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.

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).

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.

High-energy N particles in extensive air showers at 800 g/cm2

1968 ◽  
Vol 46 (10) ◽  
pp. S136-S141 ◽  
Author(s):  
B. K. Chatterjee ◽  
G. T. Murthy ◽  
S. Naranan ◽  
B. V. Sreekantan ◽  
M. V. Srinivasa Rao ◽  
...  
Keyword(s):  
High Energy ◽  
Anomalous Behavior ◽  
Lateral Distribution ◽  
Energy Measurement ◽  
Total Absorption ◽  
Air Showers ◽  
Shower Size ◽  
Total Absorption Spectrometer ◽  
Threshold Energies ◽  
Absorption Spectrometer

The results on high-energy N particles in EAS using a total absorption spectrometer for energy measurement are presented. They are compared with results from other experiments and calculations based upon plausible models of high energy interactions. (1) As expected, the NAP lateral distribution becomes steeper for particles of higher threshold energies. (2) Contrary to expectation, the lateral distribution becomes flatter with increasing shower size. The implication of this anomalous behavior in terms of interaction characteristics at energies > 1014 eV is briefly discussed. (3) For a given size, showers with steeper electron lateral distribution have more NAPs. (4) Except for the behavior of the lateral distribution as a function of size, all the other results can be explained in terms of models in which pT and inelasticity distributions are invariant and some fraction (~15%) of nucleon–antinucleon pair production is assumed.

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.

scholarly journals Model dependence of lateral distribution functions of high energy cosmic ray air showers

2004 ◽  
Vol 21 (1) ◽  
pp. 87-94 ◽  
Author(s):  
Hans-Joachim Drescher ◽  
Marcus Bleicher ◽  
Sven Soff ◽  
Horst Stöcker
Keyword(s):  
Cosmic Ray ◽  
High Energy ◽  
Distribution Functions ◽  
Lateral Distribution ◽  
Air Showers ◽  
Model Dependence

Composition and spectra of primary cosmic-ray electrons and nuclei above 10 10 eV

1975 ◽  
Vol 277 (1270) ◽  
pp. 349-363 ◽  
Keyword(s):  
Cosmic Ray ◽  
High Energy ◽  
Energy Spectra ◽  
Average Lifetime ◽  
Interstellar Space ◽  
Interstellar Matter ◽  
Electromagnetic Interactions ◽  
Nuclear Species ◽  
The Galaxy ◽  
High Energy Particles

Recent experiments have extended the knowledge of the flux and energy spectra of individual cosmic-ray components to much higher energies than had previously been accessible. Both electron and nuclear components show a behaviour at high energy which is unexpected, and which carries information regarding the sources and the propagation of particles between sources and observer. Electromagnetic interactions which are suffered by the electrons in interstellar space should steepen their spectrum, a steepening that would reveal the average lifetime a cosmic-ray particle spends in the galaxy. Measurements up to 1000 GeV show no such steepening. It was discovered that the composition of the nuclear species which is now measured up to 100 GeV/nucleon changes with energy. This change indicates traversal of less interstellar matter by the high energy particles than by those of lower energy. We discuss the experimental evidence and its implication.

scholarly journals Methods to measure the cosmic-ray composition with the Auger Engineering Radio Array

2019 ◽  
Vol 216 ◽  
pp. 02004 ◽  
Author(s):  
Fabrizia Canfora
Keyword(s):  
Cosmic Ray ◽  
High Energy ◽  
Mass Composition ◽  
Atmospheric Depth ◽  
Ultra High Energy ◽  
Air Showers ◽  
Radio Stations ◽  
High Energy Cosmic Rays ◽  
Air Shower ◽  
Number Of Particles

The mass composition of ultra-high-energy cosmic rays plays a key role in the understanding of the origins ofthese rare particles. A composition-sensitive observable is the atmospheric depth at which the air shower reaches the maximum number of particles (Xmax). The Auger Engineering Radio Array (AERA) detects the radio emission inthe 30-80 MHz frequency band from extensive air showers with energies larger than 1017 eV. It consists of more than 150 autonomous radio stations covering an area of about 17 km2. From the distribution of signals measured by the antennas, it is possible to estimate Xmax. In this contribution three independent methods for the estimation of Xmax will be presented.

scholarly journals RADIODETECTION OF COSMIC RAY EXTENSIVE AIR SHOWERS: UPGRADE OF THE CODALEMA EXPERIMENT

2005 ◽  
Vol 20 (29) ◽  
pp. 6869-6871 ◽  
Author(s):  
D. ARDOUIN ◽  
A. BELLETOILE ◽  
D. CHARRIER ◽  
R. DALLIER ◽  
L. DENIS ◽  
...  
Keyword(s):  
Antenna Array ◽  
Background Level ◽  
Cosmic Ray ◽  
High Energy ◽  
Extensive Air Showers ◽  
Ultra High Energy ◽  
Air Showers ◽  
Particle Detectors ◽  
Demonstration Experiment ◽  
And Performance

We present the characteristics and performance of a demonstration experiment devoted to the observation of ultra high-energy cosmic ray extensive air showers using a radiodetection technique. In a first step, one antenna narrowed band filtered acting as trigger, with a 4σ threshold above sky background-level, was used to tag any radio transient in coincidence on the antenna array. Recently, the addition of 4 particle detectors has allowed us to observe cosmic ray events in coincidence with antennas.

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