Cosmic ray sea level muon spectrum at large zenith angle derived from the latest JACEE primary spectrum

1985 ◽  
Vol 35 (8) ◽  
pp. 892-895 ◽  
Author(s):  
D. P. Bhattacharyya
Keyword(s):  
Sea Level ◽  
Zenith Angle ◽  
Cosmic Ray ◽  
Muon Spectrum ◽  
Primary Spectrum ◽  
Large Zenith Angle

Sea level muon spectrum from pion and kaon spectra in the atmosphere

1976 ◽  
Vol 54 (18) ◽  
pp. 1880-1883 ◽  
Author(s):  
Deba Prasad Bhattacharyya
Keyword(s):  
Diffusion Equation ◽  
Sea Level ◽  
Satellite Data ◽  
Cosmic Ray ◽  
Muon Spectrum ◽  
Momentum Range ◽  
Type Distribution ◽  
Muon Momentum ◽  
Muon Intensity

The pion and kaon spectra in the top of the atmosphere have been derived from the satellite data of cosmic ray nucleons by using the Bose-type distribution of secondary mesons produced in the inclusive reactions p + p → π− + X and p + p → K− + X. The derived pion and kaon spectra follow the relations of the form π(Eπ) dEπ = 0.184Eπ−2.6 dEπ and K(Ek) dEk = 0.036 Ek−2.6 dEk. With the help of the diffusion equation for pions and kaons in the atmosphere, the sea level muon spectrum has been derived and the results have been compared with the magnetic spectrograph data of Allkofer, Carstensen, and Dau in the muon momentum range 15–1000 GeV/c. The sea level muon intensity arising from kaon parentage increases with energy.

The rate of energy loss of high-energy cosmic ray muons

1963 ◽  
Vol 275 (1362) ◽  
pp. 391-410 ◽  
Keyword(s):  
Energy Spectrum ◽  
Energy Loss ◽  
Sea Level ◽  
Cosmic Ray ◽  
Nuclear Interaction ◽  
High Energy ◽  
Level Energy ◽  
Muon Spectrum ◽  
The Third ◽  
Muon Mass

The rate of energy loss of muons is examined by com paring the observed depth-intensity relation with that predicted from a knowledge of the sea-level energy spectrum of cosmic ray muons. The evidence for each of the parameters entering into the analysis is assessed and estimates are made of the sea-level muon spectrum up to 10000 GeV and the depth-intensity relation down to 7000 m.w.e. The effect of range-straggling on the underground intensities is considered and shown to be important at depths below 1000 m.w.e. Following previous workers the energy loss relation is written as -d E /d x =1.88+0.077 in E ' m / mc 2 + b E MeV g -1 cm 2 , where E ' m is the maximum transferrable energy in a /i-e collision and m is the muon mass. The first two terms give the contribution from ionization (and excitation) loss and the third term is the combined contribution from pair production, bremsstrahlung and nuclear interaction. The best estimate of the coefficient b from the present work is b = (3.95 + 0.25) x 10 -6 g -1 cm 2 over the energy range 500 to 10000 GeV, which is close to the theoretical value of 4.0 x 10 -6 g -1 cm 2 . It is concluded that there is no evidence for any marked anomaly in the energy loss processes for muons of energies up to 10000 GeV.

scholarly journals Zenith Angle Dependence of Cosmic Ray Shower Development from Observations of the Time Structure of Atmospheric Cerenkov Pulses

1980 ◽  
Vol 33 (3) ◽  
pp. 607 ◽  
Author(s):  
RW Clay ◽  
GJ Thornton
Keyword(s):  
Sea Level ◽  
Zenith Angle ◽  
Cosmic Ray ◽  
Time Structure ◽  
Extensive Air Showers ◽  
Attenuation Length ◽  
Air Showers ◽  
Angle Dependence ◽  
Shower Development

The attenuation of extensive air showers has been studied using atmospheric Cerenkov techniques. Observations over a range of zenith angles are correlated and an attenuation length of 234 � 38 g cm ? 2 obtained for showers with sea-level sizes of ~ 106 ?

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.

Investigation of the zenith angle dependence of cosmic-ray muons at sea level

Pramana ◽  
2013 ◽  
Vol 80 (5) ◽  
pp. 837-846 ◽  
Author(s):  
MEHMET BEKTASOGLU ◽  
HALIL ARSLAN
Keyword(s):  
Sea Level ◽  
Zenith Angle ◽  
Cosmic Ray ◽  
Angle Dependence

Cosmic-ray muon spectrum up to 1 TeV at 75° zenith angle

1979 ◽  
Vol 19 (5) ◽  
pp. 1368-1372 ◽  
Author(s):  
H. Jokisch ◽  
K. Carstensen ◽  
W. D. Dau ◽  
H. J. Meyer ◽  
O. C. Allkofer
Keyword(s):  
Zenith Angle ◽  
Cosmic Ray ◽  
Muon Spectrum

scholarly journals Muon “depth-intensity” relation measured by the LVD underground experiment and cosmic-ray muon spectrum at sea level

1998 ◽  
Vol 58 (9) ◽  
Author(s):  
M. Aglietta ◽  
B. Alpat ◽  
E. D. Alyea ◽  
P. Antonioli ◽  
G. Badino ◽  
...  
Keyword(s):  
Sea Level ◽  
Cosmic Ray ◽  
Muon Spectrum ◽  
Underground Experiment
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