On high-energy cosmic photinos

Details On high-energy cosmic photinos On high-energy cosmic photinos

Jul 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986nuphb.272..193b&link_type=abstract

Nuclear Physics B, Volume 272, Issue 1, p. 193-212.

Physics

Nuclear Physics

4

Scientific paper

We discuss the possible astrophysical consequences of ``light'' supersymmetric particles, gluinos and photinos. The high-energy photino production is discussed for the ``standard photino source'', comprising a compact source of high-energy protons surrounded by a dense gas cloud. The main channel of photino production is the subprocess g + g --> g + g followed by a gluino decay g --> γ + q + q. The fluxes of high-energy photinos are calculated for the ``standard source'' and its relevance to the possible astrophysical sources is discussed. High-energy photinos can be detected in the Earth's atmosphere by observation of extensive atmospheric showers (EAS). An especially favorable detection of photinos is the observation of upward developing showers. The cross section of γN-scattering, based on the quark subprocess γ + q --> q is calculated and the rate of the showers produced by the photino flux from the ``standard source'' is estimated.
The photino hypothesis is discussed for Cyg X-3. High-energy photinos (as well as νe neutrinos) can effectively produce EAS with the usual ``nuclear'' muon content through the resonant reactions γ + q --> q and νe + e --> W- --> hadrons. They can also produce muons with Eμ>~1 TeV in deep underground detectors. However, we claim that both of these possibilities can be excluded.

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