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Particle dynamics in a non flaring solar active region model

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Figure

Fig. 1. Panels, from L-R, showingofdescribes field lines which cross the intensity maxima of several EUV-emissive coronal loops, which have been overlaid in each panel; “CL”indicates core loops, while “SL” indicates shorter loops
Fig. 2. Illustration of initial particle grid and electromagnetic environment in our study.b)and purple surfaces of positive and negativefield lines (grey lines) and observed magnetogram at the base of the simulations, and isosurfaces of parallel electric fi
Fig. 4. Surveys of electron and proton orbits, for initial position grid seen in Fig.100 ( 2a, subject to electric field reductions of a factor 10 (a)−b)) andc)−d)) from the original electric field (Eorig) determined by the MHD active region simulations
Fig. 5./max(v||)) and magnetic field strength ( B-field line based on the initial position (but almost c)E b) and c); b) shows the change in kinetic energy (KE) and parallel electric field component (whileelectron are displayed in Position A: example of elect
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