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Synthesis of 3-D coronal-solar wind energetic particle acceleration modules

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Figure

Figure 1. Magneticthis case, the j/B color coding highlights the field configuration after flux rope insertion and subsequent relaxation
Figure 2. Eruption of the CME: (a) the magneticspeed of the plasma; and (c) the negative divergence of the plasma velocity, which highlights regions of strong compression
Figure 3. Energetic particles are accelerated over a broad latitudinal and longitudinal spread from the CME released followingin Figure 2

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