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Calculations of high-energy (40<£ Y <350 MeV) photon-nucleus (A>\2) collisions have been carried out. The results of the initial interaction of the photon with the nucleus are obtained either from Levinger's quasideuteron model or, when energetically possible, from one of the four-pion-nucleon states formed in photon-nucleon interactions. The effect of nucleon-(pion-) nucleus interactions that follow the initial photon interaction is taken into account by using an intranuclear-cascade model. The results of the calculations are compared with a variety of experimental data, and good agreement is obtained.

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The neutron flux per unit energy induced in the earth's atmosphere by solar neutrons has been calculated as a function of atmospheric depth for depths of less than 300 g/cm² (∼30,000 ft). The calculated flux is compared with estimates of the cosmic‐ray neutron flux per unit energy, and it is found that for many flares the solar neutron flux per unit energy is sufficiently above the cosmic‐ray neutron flux per unit energy to produce a measurable effect at both balloon and aircraft altitudes.

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