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Fig. 2
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Cosmic-ray energy spectra at solar minimum (φ = 200 MV c−1; continuous lines) and solar maximum (φ = 1200 MV c Cosmic-ray energy spectra; dashed lines). From top to bottom are reported me energy speciraof protons (p), ttelium (He), carbon (C), oxygen (O), nitrogen (N), and iron (Fe) nuclei.
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