scholarly journals Derivation of Muon Intensities in Sea-water Depths up to 1400 M.W.E. from a Recent Primary Cosmic Ray Spectrum

1984 ◽  
Vol 37 (5) ◽  
pp. 575 ◽  
Author(s):  
DP Bhattacharyya ◽  
Pratibha Pal ◽  
A Mukhopadhyay
Keyword(s):  
Experimental Data ◽  
Energy Loss ◽  
Pair Production ◽  
Sea Water ◽  
Cosmic Ray ◽  
Muon Energy ◽  
Energy Relation ◽  
Scaling Hypothesis ◽  
Nuclear Interactions ◽  
Water Depths

The muon intensities in sea-water depths up to 1400 M.W.E. have been derived from a recent primary cosmic ray spectrum. The scaling hypothesis of Feynman has been used in the calculation of meson spectra in the atmosphere. The range-energy relation for muons in sea water, used in the present work, accounts for the muon energy loss in sea water due to collisions, pair production, bremsstrahlung and nuclear interactions. The calculated muon range spectrum in sea water is well in accord with the experimental data obtained by Higashi et al. (1966), Davitaev et al. (1969), and Rogers and Tristam (1981, 1983

Derivation of muon range spectrum under rock from the recent primary spectrum

1985 ◽  
Vol 63 (8) ◽  
pp. 1050-1060 ◽  
Author(s):  
Pratibha Pal ◽  
D. P. Bhattacharyya
Keyword(s):  
Cosmic Ray ◽  
Muon Energy ◽  
Energy Relation ◽  
Muon Spectrum ◽  
Primary Spectrum ◽  
Atmospheric Diffusion ◽  
Data Compilation ◽  
Scaling Hypothesis ◽  
Burst Data ◽  
Good Agreement

The muon range spectra under Mont Blanc Tunnel and Kolar Gold Field rocks have been calculated from the recently measured primary cosmic ray spectrum. The scaling hypothesis of Feynman has been used for the calculation of pion and kaon spectra in the atmosphere. The meson atmospheric diffusion equation has been solved by following the method of Bugaev et al. The derived muon energy spectrum has been found to be in good agreement with the measured data of the Kiel, Durham, DEIS, and Moscow University groups. The calculated muon energy spectra at large polar angles have been compared with the different experimental results. The integral muon spectrum up to 20 TeV supports the MARS burst data favourably. Using the procedure of Kobayakawa, the muon energy loss in rock due to ionization, pair production, and bremsstrahlung and nuclear interactions from Bezrukov and Bugaev, we have constructed the range–energy relation in Mont Blanc and Kolar Gold Field rocks. The estimated range spectra have been corrected for range fluctuations and have been compared with the Mont Blanc Tunnel data of Castagnoli et al., Bergamasco et al., and Sheldon et al. and the Kolar Gold Field data compilation by Krishnaswamy et al.

scholarly journals Energy loss measurements of inclined muon bundles in the Cherenkov water detector

2019 ◽  
Vol 208 ◽  
pp. 08006
Author(s):  
R.P. Kokoulin ◽  
N.S. Barbashina ◽  
A.G. Bogdanov ◽  
S.S. Khokhlov ◽  
V.A. Khomyakov ◽  
...  
Keyword(s):  
Energy Loss ◽  
Average Energy ◽  
Cosmic Ray ◽  
Muon Energy ◽  
Single Experiment ◽  
Muon Component ◽  
Energy Deposit ◽  
Tracking Detector ◽  
Wide Range ◽  
Muon Bundles

An experiment on the measurements of the energy deposit of inclined cosmic ray muon bundles is being conducted at the experimental complex NEVOD (MEPhI). The complex includes the Cherenkov water calorimeter with a volume of 2000 m3 and the coordinate-tracking detector DECOR with a total area of 70 m2. The DECOR data are used to determine the local muon densities in the bundle events and their arrival directions, while the energy deposits (and hence the average muon energy loss) are evaluated from the Cherenkov calorimeter response. Average energy loss carries information about the mean muon energy in the bundles. The detection of the bundles in a wide range of muon multiplicities and zenith angles gives the opportunity to explore the energy range of primary cosmic ray particles from about 10 to 1000 PeV in the frame of a single experiment with a relatively small compact setup. Experimental results on the dependence of the muon bundle energy deposit on the zenith angle and the local muon density are presented and compared with expectations based on simulations of the EAS muon component with the CORSIKA code.

Imaging large vessels using cosmic-ray muon energy-loss techniques

2007 ◽  
Vol 130 (2-3) ◽  
pp. 75-78 ◽  
Author(s):  
P JENNESON ◽  
W GILBOY ◽  
S SIMONS ◽  
S STANLEY ◽  
D RHODES
Keyword(s):  
Energy Loss ◽  
Cosmic Ray ◽  
Muon Energy ◽  
Large Vessels

Muon interactions in the energy range 5 to 1 000 GeV

1968 ◽  
Vol 46 (10) ◽  
pp. S365-S368 ◽  
Author(s):  
G. N. Kelly ◽  
P. K. MacKeown ◽  
S. S. Said ◽  
A. W. Wolfendale
Keyword(s):  
Energy Range ◽  
Pair Production ◽  
High Probability ◽  
Considerable Increase ◽  
Cosmic Ray ◽  
Ground Level ◽  
Muon Energy ◽  
Frequency Of Occurrence ◽  
Electromagnetic Showers ◽  
Electromagnetic Interactions

The Durham Horizontal Spectrograph has been used to study the variation with energy of the frequency of electromagnetic interactions of muons. A considerable increase in the frequency of occurrence of electromagnetic showers with muon energy is observed and is attributable in the main to direct pair production. The form of the variation with energy of the interaction probabilities and the frequency of successive interactions of the same particle are consistent with all the particles being muons, and it is concluded that there is no evidence in favor of the existence of particles having an unusually high probability of burst production–the X particles postulated by Vernov et al. (1966)–at least in the near-horizontal cosmic-ray beam at ground level.

IONIZATION LOSS BY COSMIC-RAY MU-MESONS IN ARGON

1959 ◽  
Vol 37 (2) ◽  
pp. 189-202 ◽  
Author(s):  
Georges Hall
Keyword(s):  
Experimental Data ◽  
Energy Loss ◽  
Ionization Chamber ◽  
Cosmic Ray ◽  
Statistical Distribution ◽  
Experimental Curve ◽  
Energy Losses ◽  
Ionization Loss ◽  
Electron Collection ◽  
Probable Loss

The ionization of argon by cosmic-ray mu-mesons of minimum specific ionization has been studied by means of a calibrated pressure-ionization chamber using electron collection. Corrections which are shown to be necessary have been applied to the experimental data. The shape of the experimental curve of statistical distribution of energy loss agrees with the theoretically predicted shape, for energy losses greater than the most probable loss (300 kev).

Pair production by muons in the field of nuclei

1968 ◽  
Vol 46 (10) ◽  
pp. S387-S390 ◽  
Author(s):  
S. R. Kelner ◽  
Yu. D. Kotov
Keyword(s):  
Numerical Calculation ◽  
Differential Cross Section ◽  
Energy Loss ◽  
Pair Production ◽  
Cross Section ◽  
Differential Cross ◽  
Muon Energy ◽  
Fermi Model ◽  
Electron Pairs ◽  
Analytical Expressions

The differential cross section for the production of electron pairs by muons has been obtained under the assumption that all particles are relativistic and that the Thomas–Fermi model can be used to evaluate the effect of screening. Analytical expressions have been obtained for the energy loss of muons by pair production for the two extreme cases of "no screening" and "complete screening". Results of numerical calculation of energy loss by this process are given as a function of muon energy, for rock with Z = 11.

scholarly journals On the photon component of cosmic radiation and its absorption coefficient

1940 ◽  
Vol 175 (960) ◽  
pp. 88-100 ◽  
Keyword(s):  
Experimental Data ◽  
Energy Loss ◽  
Cosmic Radiation ◽  
Cosmic Ray ◽  
High Energy ◽  
Soft Component ◽  
Simple Method ◽  
Metal Plates ◽  
Experimental Values ◽  
Photon Component

It has been established that the soft component of the cosmic radiation consists of electrons and photons. Much experimental data on the electrons forming the soft component are available and they are known to form a fraction of about 25-30% of the whole beam of ionizing particles at sea level, excluding particles below 10 7 eV (e.g. Rossi 1933; Nielsen and Morgan 1938). The energy spectrum of the electrons is known roughly from the work of Blackett (1938), Wilson (1939) and others. The energy loss of electrons in metal plates has been investigated by Anderson and Neddermeyer (1934), Blackett and Wilson (1937), Williams (1939), Wilson (1938, 1939), showing that the experimental values of the energy loss are in agreement with the prediction of the quantum theory (Bethe and Heitler 1934). Much less is known about the photon component of cosmic radiation, as comparatively few experiments have been carried out to investigate their properties. Further the results of the investigations available are partly contradictory. The theory of the absorption of high energy photons has been worked out to the same extent as for electrons (Bethe and Heitler). Owing to the lack of experimental material, the theory could be tested only up to energies of about five million volts (McMillan 1934; Gentner 1935). The success of the theory of cascade showers due to Bhabha and Heitler (1937) and Carlson and Oppenheimer (1937), based on the Bethe-Heitler theory of electrons and photons, provides however an indirect test for the validity of the absorption formula for high energy photons. The lack of experimental data on high energy photons is due to the difficulties in the method of observation; photons unlike electrons cannot be observed directly. In the present paper a simple method for investigating cosmic-ray photons is described. Using this method, data about the number, energy distribution and absorption of cosmic-ray photons have been obtained.

scholarly journals Absorption of penetrating cosmic ray particles in gold

1939 ◽  
Vol 172 (951) ◽  
pp. 517-529 ◽  
Keyword(s):  
Experimental Data ◽  
Energy Loss ◽  
Close Agreement ◽  
Cosmic Ray ◽  
Soft Component ◽  
Additional Energy ◽  
Hard Component ◽  
Metal Plates ◽  
Theoretical Predictions ◽  
Absorption Measurements

A considerable amount of experimental data on the energy loss of cosmic-ray particles in metal plates is now available. Much of this, however, represents work carried out before the separate nature of the hard and soft components was fully understood, so that in many cases unsuitable conditions make the interpretation of the results difficult. The soft component is known to consist of electrons, and these predominate in the cosmic-ray energy spectrum for energies less than 2 x 10 8 e-volts. It has been verified for these electrons that the energy loss by ionization (Corson and Brode 1938) and by radiative collisions (Blackett 1938) is in close agreement with the theoretical predictions. At energies greater than 2 x 10 8 e-volts, very few electrons are found at sea level, and for all higher energies the majority of the particles are now considered to be mesotrons. These, together with an uncertain, but small, number of protons form the hard component of the cosmic rays. Absorption measurements for the hard component are more difficult than for the electrons, since the particles are, in general, of higher energy and the loss of energy in an absorbing plate is very much smaller. The early observations (Blackett and Wilson 1937; Crussard and Leprince Ringuet 1937; Wilson 1938 a ) lead to the conclusion that at an electron energy ( E e = 300 Hρ )* of about 5 x 10 8 e-volts, the total energy loss of penetrating particles was very small—of the same order as that due to ionization alone —but that at higher energies, E e ~ 1.5 x 10 9 e-volts, a considerable additional energy loss took place, which did not appear to be attributable to the inclusion of electrons in the measurements (Wilson 1938 a ). With the comparatively thin absorbing plates used, however, it was not certain that all electrons had been excluded from these measurements.

The muon energy spectrum at sea level from the intensities deep underground

1968 ◽  
Vol 46 (10) ◽  
pp. S395-S398 ◽  
Author(s):  
K. Kobayakawa
Keyword(s):  
Energy Spectrum ◽  
Energy Loss ◽  
Sea Level ◽  
Vertical Direction ◽  
Nuclear Interaction ◽  
Muon Energy ◽  
Energy Relation ◽  
Deep Underground ◽  
Energy Relations ◽  
The Average Range

The energy spectrum of muons at sea level is determined from the intensities deep underground. The following three points are different from past treatments: (1) From the energy-loss relation, −(dE/dt) = k(E) + b(E)E, including the effect of nuclear interaction and without the assumption that b is independent of E, the average range–energy relation is derived. (2) The reliable values of the factor which corrects for fluctuations in energy loss of muons passing through a great thickness of material are used. (3) Many authors measured the intensities under their respective rocks. The differences of these rocks are taken into account in the following way. The intensities are directly converted into the energy spectrum at sea level by using the appropriate average range–energy relations and correction factors. The resultant integral exponent of the energy spectrum in the vertical direction is β = 2.541 ± 0.190 with 95% confidence over the energy range 0.4–7 TeV having a weighted mean of 0.7 TeV.

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