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The heliospheric modulation of cosmic ray boron and carbon

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Academic year: 2021

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Figure

Fig. 1. Left panels: Computed differential intensities for galactic boron (B) as a function of kinetic  energy for both polarity cycles, at radial distances of 1, 60, and 90 AU (bottom to top) in the equatorial  plane
Fig. 2. Similar to Figure 1 but for carbon (C).
Fig. 3.  Intensity ratios of solutions for B (top) and C (bottom) with a TS model compared to those  without a TS in the model as a function of kinetic energy at radial distances of 1, 60, and 90 AU (left  panels) and as a function of radial distance at en
Fig. 4. Computed intensity ratios, B/C, with a TS in the model compared to those without a TS as a  function of kinetic energy at Earth for both polarity cycles with  α  = 10° and 75°, respectively
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