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Propagation of flare protons in the solar atmosphere

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Abstract

The velocity dispersion for a large number of solar proton events is analyzed in the energy regime of 10–60 MeV. It is found for all events that the time from the flare to particle maximum t m is well represented by a sum of two components. The first component which is energy independent describes the propagation in the solar atmosphere, the second component describes the propagation in the interplanetary medium giving a velocity dispersion v × t m = const. The additional study of time intensity profiles, onset times, and multispaceprobe observations reveals that the propagation in the solar atmosphere consists of three processes: (1) A rapid transport process in the initial (≲ 1 h) phase after the event fills up a “fast propagation region (FPR)”, which may extend up to ≈ 60° from the flare site and which is tentatively identified with a large unipolar magnetic cell as seen on Hα synoptic charts, (2) a large-scale drift process which is energy independent with drift velocities v D in the range 1° ⩽ v D ⩽ 4°h-1, and simultaneously (3) a diffusion process which yields the general broadening of the intensity time profiles for eastern hemisphere events, which is, however, of less importance than previously assumed.

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  1. Institut für Reine und Angewandte Kernphysik, Universität Kiel, W. Germany

    R. Reinhard & G. Wibberenz

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  1. R. Reinhard
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  2. G. Wibberenz
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Reinhard, R., Wibberenz, G. Propagation of flare protons in the solar atmosphere. Sol Phys 36, 473–494 (1974). https://doi.org/10.1007/BF00151216

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  • DOI: https://doi.org/10.1007/BF00151216

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