Energy spectrum of low energy cosmic ray neutrons at sea level

1982 ◽  
Vol 32 (10) ◽  
pp. 1183-1186
Author(s):  
S. R. Ganguly ◽  
Banashree Mitra ◽  
S. D. Chatterjee
Keyword(s):  
Energy Spectrum ◽  
Sea Level ◽  
Cosmic Ray ◽  
Low Energy

Energy spectrum of cosmic-ray muons at sea level

1964 ◽  
Vol 32 (6) ◽  
pp. 1524-1540 ◽  
Author(s):  
S. Miyake ◽  
V. S. Narasimham ◽  
P. V. Ramana Murthy
Keyword(s):  
Energy Spectrum ◽  
Sea Level ◽  
Cosmic Ray

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.

Time Dependence of the Decay Energy Spectrum for Stopped Cosmic-Ray Particles at Sea Level

1963 ◽  
Vol 132 (4) ◽  
pp. 1803-1809
Author(s):  
Elihu Boldt ◽  
Paul Stoler ◽  
Costa Tsipis
Keyword(s):  
Energy Spectrum ◽  
Time Dependence ◽  
Sea Level ◽  
Cosmic Ray ◽  
Decay Energy

The energy spectrum of cosmic ray pions near sea level in the range 0.7-150 GeV

1964 ◽  
Vol 83 (5) ◽  
pp. 871-877 ◽  
Author(s):  
G Brooke ◽  
M A Meyer ◽  
A W Wolfendale
Keyword(s):  
Energy Spectrum ◽  
Sea Level ◽  
Cosmic Ray

Satellite measurements of the low-energy cosmic-ray Li, Be, B, C, N, O, F nuclei and their implications

1968 ◽  
Vol 46 (10) ◽  
pp. S548-S552 ◽  
Author(s):  
C. Y. Fan ◽  
George Gloeckler ◽  
J. A. Simpson
Keyword(s):  
Energy Spectrum ◽  
Interplanetary Space ◽  
Cosmic Ray ◽  
Low Energy ◽  
Solar Modulation ◽  
Chemical Abundance ◽  
Satellite Measurements ◽  
Differential Energy Spectrum

The differential energy spectrum and chemical abundance of individual elements from lithium to fluorine have been measured near minimum solar modulation (June 1965 to March 1966) in interplanetary space on the IMP-III satellite. The spectra for Li, Be, and B are found to increase with decreasing energy below ~60 MeV/nucleon. The consequences of these results on the propagation and lifetimes of cosmic-ray particles are discussed.

scholarly journals A Comparison of Muon Flux Models at Sea Level for Muon Imaging and Low Background Experiments

2021 ◽  
Vol 9 ◽  
Author(s):  
Ning Su ◽  
Yuanyuan Liu ◽  
Li Wang ◽  
Bin Wu ◽  
Jianping Cheng
Keyword(s):  
Experimental Data ◽  
Monte Carlo ◽  
Sea Level ◽  
Flux Distribution ◽  
Monte Carlo Model ◽  
Cosmic Ray ◽  
Muon Flux ◽  
Low Energy ◽  
Analytical Models ◽  
Low Background

Cosmic-ray muons are a type of natural radiation with high energy and a strong penetration ability. The flux distribution of such particles at sea level is a key problem in many areas, especially in the field of muon imaging and low background experiments. This paper summarizes the existing models to describe sea-level muon flux distributions. According to different means used, four parametric analytical models and one Monte Carlo model, which is referred to as CRY, are selected as typical sea-level muon flux distribution models. Then, the theoretical values of sea-level muon fluxes given by these models are compared with the experimental sea-level muon differential flux data with kinetic energy values in the range of 1–1,000 GeV in the directions of zenith angles 0° and 75°. The goodness of fit of these models to the experimental data was quantitatively calculated by Pearson’s chi-square test. The results of the comparison show that the commonly used Gaisser model overestimates the muon flux in the low-energy region, while the muon flux given by the Monte Carlo model CRY at the large zenith angle of 75° is significantly lower than that of the experimental data. The muon flux distribution given by the other three parametric analytical models is consistent with the experimental data. The results indicate that the original Gaisser model is invalid in the low energy range, and CRY apparently deviates at large zenith angles. These two models can be substituted with the muon flux models given by Gaisser/Tang, Bugaev/Reyna, and Smith and Duller/Chatzidakis according to actual experimental conditions.

Primary-cosmic-ray energy spectrum up to 50 TeV derived from sea-level muon measurements

1985 ◽  
Vol 31 (7) ◽  
pp. 1557-1560 ◽  
Author(s):  
O. C. Allkofer ◽  
W. D. Dau ◽  
H. Jokisch ◽  
G. Klemke ◽  
R. C. Uhr ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Sea Level ◽  
Cosmic Ray

Measurements of the energy spectrum of cosmic-ray muons at sea-level with emulsion chambers

1978 ◽  
Vol 48 (4) ◽  
pp. 429-445 ◽  
Author(s):  
K. Mizutani ◽  
A. Misaki ◽  
T. Shirai ◽  
Z. Watanabe ◽  
M. Akashi ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Sea Level ◽  
Cosmic Ray

The energy spectrum of cosmic ray protons at sea level

1956 ◽  
Vol 4 (S2) ◽  
pp. 905-907
Author(s):  
H. Filthuth
Keyword(s):  
Energy Spectrum ◽  
Sea Level ◽  
Cosmic Ray
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