Expected Muon Energy Spectra and Zenithal Distributions Deep Underwater

Details Expected Muon Energy Spectra and Zenithal Distributions Deep Underwater Expected Muon Energy Spectra and Zenithal Distributions Deep Underwater

1999-05-19

arxiv.org/abs/hep-ph/9905399v1

Physics

High Energy Physics

High Energy Physics - Phenomenology

4 pages, LaTeX, figures included; to appear in the Proceedings of the 26th ICRC, Salt Lake City, Utah, August 17-25, 1999

Scientific paper

Energy spectra and zenith angle distributions of atmospheric muons are calculated for the depths of operation of large underwater neutrino telescopes. The estimation of the prompt muon contribution is performed with three approaches to charm hadroproduction: recombination quark-parton model, quark-gluon string model, and perturbative QCD based models. Calculations show that the larger are zenith angles and water thickness above the detector, the lower is the energy at which the prompt muon flux becomes equal to conventional one (``crossing energy'') . For instance, for the depth of the Baikal Neutrino Telescope and for zenith angle of 78 degrees the crossing energy is about 300 TeV, whereas it is only 8 TeV for the NESTOR depth. Nevertheless, the muon flux of the crossing energy at NESTOR depth is in order of magnitude lower in comparison with the Baikal depth.

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