A proposed apparatus for the measurement of the cosmic-ray muon momentum spectrum and charge ratio, and the investigation of muon interactions

1968 ◽  
Vol 46 (10) ◽  
pp. S1135-S1139 ◽  
Author(s):  
R. M. Bull ◽  
W. F. Nash ◽  
Wendy J. Milne ◽  
R. E. Woodham ◽  
Y. Yeivin ◽  
...  
Keyword(s):  
Cosmic Ray ◽  
Momentum Spectrum ◽  
Muon Flux ◽  
Low Energy ◽  
Charge Ratio ◽  
Energy Component ◽  
Expected Performance ◽  
Muon Momentum

The construction of a cosmic-ray spark-chamber spectrometer for use in the study of the charge ratio and interactions of muons at energies up to 3 000 GeV is proposed. The apparatus will consist of a stack of interleaved spark chambers and magnetized iron plates, placed at a depth of 250 m.w.e. underground in order to remove the low-energy component of the cosmic-ray muon flux. This report gives an appraisal of the design of the apparatus and summarizes its expected performance.

The muon spectra near the geomagnetic equator

1968 ◽  
Vol 46 (10) ◽  
pp. S301-S305 ◽  
Author(s):  
O. C. Allkofer ◽  
R. D. Andresen ◽  
W. D. Dau
Keyword(s):  
Integral Intensity ◽  
Geomagnetic Latitude ◽  
Cosmic Ray ◽  
Momentum Spectrum ◽  
Low Energy ◽  
Charge Ratio ◽  
Theoretical Spectrum ◽  
Measured Spectrum ◽  
Geomagnetic Equator ◽  
Chamber Technique

The vertical momentum spectrum and the charge ratio of cosmic-ray muons have been investigated in the range 0.3–25 GeV/c at a geomagnetic latitude of λ = 9 °N at sea level. The investigations have been performed by means of a magnetic spectrograph using the spark chamber technique for track location. The measured spectrum in the low-energy region is about 20% smaller than the spectra at high geomagnetic latitudes. The integral intensity for particles which penetrate more than 15 cm of lead is 7.25 × 10−3 cm−2 s−1 sr−1. The theoretical spectrum after Olbert is in agreement with our results.

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.

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.

Arrangement for measuring the momentum spectrum and the charge ratio of the high-energy cosmic-ray muon horizontal flux

1968 ◽  
Vol 46 (10) ◽  
pp. S1169-S1171
Author(s):  
S. V. Alchudjian ◽  
T. L. Asatiani ◽  
H. V. Badalian ◽  
K. A. Gazarian ◽  
G. I. Mekilov ◽  
...  
Keyword(s):  
Charged Particles ◽  
Cosmic Ray ◽  
High Energy ◽  
Momentum Spectrum ◽  
Magnetic Spectrometer ◽  
Charge Ratio ◽  
Horizontal Flux ◽  
The Wire ◽  
With Memory

The magnetic spectrometer of the wire spark chambers with memory of ferrite cores designed for the measurement of the momentum spectrum of high-energy muons (p ~ 3 × 103 GeV/c) at large zenith angles is described. Some characteristics of the wire spark chambers of large dimensions (S ~ 1 m2) are given. The magnetic deflections of the charged particles are automatically calculated and printed by means of a special calculating device. The ferrite memories of the wire spark chambers were directly used as "memory of the device".

Search for low-energy interplanetary positrons

1968 ◽  
Vol 46 (10) ◽  
pp. S527-S529 ◽  
Author(s):  
T. L. Cline ◽  
E. W. Hones Jr.
Keyword(s):  
Counting Rate ◽  
Cosmic Ray ◽  
Primary Component ◽  
Low Energy ◽  
Charge Ratio ◽  
Great Abundance ◽  
Independent Source ◽  
Equilibrium Charge ◽  
Energy Dependent ◽  
Background Effect

Preliminary results of an experiment designed to detect and measure the intensity of interplanetary positrons of energy 0–3 MeV with the satellites OGO-I and OGO-III are outlined. Evidence for a statistically significant counting rate of detected positrons is presented, and the possibility that these particles represent a true primary component rather than a background effect, such as cosmic-ray induced secondaries in the detector, is considered. It is shown that the apparent intensity of low-energy positrons, assuming that value derived from their counting rate, would be consistent with an equilibrium charge ratio. This result would not be predicted with mechanisms involving the ionization of matter or the acceleration of electrons, but would be consistent with a strongly energy-dependent galactic trapping parameter allowing meson-decay electrons to slow down in great abundance, or with the existence of an independent source.

The results of simultaneous measurements of the cosmic-ray intensity over the Antarctic and Arctic

1968 ◽  
Vol 46 (10) ◽  
pp. S823-S824
Author(s):  
S. N. Vernov ◽  
A. N. Charakhchyan ◽  
T. N. Charakhchyan ◽  
Yu. J. Stozhkov
Keyword(s):  
Cosmic Rays ◽  
Temperature Effects ◽  
Cosmic Ray ◽  
Primary Component ◽  
Low Energy ◽  
Cosmic Ray Intensity ◽  
Simultaneous Measurements ◽  
Murmansk Region ◽  
The Antarctic

The results of the analysis of data obtained from measurements carried out by means of regular stratospheric launchings of cosmic-ray radiosondes over the Murmansk region and the Antarctic observatory in Mirny in 1963–66 are presented. The problem of the anisotropy of the primary component of low-energy cosmic rays and of temperature effects on the cosmic-ray intensity in the atmosphere are discussed.

scholarly journals Measurement of Low-Energy Cosmic-Ray Antiprotons at Solar Minimum

1998 ◽  
Vol 81 (19) ◽  
pp. 4052-4055 ◽  
Author(s):  
H. Matsunaga ◽  
S. Orito ◽  
H. Matsumoto ◽  
K. Yoshimura ◽  
A. Moiseev ◽  
...  
Keyword(s):  
Solar Minimum ◽  
Cosmic Ray ◽  
Low Energy
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