Abstract
Ten to 100 meV protons from the solar flare of March 24, 1966 were observed on the University of California scintillation counter on OGO-I. The short rise and decay times observed in the count rates of the 32 channels of pulse-height analysis show that scattering of the protons by the interplanetary field was much less important in this event than in previously observed proton flares. A diffusion theory in which D = M βr is found to be inadequate to account for the time behavior of the count rates of this event. Small fluctuations of the otherwise smooth decay phase may be due to flare protons reflected from the back of a shock front, which passed the earth on March 23.
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Kahler, S.W., Primbsch, J.H. & Anderson, K.A. Energetic protons from the solar flare of March 24, 1966. Sol Phys 2, 179–191 (1967). https://doi.org/10.1007/BF00155918
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DOI: https://doi.org/10.1007/BF00155918