arXiv subjects

A. A. Al-Rubaiee

Publications and source records attributed to A. A. Al-Rubaiee.

15 recordsLinked to original sources

arXiv2026

Longitudinal Development Analysis of Extensive Air Showers Using CORSIKA Simulations

We present a comprehensive analysis of the longitudinal development of Extensive Air Showers (EAS) simulated with CORSIKA version 7.7500 for proton, helium, and iron primaries at energies of 10^15, 10^16, and 10^17 eV across zenith angles of 0, 30, and 45 degrees. For each combination of primary type, energy, and zenith angle, 50 independent showers were simulated, resulting in a total of 450 simulated showers. The Gaisser - Hillas function was fitted to extract the depth of shower maximum (Xmax) and the number of particles at maximum (Nmax). Our results confirm the expected logarithmic increase of Xmax with energy (about 10 g/cm^2 per decade), as well as systematically shallower Xmax for heavier primaries (iron vs. proton: Delta (Xmax) equal to about 160 g/cm^2 at 10^17 eV).The simulations also reproduce the expected sec (theta) scaling behavior. Multi-component analysis reveals distinct evolutionary patterns for electromagnetic, muonic, and hadronic components. These findings provide benchmark-level simulations for cosmic-ray composition studies and validate the CORSIKA framework for multi-parameter analyses of air-shower development.

astro-ph.HE↗

arXiv2025

Investigating the ground energy distribution of particles produced in extensive air showers

The energy spectra of particles arriving at the ground is a significant observable in the analysis of extensive air showers (EAS). Energy distributions at ground were studied for primary particles (12C,56Fe, p, and 28Si) with high primary energies (10^17, 10^18, 10^19, and 10^20 eV) from two zenith angles (0 and 30 Deg.). 960 EAS were simulated using the Monte-Carlo program Aires (version 19.04.00) with three models of hadronic interaction (EPOS-LHC, QGSJET-II-04, and Sibyll2.3c). Good agreement was obtained by comparing the present results with results simulated using CORSIKA for primary iron at an energy of 10^20 eV. In this study we investigated various secondary particles that arrive at the ground and deposit a portion of their energy on ground detectors. These results show that the distinction in energy distribution at ground is greater for primary protons than carbon, iron, or silicon nuclei at higher energies and steeper zenith angles.

astro-ph.HE↗

arXiv2022

Simulation and Parameterization of Longitudinal Development in Extensive Air Showers for Different Hadronic Interaction Models

The simulation analysis of the Extensive Air Showers (EAS) was executed by exploring the longitudinal development employing the AIRES system (version 19.04.00) for several hadronic interaction models (SIBYLL, QGSJET, and EPOS) for high energies. The simulation was performed for different high energies (10^17, 10^18, and 10^19) eV and two dissimilar primary particles, proton as well iron nuclei, with several zenith angles values (0^o, 10^o, and 30^o). The shower size of longitudinal development was parameterized using the sigmoidal function (Boltzmann model) and gave a new four parameters as functions of the primary energy between the energy extent (10^17-10^19) eV. The comparison among the acquired results data (the parameterized number of shower particles) along with the experimental results (Pierre Auger experiment) had offered a fascinating matching for the primary proton at the fixed primary energy 10^19 eV for vertical EAS showers.

hep-ex↗

arXiv2022

Reconstruction of Air-Shower Parameters Through the Lateral Distribution Function of Ultra-High Energy Particles

In this study, the necessity of the simulation study for exploring the interactions of ultra-high energy particles cosmic rays was examined. Different hadronic interaction models such as (SIBYLL, QGSJET, and EPOS) were simulated by using air showers simulation AIRES system (version 19.04.00). Also, the charged particle density of Extensive Air Showers (EAS) was calculated by estimating the lateral distribution function (LDF). Moreover, the LDF simulation of the two primary particles (proton and iron nuclei) was performed, taking into account their primary energies effect and the zenith angle of charged particles that produced in the EAS, within the energy range (10^17-10^19) eV. At extremely high energies (10^17, 10^18, and 10^19) eV, new parameters as a function of the primary energy were obtained by fitting the lateral distribution curves of EAS using Sigmoidal function (Logistic model). Comparison of the results showed a good agreement between the values obtained from the parameterized LDF using Sigmoidal function with experimental results by AGASA EAS observatory for the primaries proton as well iron nuclei, with the production of (electron positron) pair and the charged muons secondary particles at high energy about 10^19 eV and (theta = 0 degree).

hep-ph↗

arXiv2021

Parametric analysis of the Lateral Distribution Function of Cherenkov light for Yakutsk EAS Array in the Energy Range 1-20 PeV

In this research, the simulation of lateral distribution function (LDF) of Cherenkov radiation was performed using CORSIKA software for two hadronic models QGSJET and GHEISHA. This simulation was performed for several elementary particles such as protons, iron nuclei, electrons and gamma quanta, in the range of energies 1-20 PeV for three zenith angles 0, 20 and 30 degrees. A parameterization of Cherenkov light LDF was performed for that simulated curves using Lorentzian function. The comparison between the obtained results for LDF of Cherenkov light with that measured with Yakutsk EAS array gave a good agreement within the distances of 100-1000 m from the shower axis.

astro-ph.HE↗

arXiv2021

Investigating the Longitudinal Development of EAS with Ultra High Energies

The simulation of the extensive air showers was performed by investigating the longitudinal development parameters (N and Xmax) by using AIRES system version 19.04.0. The simulation was performed at the energy range (10^18-10^20 eV) for different primary particles (such as primary proton and iron nuclei) and different zenith angles. The longitudinal development curves of EAS are fitted using Gaussian function that gave a new parameters for different primary particles and different zenith angles at the energy range (10^18-10^20 eV).

astro-ph.HE↗

arXiv2020

Theoretical Study of Extensive Air Shower Effects in Atmosphere by Simulating the Lateral structure of Several Cosmic Radiations

Extensive air showers (EAS) are a cascade of electromagnetic radiation and ionized particles that produced in the atmosphere through the interaction of a primary cosmic ray with the atom of nucleus in the air producing a huge amount of secondary particles such as X-ray, electrons, neutrons, muons, alpha particles, etc. In this work, EAS effects were demonstrated by estimating the lateral distribution function (LDF) at ultrahigh energies of the various cosmic ray particles. The LDF of charged particles such as electron and positron pair production, gamma and muons particles was simulated at ultrahigh energies 10^16, 10^18 and 10^19 eV. The simulation was carried out using an air shower simulator called AIRES system version 2.6.0. The effect of the primary particles, energies and zenith angle on the LDF of charged particles produced in the EAS was taken into account. Comparison of LDF for charged particles and experimental results gave good agreement for electron and positron pair production and muons particles at 10^19 eV for 0 and 10 zenith angles

astro-ph.HE↗

arXiv2020

Thinning Energy Effect on the Fluctuations of Charged Particles Lateral Distribution Produced in Extensive Air Showers

In this work, the effects of the extensive air showers (EAS) were described by estimating the lateral distribution function (LDF) at very high energies of various cosmic ray particles. LDF was simulated for charged particles such as the electron and positron pair production, gamma, muons and all charged particles at very high energies 10^16, 10^18 and 10^19 eV. The simulation was performed using air shower simulator system (AIRES) version 2.6.0. The effect of primary particles, energies, thinning energy and zenith angle on the charged LDF particles produced in the EAS was taken into account. The comparison of the estimated LDF of charged particles such as the electron and positron pair production and muons with the simulated results by Sciutto and experimental results by Yakutsk EAS observatory gives a good acceptance at the energy 10^19 eV for 0 and 10 zenith angles.

astro-ph.HE↗

arXiv2018

Approximating the Lateral Distribution Function of Cherenkov Radiation as a Function of the Particle Type for Tunka-133 Array

The main interest of the present work is in analyzing the lateral distribution function (LDF) of Cherenkov radiation from particles that produced in Extensive Air Showers (EAS). The simulation of Cherenkov radiation LDF is fulfilled by utilizing the CORSIKA program at 1 PeV of the primary energy around the knee region for many primaries for vertical showers for Tunka-133 array conditions. Depending on the numerical simulation results of Cherenkov light LDF, sets of parameterized polynomial functions are resetted for several particles as a function of primary particle type. The comparison between the approximated LDF of Cherenkov radiation with the LDF which has been simulated using CORSIKA program for Tunka-133 array is verified for several primary particles for vertical EAS cascade.

astro-ph.HE↗

arXiv2017

Cherenkov Light Lateral Distribution Function Estimation as a Function of Zenith Angle

The simulation of Cherenkov light lateral distribution function (CLLDF) in Extensive Air Showers (EAS) was performed by using the Monte Carlo CORSIKA code for configurations of Tunka-133 EAS Cherenkov array. This simulation was carried out for different primary particles (e+, e-, p, O, Ar and Fe) around the knee region with the energy 3.10^15 eV at different zenith angles. By depending on the Breit-Wigner function a parameterization of CLLDF was reconstructed on the basis of this simulation as a function of the zenith angle. The parameterized CLLDF was verified for four fixed zenith angles in comparison with the simulation that performed using CORSIKA code for each primary particle.

astro-ph.IM↗

arXiv2016

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

Cherenkov light lateral distribution function (CLLDF) simulation was fulfilled using CORSIKA code for configurations of Tunka EAS array of different zenith angles. The parameterization of the CLLDF was carried out as a function of the distance from the shower core in extensive air showers (EAS) and zenith angle on the basis of the CORSIKA simulation of primary proton around the knee region with the energy 3.10^15 eV at different zenith angles. The parameterized CLLDF is verified in comparison with the simulation that performed using CORSIKA code for two zenith angles.

astro-ph.IM↗

arXiv2016

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

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 parameterized CLLDF with that simulated with Yakutsk EAS array is verified. The parameterized CLLDF also is compared with that measured on the Yakutsk EAS array.

astro-ph.HE↗

arXiv2015

Study of Cherenkov Light Lateral Distribution Function around the Knee Region in Extensive Air Showers

The Cherenkov light lateral distribution function (LDF) was simulated with the CORSIKA code, in the energy range (10^13-10^16) eV. This simulation was performed for conditions and configurations of the Tunka EAS Cherenkov array for 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 which measured with Tunka Cherenkov array experiment. Comparison of the calculated LDF of Cherenkov radiation with that measured at the Tunka EAS array shows the ability for identifying of the primary particle that initiated the EAS cascades determining of its primary energy around the knee region of the cosmic ray spectrum.

physics.gen-ph↗

arXiv2011

Parametrization for Cherenkov light lateral distribution function in Extensive Air Showers

The simulation of the Cherenkov light lateral distribution function (LDF) in Extensive Air Showers (EAS) was perfomed with the CORSIKA code in the energy range 10^13-10^16 eV for configuration of the Tunka-25 EAS array. On the basis of this simulation we obtained sets of approximating functions for primary protons, iron nuclei and gamma-quanta for zenith angles Theta<=20. The comparison of the calculated Cherenkov light LDF with that measured with the Tunka-25 array has shown an opportunity of primary particle identification and definition of its energy around the "knee".

physics.gen-ph↗

arXiv2011

Cherenkov light Extrapolation at Ultra High Energy Cosmic Rays in Extensive Air Showers

The Simulation of Cherenkov light lateral distribution function (LDF) from particles of Extensive Air Showers (EAS) with ultra high energy cosmic rays (E>=10^16 eV) was simulated for primary protons by the computer code CORSIKA. The parameterization, that constructed on the basis of this simulation have allowed us to reconstruct the events, that is, to reconstruct the type and energy of the particle that generated EAS from signal amplitudes of Cherenkov light registered with the Tunka-25 facility. The extrapolation of the Cherenkov light LDF approximation at the energy range (10^16-2.10^18 eV) was taken into account.

physics.gen-ph↗