Expected Muon Energy Spectra and Zenithal Distributions Deep Underwater

Simple item page
dc.creatorMisaki, A.
dc.creatorNaumov, V. A.
dc.creatorSinegovskaya, T. S.
dc.creatorSinegovsky, S. I.
dc.creatorTakahashi, N.
dc.date1999-05-19
dc.date.accessioned2026-07-07T04:07:07Z
dc.date.available2026-07-07T04:07:07Z
dc.descriptionEnergy 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.
dc.description4 pages, LaTeX, figures included; to appear in the Proceedings of the 26th ICRC, Salt Lake City, Utah, August 17-25, 1999
dc.identifierhttps://arxiv.org/abs/hep-ph/9905399
dc.identifierhttp://arxiv.org/abs/hep-ph/9905399
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/49030
dc.subjectHigh Energy Physics - Phenomenology
dc.subjectHigh Energy Physics - Experiment
dc.titleExpected Muon Energy Spectra and Zenithal Distributions Deep Underwater
dc.typetext

Files

Collections

arXiv