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Fig. 3


PAMELA energy spectra for galactic CR protons (top) and electrons (bottom) are given by the coloured circles, and are overlaid by modelled spectra (solid lines) of corresponding colour. They are computed for an A < 0 HMF polarity configuration, with respect to the VLIS specified at 122 AU (grey lines). PAMELA measurements were reported by Adriani et al. (2013, 2015).

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