Effects of pi meson decay-absorption phenomena on the high-energy mu meson zenithal variation near sea level

Abstract

An approximate calculation of the ground‐level high‐energy mu meson intensities is presented, with curves showing peculiar maxima in the angular vicinity from about 55° to 75° with respect to the vertical at ground‐level energies from about 60 bev to 160 bev. The effects are explained in terms of well known pi meson decay‐absorption phenomena high in the earth's atmosphere.

Exploring low-energy neutrino physics with the Coherent Neutrino Nucleus Interaction Experiment

“…The steep increase in the rate at low energies is dominated by secondary products of these muons, showering in the detector and in the nearby shielding components. This is demonstrated with a full Geant4 [44] simulation of atmospheric muons hitting the detector, following the energy and angular distribution of [45], which reproduces reasonably well the moun distribution at sea level [46]. The resulting spectrum matches the shape of the overall CONNIE spectrum above 5 keV, as shown in Fig.…”

Development of the very long-range cosmic-ray muon radiographic imaging technique to explore the internal structure of an erupting volcano, Shinmoe-dake, Japan

“…For instance, while the integrated vertical muon flux (0 • from zenith) is 7 × 10 −3 and 5 × 10 −8 cm −2 sr −1 s −1 above 1 GeV and 1 TeV, respectively (Beringer et al, 2012), the horizontal flux (85 • from zenith) is 1 × 10 −4 and 1.6 × 10 −7 cm −2 sr −1 s −1 above 1 GeV and 1 TeV, respectively (Allkofer et al, 1985). For the purpose of interpolating the measured flux, several groups have formulated approximate equations of the muon energy spectrum as a function of energy and zenith angle (e.g., Gaisser, 2002;Matsuno et al, 1984;Smith and Duller, 1959). However, the systematic difference between them ranges from 10 to 100 % (Lesparre et al, 2010).…”

Measurements of muons at sea level

“…The data for the analyses of the azimuthal angular dependence of muons at zenith angles of 20 • and 40 • was accumulated in the observation period from 3 June 1997 to 17 December 1997. The effective observation times are 3258 h [14]; ♦, observed flux in Nottingham [15]; , observed flux by Kiel-Desy [22]; full curves, theoretical spectra by Smith and Duller [25]; broken curves, theoretical spectra by Maeda [26]. in the azimuth measurements.…”