We discuss the possible existence of an observational window, in the TeVPeV energy range, for the detection of prompt neutrinos from the decay of charmed particles produced in cosmic ray interactions with the atmosphere. We calculate the event rates for muon and tau neutrinos of heavy quark, mostly charm, origin. We argue that their prompt fluxes are observable in a kilometer-scale neutrino telescope, even though the calculations are subjected to large uncertainties, which we quantify. We raise the possibility that a small component of prompt neutrinos may already be present in the observed samples of current experiments. We also discuss the interplay of the predicted fluxes with those produced by the flavor oscillation of conventional atmospheric neutrinos, and by anticipated cosmic sources. Typeset using REVT E X 1The quest to search for sources of cosmic neutrinos beyond the sun, to search for the particles that constitute the cold dark matter, and to exploit other science opportunities ranging from astronomy to particle physics, led to the commissioning of large volume highenergy neutrino telescopes. While AMANDA and Baikal are taking data [1,2], similar and much larger instruments are contemplated [3][4][5][6]. These detectors collect the Cherenkov radiation emitted by charged secondaries (electrons, muons and taus) produced in neutrino charged current interactions in the ice or water surrounding the optical sensors. In order to filter the background of atmospheric muons created by cosmic-ray interactions, only upwardgoing neutrinos which traverse the Earth are monitored. The first mission of a new neutrino telescope is to calibrate the detector on the known flux of atmospheric neutrinos [7]. Up to about 10 TeV, the main source of atmospheric neutrinos is the decay of pions and kaons in the atmosphere produced in the interactions of cosmic rays with the Earth's atmosphere; we will refer to them as constituting the "conventional" atmospheric neutrino flux. At higher energies, these mesons interact rather than decaying into a neutrino because of the increasing lifetime of the parent mesons. Therefore the semileptonic decay of very-short lived charmed particles becomes the dominant atmospheric source, giving rise to the "prompt" neutrino flux. The energy dependence of prompt neutrinos follows the cosmic ray spectrum whereas the spectrum of conventional neutrinos is steeper by one power in energy because of the competition of decay with interaction of the parent particles. The prompt neutrino flux is independent of zenith angle whereas conventional neutrinos are preferentially produced in the rarified atmosphere at large zenith.In this letter we discuss the possible existence of an observational window for prompt neutrinos in the TeV-PeV energy range. We calculate neutrino induced muon and tau event rates, recognizing that the fluxes are subject to large uncertainties arising from the combination of extreme atmospheric cascade parameters with different charm production models. We will argue that the pro...

Analytical solutions of the three-dimensional di usion equations for the hadronic cascade induced by one single nucleon in the atmosphere are obtained and the behaviour of the lateral component is discussed. We study the hadronic lateral distribution of a high energy cosmic ray family detected at Mt. Chacaltaya.

We describe charged hadronic energy spectra of the cosmic-ray superfamilies named Ursa Maior and P3'-C1-890, detected by the Chacaltaya and Pamir Emulsion Chamber Collaborations, respectively, using analytical solutions for the di6'usion equations. We obtain a very good description of these events incorporating Feynman scaling breaking in the multiparticle production model of our cascading formalism. Centauro exotic events are also investigated. PACS number(s): 13.85. Tp, 96.40.De

We show that a simple scaling model of very forward particle production, consistent with accelerator and air shower data, can describe all features of the very high-energy interactions recorded with emulsion chambers. This is somewhat surprising after numerous claims that the same data implied large scaling violations or new dynamics. Interestingly, we cannot describe some of the Centauro events, suggesting that these events are anomalous independently of their well-advertised unusual features such as the absence of neutral secondaries.