scholarly journals Studying the thinning Effect of Longitudinal development in Extensive Air Showers for Primary Proton and Iron Nuclei at Ultra-High Energies

2020 ◽  
Vol 31 (3) ◽  
pp. 114
Author(s):  
Abbas R. Raham ◽  
Ahmed A. Al-Rubaiee ◽  
Majida H. Al-Kubaisy ◽  
Suror N. Esmaeel
Keyword(s):  
Charged Particles ◽  
Cosmic Ray ◽  
Primary Energy ◽  
Extensive Air Showers ◽  
Primary Proton ◽  
Air Showers ◽  
Longitudinal Development ◽  
High Energies ◽  
Charged Pions ◽  
Very High

In the present work, extensive air showers (EAS) effects are described by estimating the longitudinal development model of EAS at very high energies of various cosmic ray particles. The longitudinal development was simulated for charged particles such as gamma, charged pions and charged muons at very high energies 1017, 1018 and 1019eV. The simulation was performed using an air shower simulator system (AIRES) version 19.04.0. The effect of primary particles, energies, thinning energy and zenith angle (θ) on the number of charged particles (longitudinal development) produced in the EAS was taken into account. The rapprochement of the estimated longitudinal development of the charged particles such as the charged muons and charged pions with the experimental measurements (AUGER experiment) that gave a good agreement for primary proton at the fixed primary energy 1019eV for θ =0˚.

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.

scholarly journals Extension of Cherenkov Light LDF Approximation for Yakutsk EAS Array

2014 ◽  
Vol 2014 ◽  
pp. 1-6 ◽  
Author(s):  
A. A. Al-Rubaiee ◽  
Y. Al-Douri ◽  
U. Hashim
Keyword(s):  
Distribution Function ◽  
Cosmic Ray ◽  
High Energy ◽  
Primary Energy ◽  
Cherenkov Light ◽  
Primary Proton ◽  
Air Showers ◽  
High Energies ◽  
Primary Particles

The simulation of the Cherenkov light lateral distribution function (LDF) in extensive air showers (EAS) was performed using CORSIKA code for configuration of Yakutsk EAS array at high energy range for different primary particles (p, Fe, and O2) and different zenith angles. Depending on Breit-Wigner function a parameterization of Cherenkov light LDF was reconstructed on the basis of this simulation as a function of primary energy. A comparison of the calculated Cherenkov light LDF with that measured on the Yakutsk EAS array gives the possibility of identification of the particle initiating the shower and determination of its energy in the knee region of the cosmic ray spectrum. The extrapolation of approximated Cherenkov light LDF for high energies was obtained for primary proton and iron nuclei.

scholarly journals Longitudinal profiles of Extensive Air Showers with inclusion of charm and bottom particles

2019 ◽  
Vol 34 (12) ◽  
pp. 1950069
Author(s):  
M. A. Müller ◽  
V. P. Gonçalves
Keyword(s):  
Large Fraction ◽  
Cosmic Ray ◽  
Primary Energy ◽  
Considerable Change ◽  
Extensive Air Showers ◽  
Longitudinal Profile ◽  
Air Showers ◽  
Energy Deposit ◽  
Production Models ◽  
Longitudinal Profiles

Charm and bottom particles are rare in Extensive Air Showers, but their effects can be radical on the EASs development. If such particles show up with a large fraction of primary energy, they can reach large atmospheric depths, depositing energy in deeper layers of the atmosphere. That will cause changes at the EAS observables ([Formula: see text], RMS and [Formula: see text]), besides a considerable change in the shape of longitudinal profile energy deposit in the atmosphere. We are using for this work a modified code of an EAS simulator, CORSIKA, with production of charm and bottom particles at the first interaction of the primary cosmic ray. We will show in this paper some results to different [Formula: see text] values and different production models.

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.

Search for tachyons preceding cosmic ray extensive air showers of energy

1977 ◽  
Vol 55 (14) ◽  
pp. 1280-1288 ◽  
Author(s):  
Gary R. Smith ◽  
S. Standil
Keyword(s):  
Cosmic Ray ◽  
Time Spectrum ◽  
Primary Energy ◽  
Convincing Evidence ◽  
Extensive Air Showers ◽  
Air Showers ◽  
Air Shower ◽  
Particle Arrival ◽  
Energy Formula ◽  
Shower Array

A search for tachyons preceding extensive air showers has been conducted using an air shower array operated in conjunction with a large aperture, five element cosmic ray telescope. More than 200 000 air showers of primary energy [Formula: see text] were observed over a period of 223 days and a 290 μs period before each of these showers was scanned for a related particle signal from the telescope. In this way a particle arrival time spectrum containing 1519 tachyon candidates was observed. No convincing evidence was found for any subgroup of these events that might be attributable to tachyons.

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