Abstract
Neutrinos are considered promising probes for high energy astrophysics. Many indications suggest, indeed, that cosmic objects where acceleration of charged particles takes place, e.g. GRBs and AGNs, are the sources of the detected UHE-CRs. Accelerated hadrons, interacting with ambient gas or radiation, can produce HE neutrinos. Differently from charged particles and gamma rays having \(E_\gamma > TeV\), neutrinos can reach the Earth from far cosmic accelerators, traveling in straight line, therefore carrying direct information on the source. Theoretical models indicate that a detection area of ≃ km2 is required for the measurement of HE cosmic ? fluxes. The underwater/ice Cherenkov technique is widely considered the most promising experimental approach to build high energy neutrino detectors. The first generation of underwater/ice neutrino telescope, BAIKAL and AMANDA, despite their limited size have already set first constraints on TeV neutrino production astrophysical models. The quest for the construction of km2 size detectors have already started: in the South Pole the ICECUBE neutrino telescope is under construction; the ANTARES, NEMO and NESTOR Collaborations are working towards the installation of a neutrino telescope in the Mediterranean Sea.
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Migneco, E., Riccobene, G. (2005). High Energy Neutrino Astronomy and Underwater Detectors. In: Shapiro, M.M., Stanev, T., Wefel, J.P. (eds) Neutrinos and Explosive Events in the Universe. NATO Science Series, vol 209. Springer, Dordrecht. https://doi.org/10.1007/1-4020-3748-1_16
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