LATERAL DISTRIBUTION OF MUONS IN EAS AS A FUNCTION OF PRIMARY ENERGY

2005 ◽  
Vol 20 (29) ◽  
pp. 6808-6810
Author(s):  
V. EGANOV ◽  
A. GARYAKA ◽  
R. MARTIROSOV ◽  
E. MNATSAKANYAN ◽  
L.-W. JONES ◽  
...  
Keyword(s):  
Primary Energy ◽  
Lateral Distribution ◽  
New Method ◽  
Knee Region ◽  
Approximation Function ◽  
Primary Particles ◽  
Muon Hodoscope

Experimental EAS muon lateral distributions for Eμ ≥ 5 GeV at fixed primary energy at the knee region measured with the modernized muon hodoscope of the GAMMA installation (Mt. Aragats, Armenia) are presented. Comparison with the data of the previous hodoscope configuration for fixed shower sizes is made. The experimental muon lateral distributions at fixed primary energies are obtained using a new method for estimation of energy of the primary particles. Approximation function for experimental distributions is proposed. Data are compared with the simulated CORSIKA data.

scholarly journals Study of Cherenkov light lateral distribution function around the knee region in extensive air showers

2015 ◽  
pp. 79-85
Author(s):  
A. Al-Rubaiee ◽  
U. Hashim ◽  
M. Marwah ◽  
Y. Al-Douri
Keyword(s):  
Distribution Function ◽  
Cherenkov Radiation ◽  
Cosmic Ray ◽  
Primary Energy ◽  
Lateral Distribution ◽  
Cherenkov Light ◽  
Air Showers ◽  
Knee Region ◽  
Lateral Distribution Function ◽  
Primary Particles

The Cherenkov light lateral distribution function (LDF) was simulated with the CORSIKAcode in the energy range (1013 - 1016) eV. This simulation was performed for conditions and configurations of the Tunka EAS Cherenkov array for the two primary particles (p and Fe). Basing on the simulated results, many approximated functions are structured for two primary particles and different zenith angles. This allowed us to reconstruct the EAS events, which is, to determine the type and energy of the primary particles that produced showers from signal amplitudes of Cherenkov radiation measured by the Tunka Cherenkov array experiment. Comparison of the calculated LDF of Cherenkov radiation with that measured at the Tunka EAS array shows the ability to identify the primary particle that initiated the EAS cascades by determining its primary energy around the knee region of the cosmic ray spectrum.

scholarly journals Demonstrating of Cosmic Ray Characteristics by Estimating the Cherenkov Light Lateral Distribution Function for Yakutsk Array as a Function of the Zenith Angle

2016 ◽  
Vol 67 ◽  
pp. 21-30
Author(s):  
Marwah M. Abdulsttar ◽  
A.A. Al-Rubaiee ◽  
Abdul Halim K. Ali
Keyword(s):  
Numerical Simulation ◽  
Distribution Function ◽  
Zenith Angle ◽  
Cosmic Ray ◽  
Primary Energy ◽  
Lateral Distribution ◽  
Cherenkov Light ◽  
Air Showers ◽  
Lateral Distribution Function ◽  
Primary Particles

Cherenkov light lateral distribution function (CLLDF) in Extensive Air Showers (EAS) for different primary particles (e-, n , p, F, K and Fe) was simulated using CORSIKA code for conditions and configurations of Yakutsk EAS array with the fixed primary energy 3 PeV around the knee region at different zenith angles. Basing on the results of CLLDF numerical simulation, sets of approximated functions are reconstructed for different primary particles as a function of the zenith angle. A comparison of the parametrized CLLDF with that simulated with Yakutsk EAS array is verified.The parameterized CLLDF also is compared with that measured on the Yakutsk EAS array.

Investigating the Characteristics of Longitudinal Profile of Primary Particles in Extensive Air Showers

2015 ◽  
Vol 754-755 ◽  
pp. 859-864
Author(s):  
A.A. Al-Rubaiee ◽  
Uda Hashim ◽  
Mohd Khairuddin Md Arshad ◽  
A. Rahim Ruslinda ◽  
R.M. Ayub ◽  
...  
Keyword(s):  
Charged Particles ◽  
Cosmic Ray ◽  
Primary Energy ◽  
Extensive Air Showers ◽  
Air Showers ◽  
Longitudinal Development ◽  
Extensive Air Shower ◽  
Primary Particles ◽  
Shower Maximum ◽  
Hadronic Model

One of the characteristics of longitudinal development of extensive air showers is the number of charged particles and depth of shower maximum in extensive air showers as a function of primary energy, which is often used to reconstruct the elemental composition of primary cosmic rays. Studying of extensive air shower characteristics was performed by investigating the longitudinal development parameters depending on Heitler model for different primary particles. The simulation of the number of charged particles and depth of shower maximum (NandXmax) in extensive air showers of particle cascades was performed using AIRES code for SIBYLL hadronic model for different primary particles like electron, positron, gamma quanta and iron nuclei at the energy range 1014-1019eV. The comparison between the simulated longitudinal development ofNandXmaxusing SIBYLL hadronic model with two hadronic models (QGSJET99 ans SIBYLL16) has shown an opportunity for determination of cosmic ray cascade interactions in extensive air showers.

Arrival directions of extensive air showers of primary energy ~1017 eV

1968 ◽  
Vol 46 (10) ◽  
pp. S78-S80 ◽  
Author(s):  
P. R. Blake ◽  
J. D. Hollows ◽  
H. W. Hunter ◽  
R. J. O. Reid ◽  
R. M. Tennent ◽  
...  
Keyword(s):  
Primary Particle ◽  
Primary Energy ◽  
Air Showers ◽  
Time Intervals ◽  
Running Time ◽  
Upper Limits ◽  
Primary Particles ◽  
Stage 1 ◽  
Right Ascension ◽  
Arrival Directions

A detailed study of the arrival directions of primary particles of mean energy 2 × 1017 eV recorded by the Haverah Park Stage 1 (500-m) EAS array is reported. After rejecting time intervals randomly to equalize the sidereal running time of the array, upwards of 30 000 showers were available for analysis. In two energy intervals with mean energies about 1017 eV and 5 × 1017 eV significantly lower upper limits have been set on primary particle anistropy, and for all showers the amplitude of the first harmonic in right ascension is 0.6 ± 1.1% with a maximum at about 210°.An azimuthal asymmetry in detected showers (mainly arising from a 2° tilt of the array plane) limits the precision with which variations in declinations could be detected, and no analysis in galactic coordinates has been attempted. However, a plot in squares 10° RA by 10° declination reveals no deviations from isotropy within declination bands, and the overall distribution of intensity fluctuations is consistent with statistical expectation.Some general remarks are made on isotropy measurements.

scholarly journals Parameterization of Cherenkov Light Lateral Distribution Function as a Function of the Zenith Angle around the Knee Region

2016 ◽  
Vol 66 ◽  
pp. 71-78
Author(s):  
Marwah M. Abdulsttar ◽  
A.A. Al-Rubaiee ◽  
Abdul Halim K. Ali
Keyword(s):  
Distribution Function ◽  
Zenith Angle ◽  
Lateral Distribution ◽  
Extensive Air Showers ◽  
Cherenkov Light ◽  
Primary Proton ◽  
Air Showers ◽  
Knee Region ◽  
Lateral Distribution Function ◽  
Shower Core

Cherenkov light lateral distribution function (CLLDF) simulation was fullfiled using CORSIKA code for configurations of Tunka EAS array for different zenith angles. The parameterization of the CLLDF was carried out as a function of the destance from tehe shower core in extensive air showers (EAS) and zenith angle on the basis of the CORSIKA simulation for primary proton around the knee region with the energy 3.1015 eV at different zenith angles. The parametrized CLLDF is verified in comparison with the simulation that performed using CORSIKA code for two zenith angles.

Cosmic Ray Composition in the `Knee' Region Deduced from the Lateral Distribution of Cerenkov Light Emitted in Extensive Air Showers

1999 ◽  
Vol 16 (8) ◽  
pp. 622-624
Author(s):  
Min Zha ◽  
Tsang Chueng ◽  
Lin-kai Ding ◽  
Xiao-yu Gao ◽  
Qing-xi Geng ◽  
...  
Keyword(s):  
Cosmic Ray ◽  
Lateral Distribution ◽  
Extensive Air Showers ◽  
Air Showers ◽  
Knee Region ◽  
Cerenkov Light

scholarly journals PRIMARY ENERGY SPECTRUM AND MASS COMPOSITION DETERMINED WITH THE TUNKA EAS CHERENKOV ARRAY

2005 ◽  
Vol 20 (29) ◽  
pp. 6799-6801 ◽  
Author(s):  
D. V. CHERNOV ◽  
E. E. KOROSTELEVA ◽  
L. A. KUZMICHEV ◽  
V. V. PROSIN ◽  
I. V. YASHIN ◽  
...  
Keyword(s):  
Monte Carlo ◽  
Distribution Function ◽  
Energy Spectrum ◽  
Monte Carlo Simulations ◽  
Light Pulse ◽  
Primary Energy ◽  
Cherenkov Light ◽  
Mass Composition ◽  
Knee Region ◽  
The Mean

New results of 300 hours of operation of the TUNKA array are presented. An improved parametrization of the Cherenkov light lateral distribution function (LDF), based on CORSIKA Monte Carlo simulations and the experiment QUEST, has been used for the reconstruction of EAS parameters. The corrected energy spectrum in the knee region is obtained. The mean depth of the EAS maximum has been derived both from the analysis of LDF steepness and the FWHM of Cherenkov light pulse. The mean mass composition around the knee is estimated.

The energy spectra of atmospheric and neutrino-induced muons

1968 ◽  
Vol 46 (10) ◽  
pp. S352-S357
Author(s):  
R. Craig ◽  
J. L. Osborne ◽  
A. W. Wolfendale ◽  
E. C. M. Young
Keyword(s):  
Energy Spectrum ◽  
Cross Section ◽  
Ground Level ◽  
Primary Energy ◽  
Energy Spectra ◽  
Intensity Curve ◽  
Intermediate Boson ◽  
Neutrino Interactions ◽  
Primary Particles ◽  
Muons And Neutrinos

The interrelation of the primary energy spectrum and the energy spectra of muons and neutrinos is examined. The energy spectra of "atmospheric" muons at ground level and underground are calculated for various assumptions about the form of the depth–intensity curve at great depths and alternative assumptions as to the composition and energy spectrum of the primary particles. The implications are discussed. Calculations have also been made of the energy spectrum of neutrino-induced muons underground. It is shown how the spectrum is sensitive to the form of the cross section for inelastic neutrino interactions and to the mass of the (hypothetical) intermediate boson.

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