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The AMS-02 experiment has reported precise measurements of energy spectra ofseveral cosmic-ray species in the range of ~(0.5-2000) GeV/n. An intriguingfinding is the differences in the spectral shape between the different species.Protons exhibit the steepest spectrum of all the species, and helium, carbon,oxygen and iron spectra are found to be harder than that of neon, magnesium andsilicon. These observations are difficult to explain as diffusive shockacceleration, the currently most plausible theory for cosmic particleacceleration at high energies, expects independence of the spectral index frommass and charge of the accelerated particle. Moreover, propagation in theGalaxy has been shown to not being able to compensate for this discrepancy. Inthis work, we present an explanation based on two-component model for theorigin of cosmic rays in the Galaxy -- the first component originating fromregular supernova remnants in the interstellar medium and the second componentfrom Wolf-Rayet supernovae. Using recent results on cosmic-ray injectionenhancement at supernova shocks in the uniform interstellar medium and in thewind environment of Wolf-Rayet stars, we show that the combination of the twocomponents may explain most of the behavior observed by the AMS-02 experiment.

Cosmic rays in the GeV-TeV energy range from two types of supernovae