Energy distribution of parent nucleons for muons observed at sea level and underground
TL;DR: In this article, the energy distributions of primary cosmic-ray nucleons responsible for muons detected at sea level and underground have been calculated using a phenomenological model using the Feynman scaling hypothesis of nucleon-nucleon interactions.
Abstract: The energy distributions of primary cosmic-ray nucleons responsible for muons detected at sea level and underground have been calculated using a phenomenological model. The Feynman scaling hypothesis of nucleon-nucleon interactions has been employed using cross sections determined from high-energy scattering experiments.
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TL;DR: In this paper, the similarity between the general remote sensing integral equation and Dorman's integral equation relating secondary to primary muon variation spectra has been pointed out and exploited, and based on relationships among kernels of the integral equation, optimization of location and orientation of measuring stations become possible.
Abstract: The similarity between the general remote sensing integral equation and Dorman's integral equation relating secondary to primary muon variation spectra has been pointed out and exploited. Primary muon variation spectra and parameters of interplanetary field inhomogeneities are remotely sensed by a nonlinear inversion technique, using two different coupling functions. Results are compared to those obtained by the spectrographic technique and interpreted in terms of interplanetary field fluctuations. Based on relationships among kernels of the integral equation, optimization of location and orientation of measuring stations become possible.
4 citations
01 Apr 2015-Nuclear Instruments & Methods in Physics Research Section A-accelerators Spectrometers Detectors and Associated Equipment
TL;DR: In this article, the angular and energy distributions of the primary cosmic rays that are responsible for the muons reaching the sea level have been estimated using the Geant4 simulation package.
Abstract: The angular and energy distributions of the primary cosmic rays that are responsible for the muons reaching the sea level have been estimated using the Geant4 simulation package. The models used in the simulations were tested by comparing the simulation results for the differential muon flux with the BESS measurements performed in Lynn Lake, Canada. Then, direct relationship between the propagation directions of the muons and those of the responsible primary particles has been investigated. The median energies for the parent primaries of vertical muons reaching the sea level with the threshold energies ( E μ ) in the range 0.5–300 GeV were obtained. Simulation results for the median primary energies, 15.5 E μ and 11.2 E μ for E μ = 14 GeV and E μ = 100 GeV , have been found to be in good agreement with the literature. Furthermore, median primary energies for the low energy muons with large zenith angle have been seen to be relatively higher than the ones for the muons with narrower angles.
2 citations
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TL;DR: In this article, the authors measured the energy spectra of cosmic-ray protons and He nuclei by an ionization spectrometer flown at balloon altitudes, with an energy range extended from 50 to g 1000 GeV.
Abstract: Differential energy spectra of cosmic-ray protons and He nuclei have been measured for the first time by an ionization spectrometer flown at balloon altitudes. The energy range extended from 50 to g 1000 GeV. The observed differential intensities can be represented with power-law spectra with a slope of -2.75 \ifmmode\pm\else\textpm\fi{} 0.03 for protons and of -2.77 \ifmmode\pm\else\textpm\fi{} 0.05 for He nuclei. The proton-to-He ratio is 26 \ifmmode\pm\else\textpm\fi{} 3 at 40 GeV/nucleon and is constant within errors up to 400 GeV/nucleon.
197 citations
TL;DR: The absolute vertical muon intensity in the range 0.2 -1000 GeV/c has been determined from four different measurements as mentioned in this paper, which is 10 - 25% higher than previous spectra which have usually been normalized to the intensity at 1 GeV /c given by Rossi in 1948.
171 citations
TL;DR: In this paper, les abondances relatives des elements de charge 4 ≤ Z ≤ 28 and le spectre d'energie absolu de ces elements sont determined.
Abstract: Une analyse de la composition elementaire du rayonnement cosmique est realisee a partir des donnees du satellite HEAO-3-C2. Les abondances relatives des elements de charge 4 ≤ Z ≤ 28 et le spectre d'energie absolu de ces elements sont determines.
124 citations
TL;DR: In this paper, the authors derived the energy and rigidity spectra of the primary cosmic ray proton and helium nuclei intensities in the range from a few MeV nuc−1 to ∼100 GeV nunc−1 using a considerable body of recently published data.
Abstract: We have re-examined and extended the measurements of the primary cosmic ray proton and helium nuclei intensities in the range from a few MeV nuc−1 to ∼100 GeV nuc−1 using a considerable body of recently published data. The differential spectra obtained from this data are determined as a function of both energy and rigidity. The exponents of the energy spectra of both protons and helium nuclei are found to be different at the same energy/nucleon and to increase with increasing energy between 1 and 100 GeV nuc−1 reaching a value=−2.70 at higher energies and in addition, theP/He ratio changes from a value ≲5 at 1 GeV nuc−1 and below to a value ∼30 at 100 GeV nuc−1. On a rigidity representation the spectral exponent for each species is nearly identical and remains virtually constant above several GV at a value of −2.70, and in addition, theP/He ratio is also a constant ∼7 above ∼3 GeV. The changingP/He ratio and spectral exponent on an energy representation occur at energies well above those at which interplanetary modulation effects or interstellar ionization energy loss effects can significantly affect the spectra. In effect by comparing energy spectra and rigidity spectra in the intermediate energy range above the point where solar modulation effects and interstellar energy loss effects are important, but in the range where there are significant differences between energy and rigidity spectra, we deduce that the cosmic ray source spectra are effectively rigidity spectra. This fact has important implications regarding the mechanism of acceleration of this radiation and also with regard to the form of the assumed galactic spectrum at low energies. The relationship between the proton and helium spectra derived here and the heavier nuclei spectral differences recently reported in the literature is also examined. If rigidity spectra are adopted for protons and helium nuclei, then the source abundance ratio of these two components is determined to be ∼7:1. Some cosmological implications of this ratio are discussed.
71 citations
TL;DR: In this article, the last of a set of five papers reporting latitude surveys carried out in 1965 and 1966 at the time of and soon after the IQSY cosmic-ray maximum, the observations are reduced to a common...
Abstract: In this, the last of a set of five papers reporting latitude surveys carried out in 1965 and 1966 at the time of and soon after the IQSY cosmic-ray maximum, the observations are reduced to a common...
49 citations