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

Bayesian analysis of the hardening in AMS-02 nuclei spectra