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 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

Energy spectrum of cosmic ray primaries at super high energies estimated from the recent balloon-borne calorimeter measurements

1983 ◽  
Vol 61 (3) ◽  
pp. 434-439 ◽  
Author(s):  
D. P. Bhattacharyya
Keyword(s):  
Energy Spectrum ◽  
Cosmic Ray ◽  
High Energy ◽  
Japanese American ◽  
Primary Spectrum ◽  
Atmospheric Diffusion ◽  
Neutron Spectra ◽  
High Energy Cosmic Rays ◽  
High Energies ◽  
Scaling Hypothesis

The energy spectrum of primary cosmic ray particles has been estimated from the analysis of the chemical composition data of high energy cosmic rays, data obtained by the Japanese American cooperative emulsion experiments for proton and helium intensities and the Goddard Space Flight Centre measurements for cosmic ray nuclei. The results indicate no drastic change in abundance ratios at high energies. The elemental fluxes have been calculated by assuming that the primary cosmic ray nuclei break up into their constituent nucleons near the top of the atmosphere. The calculated total primary spectrum in the range 2–300 TeV follows the form N(E) dE = 2.24 × 104 E−2.7 dE where E is the energy expressed in GeV/nucleon and N(E) is the intensity expressed in (m2∙s∙sr∙GeV/nucleon) −1.Using this primary spectrum as the source of nucleons near the top of the atmosphere, the sea level proton and neutron spectra have been estimated by using the Feynman scaling hypothesis and the conventional nucleon-atmospheric diffusion equation. The derived spectra are in accord with the measured proton and neutron spectra of Brooke and Wolfendale, Ashton and Coates, and Ashton et al.

MUON FLUXES DERIVED FROM THE DIRECTLY MEASURED PRIMARY COSMIC RAY ELEMENTAL SPECTRA

1996 ◽  
Vol 11 (30) ◽  
pp. 2427-2433
Author(s):  
MALA MITRA ◽  
PRATIBHA PAL ◽  
D.P. BHATTACHARYYA
Keyword(s):  
Cosmic Ray ◽  
Upper Atmosphere ◽  
Energy Spectra ◽  
Muon Energy ◽  
Spectral Indices ◽  
Muon Spectrum ◽  
Indirect Measurements ◽  
Large Zenith Angle ◽  
Nucleon Spectrum ◽  
The Individual

The muon energy spectra at 0° and 89° have been estimated from the decay of nonprompt and prompt mesons created by the individual elemental primary cosmic ray groups during nucleus-air collisions in the upper atmosphere and the results are found to be fairly comparable with the measured muon fluxes obtained from the direct magnetic spectrograph results in Refs. 2–4, and also from the underground indirect measurements in Refs. 5–10. The muon spectrum derived from the single slope primary nucleon spectrum with a constant spectral index of value −2.73 is only slightly different from the present result for energies below 20 TeV. The present muon spectra at large zenith angle exhibit steeper spectral indices when compared to the expected results obtained from primary elemental groups by Parente et al.

Sea level muon spectrum derived from the primary nucleon spectrum using the Cocconi–Koester–Perkins model

1979 ◽  
Vol 57 (3) ◽  
pp. 375-380
Author(s):  
A. K. Chakrabarti ◽  
A. K. Das ◽  
A. K. De
Keyword(s):  
Energy Spectrum ◽  
Sea Level ◽  
Critical Analysis ◽  
Muon Energy ◽  
Measured Spectrum ◽  
Muon Spectrum ◽  
Nucleon Spectrum ◽  
Good Agreement

In a recent paper Sarkar, Bhattacharyya, and Basu have derived the sea level muon energy spectrum from the measured nucleon spectrum of Ryan, Ormes, and Balasubrahmanyan using the Cocconi–Koester–Perkins model. They have found good agreement between this muon spectrum and the precisely measured spectrum of Ayre, Baxendale, Hume, Nandi, Thompson, and Whalley. In this report a critical analysis of the paper has been made and it is found that there are some obvious mistakes both in the formulation and in the calculation. The corrected results do not agree with the Ayre et al. spectrum. The unjustified values of some of the parameters used in their work are discussed.

Das Impulsspektrum der Ultrastrahlungs-Muonen und das Ladungsverhältnis in 5200 m Höhe

1966 ◽  
Vol 21 (8) ◽  
pp. 1205-1210
Author(s):  
O. C. Allkofer ◽  
E. Kraft
Keyword(s):  
Sea Level ◽  
Cosmic Ray ◽  
Theoretical Models ◽  
Momentum Spectrum ◽  
Charge Ratio ◽  
Lead Absorber ◽  
Muon Spectrum ◽  
Total Spectrum ◽  
Good Agreement

The momentum spectrum of cosmic ray muons and the charge ratio at 5200 m above sea level have been measured. To separate the spectrum of muons from the total spectrum a lead absorber was used. From theoretical models the spectrum of muons is calculated. Good agreement is found between the calculated and measured muon spectrum.

Pion production spectrum from primary cosmic ray spectrum and scaling constants

1977 ◽  
Vol 55 (2) ◽  
pp. 154-157 ◽  
Author(s):  
D. P. Bhattacharyya ◽  
R. K. Roy Choudhury ◽  
D. Basu
Keyword(s):  
Energy Spectrum ◽  
Sea Level ◽  
Satellite Data ◽  
Pion Production ◽  
Cosmic Ray ◽  
Muon Spectrum ◽  
Production Spectrum ◽  
Average Value ◽  
Scaling Hypothesis ◽  
Cosmic Muons

The scaling hypothesis of Dao et at. in p + p → π− + X reactions has been used to derive the sea level spectrum of cosmic muons from the satellite data of primary cosmic ray nucleons. It is found that the derived pion production spectrum depends on [Formula: see text], the average value of the Feynman variable x. Taking as input the energy spectrum of primary cosmic ray nucleons determined by Grigorov et al., as well as the sea level muon spectrum determined by Allkofer, Carstensen, and Dau, the value of [Formula: see text] at different pion energies has been estimated. A fit to the calculated results gives the following energy dependence of [Formula: see text]:[Formula: see text]

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