On the reported detection of sub-GeV antiprotons in galactic cosmic rays

Details On the reported detection of sub-GeV antiprotons in galactic cosmic rays On the reported detection of sub-GeV antiprotons in galactic cosmic rays

Feb 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982natur.295..391e&link_type=abstract

Nature, vol. 295, Feb. 4, 1982, p. 391-393. Research supported by the Alfred P. Sloan Foundation

Astronomy and Astrophysics

Astronomy

13

Antiprotons, Galactic Radiation, High Energy Interactions, Interstellar Gas, Proton Flux Density, Secondary Cosmic Rays, Astronomical Models, Black Holes (Astronomy), Optical Thickness, Particle Collisions, Primary Cosmic Rays, Radiation Sources

Scientific paper

Buffington et al. (1981) claimed to have detected an antiproton/proton ratio of 2.2 + or - 0.6 x 10 to the -4th power at energies between 130 and 320 MeV. This result is, however, several orders of magnitude above theoretical predictions (Gaisser and Maurer, 1973; Stephens, 1981; Szabalski et al., 1980) at these energies for antiproton fluxes resulting from collisions of primary cosmic rays with the interstellar gas. Scenarios are discussed, in which the reported sub-GeV antiproton excess might be produced as secondaries in high-energy collisions. Production would have to take place in compact, optically thick sources. It is concluded that the results of Buffington et al. can be explained, but should still be checked by further experiments. It is also shown that the antiproton/positron and antiproton/gamma flux ratios are of greater importance than the antiproton flux itself in setting constraints on models of antiproton origin.

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