![]() ![]() These neutrinos will hopefully be detected in the next decade. Two guaranteed-although not yet detected-fluxes are the diffuse flux of neutrinos from past supernovae (marked “background from old supernovae”) and the flux of neutrinos generated in collisions of ultra-energetic protons with the 3 K cosmic microwave background (marked GZK after Greisen, Zatsepin and Kuzmin who first considered such collisions). Solar neutrinos, burst neutrinos from SN-1987A, reactor neutrinos, terrestrial neutrinos from radioactive decay processes in the Earth and neutrinos generated in cosmic ray interactions in the Earth atmosphere (“atmospheric neutrinos”) have been already detected. On the other hand, their extremely low interaction cross section makes their detection extraordinarily difficult.įigure 17.1 shows a compilation of the spectra of dominant natural and artificial neutrino fluxes. Different to gamma rays, neutrinos provide incontrovertible evidence for hadronic acceleration. Since these neutrinos can escape much denser celestial bodies than light, they can trace processes hidden to traditional astronomy. Among them, the detection of the feeble fluxes of astrophysical neutrinos which should accompany the production of high energy cosmic rays is the clear primary goal. Underwater/ice neutrino telescopes are multi-purpose detectors covering astrophysical, particle physics and environmental aspects. ![]()
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