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 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˚.

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 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.

Computer simulations of cosmic-ray air showers II. Showers initiated by heavy primary particles

1974 ◽  
Vol 339 (1617) ◽  
pp. 157-170 ◽  
Keyword(s):  
Computer Simulations ◽  
Primary Particle ◽  
Cosmic Ray ◽  
High Energy ◽  
Air Showers ◽  
Heavy Particles ◽  
Longitudinal Development ◽  
Energy Interaction ◽  
Precise Knowledge ◽  
Primary Particles

Computer simulations have been made of large extensive air showers initiated by nuclei heavier than protons. The work forms part of a study of future experiments designed to identify the nature of the energetic primary particles. A model based upon data from nuclear emulsion experiments has been used to represent the break-up of the primary nuclei in collision with air nuclei. Differences in shower characteristics are predicted which are dependent upon the choice of model for the fragmentation of the primary nucleus and its energy. The major cause of fluctuations in the longitudinal development of showers produced by heavy particles is shown to be the pattern of the fragmentation of the incident nucleus. In the absence of a precise knowledge of the high-energy interaction, we have not identified any parameter in large showers which, if measurable and averaged over many showers, will reflect strongly the nature of the primary particle.

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.

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.

scholarly journals Radio interferometry applied to the observation of cosmic-ray induced extensive air showers

2021 ◽  
Vol 81 (12) ◽  
Author(s):  
Harm Schoorlemmer ◽  
Washington R. Carvalho
Keyword(s):  
Cosmic Ray ◽  
High Energy ◽  
High Accuracy ◽  
Extensive Air Showers ◽  
Ultra High Energy ◽  
Air Showers ◽  
Interferometric Technique ◽  
Radio Detection ◽  
Cosmic Particle ◽  
Shower Maximum

AbstractWe developed a radio interferometric technique for the observation of extensive air showers initiated by cosmic particles. In this proof-of-principle study we show that properties of extensive air showers can be derived with high accuracy in a straightforward manner. When time synchronisation below $$\sim $$ ∼ 1 ns between different receivers can be achieved, direction reconstruction resolution of $$< 0.2^\circ $$ < 0 . 2 ∘ and resolution on the depth of shower maximum of $$<10$$ < 10  g/cm$$^2$$ 2 are obtained over the full parameter range studied, with even higher accuracy for inclined incoming directions. In addition, by applying the developed method to dense arrays of radio antennas, the energy threshold for the radio detection of extensive air showers can be significantly lowered. The proposed method can be incorporated in operational and future cosmic particle observatories and with its high accuracy it has the potential to play a crucial role in unravelling the composition of the ultra-high-energy cosmic-particle flux.

scholarly journals The use of aerosol data in Auger Fluorescence Detector analysis

2019 ◽  
Vol 197 ◽  
pp. 01004
Author(s):  
Bruce R. Dawson
Keyword(s):  
Light Attenuation ◽  
Cosmic Ray ◽  
Primary Energy ◽  
Air Showers ◽  
Fluorescence Detector ◽  
Air Shower ◽  
Systematic Uncertainties ◽  
Surface Detector ◽  
Shower Maximum ◽  
Fluorescence Light

The Pierre Auger Observatory’s Fluorescence Detector (FD) consists of 27 telescopes arranged in four sites around the perimeter of the 3000 square kilometre Surface Detector (SD). Cosmic ray extensive air showers are viewed via the nitrogen fluorescence light they induce in the atmosphere. Careful treatment of light attenuation processes must be made, especially given that some showers are viewed at distances in excess of 30 km. Of particular importance is the attenuation due to scattering by aerosol particles, a challenging topic given that aerosol concentrations can vary on time-scales of hours. At the Auger Observatory, the vertical distribution of aerosols is measured hourly with a series of bi-static lidar systems (consisting of central laser facilities and each of the FD sites), and three times per night with a Raman lidar system. In this contribution we describe the use of aerosol profiles in the analysis of air shower data, in particular in the estimation of the cosmic ray primary energy, and the depth of shower maximum, Xmax. We also demonstrate how statistical and systematic uncertainties in the aerosol concentrations propagate through to a contribution to energy and Xmax uncertainties.

SIMULATIONS OF EXTENSIVE AIR SHOWERS TRIGGERED BY PROTON, IRON AND GAMMA PRIMARIES

2005 ◽  
Vol 20 (29) ◽  
pp. 6814-6816
Author(s):  
A. GERANIOS ◽  
E. FOKITIS ◽  
S. MALTEZOS ◽  
K. PATRINOS ◽  
A. DIMOPOULOS
Keyword(s):  
Energy Range ◽  
Cosmic Ray ◽  
High Energy ◽  
Extensive Air Showers ◽  
Ultra High Energy ◽  
Air Showers ◽  
Extensive Air Shower ◽  
Air Shower

Using the AIRES code, we have generated a large number of Extensive Air Showers corresponding to Ultra high energy cosmic ray gammas, protons and iron nuclei with energy range 1015 – 1022 eV. These simulations clearly show the different atmospheric depths of the Extensive Air Shower maxima in this energy range.

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