Fig. 2.28.3. The same as in Fig. 2.28.2, but the magnetic cloud is running ahead of a solar energetic particle event (lower set of curves) and a shock accelerated particle event (upper). According to Kallenrode (2001a).
According to Kallenrode (2001a), the most important results are (1) a pronounced decrease in intensities upstream of the magnetic cloud combined with (2) a pronounced increase in intensities downstream of the cloud, and (3) a strong drop in intensity at the time of passage of the cloud combined with a pronounced positive anisotropy, indicating a net-streaming of particles from the cloud's downstream into its upstream medium (again following the gradient in particle intensities). Again, effects are very similar for a solar injection and a continuous injection from a propagating shock. These results strongly point to a barrier effect of the magnetic cloud for the propagation of energetic particles.
Fig. 2.28.4 shows a comparison between a model run and the Helios observations in the 27 May 1981 event (for a detailed description see Kallenrode, 1997).
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