Abstract
Electromagnetic waves, the traditional carriers of astrophysical information, are unable to distinguish be tween matter and antimatter. Until neutrino astronomy canreally set off, cosmic rays should give the only direct information about any antimatter existing in our astrophy sical environment. After the pioneering work of Aizu and co-workers /1961/ and of Brooke and Wolfendale /1964/ the search continued with negative results, but with improving upper limits /for a survey see Steigman 1976/, until Golden and co-workers /1979/ identified the first cosmic antiprotons /p/ at several GeV in a balloon-borne superconducting-magnet spectrometer. At about the same time, Bogomolov and co-workers /1979/ also reported on p observations at similar energies /2 events/. Finally, Buffington and co-workers /1981 a, b, c/, covering a much lower energy range, where p production by collisions is much less efficient, also found a substantial p flux.
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Kiraly, P. (1982). Antimatter in Cosmic Rays. In: Wolfendale, A.W. (eds) Progress in Cosmology. Astrophysics and Space Science Library, vol 99. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7873-7_7
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