A study of solar proton spectrums in the range from a few Mev to a few bey reveals that at most times the number spectrums of these particles near the earth may be represented by an exponential rigidity spectrum of the form J = Joe-P/•'o Such a spectral representation also applies to a particles. The rigidity, P, is the momentum per unit charge. Intensity-time characteristics of the solar protons are examined, and it is significant that propagation changes Po and Jo but not the exponential nature of the spectrum. Changes in the intensity and spectrum of the solar protons are investigated at times of magnetic storms. The features of these changes are discussed, and certain relationships between the low-energy plasma producing the magnetic storm and the high-energy solar proton plasma are pointed out. As a result of our observations of expo.nential rigidity spectrums for solar protons and a particles observed at the earth and features of the continuum solar radio emission at the times of flares, a consistent understanding of the acceleration and propagation of the solar protons is obtained if we assume that a very rapid accelerating mechanism exists (about 1 minute or less) and that this mechanism accelerates particles of different ze/m, producing similar rigidity spectrums. These exponential spectrums are then maintained, in general, throughout the propagation of the particles in the interplanetary medium. Biswas, S., C. E. Fichtel, and D. E. Guss, A study of the hydrogen, helium, and heavy nuclei in the November 12, 1960, solar cosmic ray event (to be published in Phys. Rev.), NASA Tech. Rept.

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