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The production and propagation of secondary cosmic-ray antiprotons is discussed. The flux expected on the basis of the usual picture of cosmic-ray propagation, including an energy-dependent confinement time, is calculated. It is also pointed out that kinematical features of the expected secondary-antiproton spectrum provide a possible way to discriminate between secondary antiprotons and a hypothetical primary p̄ component in the cosmic radiation.
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Gaisser et al. (1974) studied this question.
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