its propagation in the
heliosphere, but also on its production cross section. All these new results
should be seriously studied in the future.
