scholarly journals An Analysis of Cosmic Ray Air Showers for the Determination of Shower Age

1993 ◽  
Vol 46 (4) ◽  
pp. 589 ◽  
Author(s):  
S Sanyal ◽  
B Ghosh ◽  
SK Sarkar ◽  
A Bhadra ◽  
A Mukherjee ◽  
...  
Keyword(s):  
Size Range ◽  
Age Distribution ◽  
Radial Distance ◽  
Cosmic Ray ◽  
Shower Axis ◽  
The Other ◽  
Air Showers ◽  
Shower Size ◽  
Electron Photon

A sample of 8651 air showers in the size range 104 . 3_106 . 2 has been analysed to determine the distribution of the measured age in terms of (i) the number of showers in a specified size range, and (ii) the radial distances in individual showers. It is shown that the radial age distribution in an individual shower leads to an average shower age approximately the same as the prediction of the electron-photon cascade theory. The other results include a study of the variation of (i) shower age, as measured by the x2-minimisation technique, with shower size of vertically incident showers, and (ii) the measured electron density at any point with its radial distance from the shower axis, as a function of the age of a large shower group with very small spread in size. A comparison of similar measurements with relevant theory is also included.

Lateral distribution and energy spectra of high-energy muons in cosmic-ray air showers

1990 ◽  
Vol 68 (1) ◽  
pp. 41-48 ◽  
Author(s):  
D. K. Basak ◽  
S. K. Sarkar ◽  
N. Mukherjee ◽  
S. Sanyal ◽  
B. Ghosh ◽  
...  
Keyword(s):  
Size Range ◽  
Detection Efficiency ◽  
Cosmic Ray ◽  
High Energy ◽  
Lateral Distribution ◽  
Energy Spectra ◽  
Recent Experimental Data ◽  
Air Showers ◽  
Shower Size ◽  
Primary Composition

The energy spectra and the lateral distribution of muons in cosmic-ray air showers, in the size range 104–106 particles as measured by two magnetic spectrographs each of full detection efficiency for muons in the energy range 2.5–500 GeV, are presented along with the derived muon size vs. shower size results. Comparisons with similar recent experimental data and calculations are given to infer the cosmic-ray primary composition.

A study of the cores of air showers in the size range 104 to 107 particles

1968 ◽  
Vol 46 (10) ◽  
pp. S30-S32 ◽  
Author(s):  
A. M. Bakich ◽  
D. Melley ◽  
C. B. A. McCusker ◽  
D. Nelson ◽  
L. S. Peak ◽  
...  
Keyword(s):  
Transverse Momentum ◽  
Size Range ◽  
Cosmic Ray ◽  
High Energy ◽  
Air Showers ◽  
Shower Size ◽  
Charge Spectrum ◽  
Very High Energy ◽  
The Mean ◽  
Very High

Results from the Sydney 64-scintillator array are reported. The array now uses logarithmic amplifiers with a range from 1 to 300 000 particles per square meter. This allows us to detect both higher and lower central densities than was previously possible. Further observations and comparison with Monte Carlo calculations confirm the previous result that air showers in the size range 104 to 5 × 105 particles are due to cosmic-ray primaries with much the same charge spectrum as at 1011 eV total energy.Showers of size greater than 106 particles seem mostly to be multicored (in agreement with previous results). The apparent transverse momentum is high and increases with shower size. The quantity rpL/n, which is a measure of the mean transverse momentum in very high energy interactions, is always greater than 1 GeV/c and increases with shower size. The existence and nature of a possible superstrong interaction are briefly discussed.

Low-energy muons in extensive air showers at 800 g cm−2

1968 ◽  
Vol 46 (10) ◽  
pp. S131-S135 ◽  
Author(s):  
B. K. Chatterjee ◽  
N. V. Gopalakrishnan ◽  
G. T. Murthy ◽  
S. Naranan ◽  
B. V. Sreekantan ◽  
...  
Keyword(s):  
Size Range ◽  
Low Energy ◽  
Extensive Air Showers ◽  
Air Showers ◽  
Average Total Number ◽  
The Right ◽  
Electron Photon ◽  
Photon Component ◽  
Lateral Structure ◽  
Right Ascension

The following results on the low-energy (> 0.6 GeV and > 1.0 GeV) muons in air showers of size 105 to 2 × 107 at Ootacamund (800 g cm−2) are obtained: (1) The average total number of muons [Formula: see text] varies as Ne0.32 ± 0.2 for 105 < Ne < 106, and as Ne0.8 ± 0.15for 106 < Ne < 2 × 107. (2) In showers showing flat electron lateral structure, the [Formula: see text] variation with Ne is similar to (1). However, in steep showers, [Formula: see text] varies as Ne0.75 ± 0.15 in the whole size range 105 to 2 × 107. (3) "Muon-rich" showers of size < 106 have less energy in the electron–photon component compared to "normal" showers. No such difference is found for showers of size > 106. (4) There is a slight indication of a deficiency of muon-rich showers having a flat lateral distribution of electrons in the right ascension interval 15–21 hours for showers of size 106–107. A similar deficit of showers was observed by the Tokyo group for muon-rich showers in the same RA interval.

scholarly journals Muon Measurements with IceTop

2019 ◽  
Vol 208 ◽  
pp. 03003 ◽  
Author(s):  
Javier G. Gonzalez
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Simulations ◽  
Cosmic Ray ◽  
Shower Axis ◽  
South Pole ◽  
Air Showers ◽  
Hadronic Interaction ◽  
Interaction Models ◽  
Lateral Distance ◽  
Cosmic Ray Flux

We present the measurement of the density of GeV muons in near-vertical air showers by the IceTop array at the South Pole. The muon density is measured at 600 m and 800 m lateral distance from the shower axis in air showers between 1 PeV and 100 PeV. This result can be used to constrain hadronic interaction models by comparing it with the outcome of Monte Carlo simulations. We show that some models do not produce muon densities in agreement with this result unless an unphysical composition of the primary cosmic ray flux is assumed.

The Kolar Gold Fields extensive air shower experiment

1968 ◽  
Vol 46 (10) ◽  
pp. S13-S16 ◽  
Author(s):  
B. K. Chatterjee ◽  
G. T. Murthy ◽  
S. Naranan ◽  
K. Sivaprasad ◽  
B. V. Sreekantan ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Size Range ◽  
High Energy ◽  
Lateral Distribution ◽  
Extensive Air Showers ◽  
Lateral Spread ◽  
Air Showers ◽  
Extensive Air Shower ◽  
Air Shower ◽  
Shower Size

Measurements have been made on high-energy muons (>220 GeV and >640 GeV) in extensive air showers in the size range 105–107 particles. Results on the energy spectrum, lateral spread (for Eμ > 220 GeV), and the dependence of the total number of muons on the shower size are given. The relation between the number of muons (Nμ) and the shower size (N) can be expressed as[Formula: see text]Assuming an exponential lateral distribution of high-energy muons, the average lateral spread of muons of energy >220 GeV has been found to be ~40 m.The results are compared with the predictions of the calculations done by Murthy et al. (1967).

scholarly journals Monte Carlo simulation of the cosmic muon charge ratio

2021 ◽  
Vol 49 (1) ◽  
Author(s):  
Abd Al Karim Haj Ismail ◽  
◽  
Keyword(s):  
Monte Carlo ◽  
Charged Particles ◽  
Radial Distance ◽  
Cosmic Ray ◽  
Charge Ratio ◽  
Air Showers ◽  
Central European ◽  
Hadronic Interactions ◽  
High Energies ◽  
Deep Underground

The muonic component of air showers is sensitive to the mass and energy of the primary cosmic ray and is the most abundant component of charged particles arriving at the surface, and able to penetrate deep underground. The muon charge ratio, defined as the number of positive over negatively charged muons, is a very interesting quantity for the study of hadronic interactions at high energies and the nature of cosmic ray primaries. Furthermore, Earth's atmosphere is the development medium of cosmic air showers before they arrive at the ground. Therefore, variations in the density of the atmosphere between seasons must be studied. It is also very important to account for the zenith angular dependence of atmospheric muons, in particular for showers penetrating the atmosphere at high zenith angles. We present a study of the muon charge ratio using Monte Carlo simulations of two cosmic primaries, proton, and iron, of 100 TeV and 1 PeV energies, and with a zenith angle of 0° to 60°. The dependence on the direction of extensive air showers EAS and their radial distance appears to be very pronounced. In addition, the muon density is discussed assuming the Central European Atmosphere in June and December.

Energy determination of electron-photon showers induced by heavy cosmic-ray primaries

1989 ◽  
Vol 276 (1-2) ◽  
pp. 317-339 ◽  
Author(s):  
Takashi Fujinaga ◽  
Masakazu Ichimura ◽  
Yasuo Niihori ◽  
Toru Shibata
Keyword(s):  
Cosmic Ray ◽  
Electron Photon ◽  
Energy Determination

scholarly journals Latest Cosmic Ray Results from IceTop and IceCube

2019 ◽  
Vol 210 ◽  
pp. 03005
Author(s):  
Karen Andeen ◽  
Matthias Plum
Keyword(s):  
Energy Spectrum ◽  
Cosmic Rays ◽  
Gamma Ray ◽  
Cosmic Ray ◽  
High Energy ◽  
Low Energy ◽  
South Pole ◽  
Air Showers ◽  
Future Plans

The IceCube Neutrino Observatory at the geographic South Pole, with its surface array IceTop, detects three different components of extensive air showers: the total signal at the surface, low energy muons on the periphery of the showers, and high energy muons in the deep In Ice array of IceCube. These measurements enable determination of the energy spectrum and composition of cosmic rays from PeV to EeV energies, the anisotropy in the distribution of cosmic ray arrival directions, the muon density of cosmic ray air showers, and the PeV gamma-ray flux. Furthermore, IceTop can be used as a veto for the neutrino measurements. The latest results from these IceTop analyses will be presented along with future plans.

Late arriving particles in cosmic ray air showers and determination of UHECR energies by AGASA

2005 ◽  
Vol 24 (4-5) ◽  
pp. 372-381 ◽  
Author(s):  
Hans-Joachim Drescher ◽  
Glennys R. Farrar
Keyword(s):  
Cosmic Ray ◽  
Air Showers
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