Discrimination of Muons for Mass Composition Studies of Inclined Air Showers Detected with IceTop

In order to get the primary energy of cosmic rays from their extensive air showers using the fluorescence detection technique, the invisible energy should be added to the measured calorimetric energy. The invisible energy is the energy carried away by particles that do not deposit all their energy in the atmosphere. It has traditionally been calculated using Monte Carlo simulations that are dependent on the assumed primary particle mass and on model predictions for neutrino and muon production. In this work the invisible energy is obtained directly from events detected by the Pierre Auger Observatory. The method applied is based on the correlation of the measurements of the muon number at the ground with the invisible energy of the showers. By using it, the systematic uncertainties related to the unknown mass composition and to the high energy hadronic interaction models are significantly reduced, improving in this way the estimation of the energy scale of the Observatory.

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Study of muons from ultrahigh energy cosmic ray air showers measured with the Telescope Array experiment

EPJ Web of Conferences ◽

10.1051/epjconf/201921002012 ◽

2019 ◽

Vol 210 ◽

pp. 02012

Author(s):

R. Takeishi

Keyword(s):

Interaction Model ◽

Cosmic Ray ◽

Mass Composition ◽

Ultrahigh Energy ◽

Air Showers ◽

Hadronic Interaction ◽

Telescope Array ◽

Interaction Models ◽

Air Shower ◽

Number Of Particles

One of the uncertainties in ultrahigh energy cosmic ray (UHECR) observation derives from the hadronic interaction model used for air shower Monte-Carlo (MC) simulations. One may test the hadronic interaction models by comparing the measured number of muons observed at the ground from UHECR induced air showers with the MC prediction. The Telescope Array (TA) is the largest experiment in the northern hemisphere observing UHECR in Utah, USA. It aims to reveal the origin of UHECRs by studying the energy spectrum, mass composition and anisotropy of cosmic rays by utilizing an array of surface detectors (SDs) and fluorescence detectors. We studied muon densities in the UHE extensive air showers by analyzing the signal of TA SD stations for highly inclined showers. On condition that the muons contribute about 65% of the total signal, the number of particles from air showers is typically 1.88 ± 0.08 (stat.) ± 0.42 (syst.) times larger than the MC prediction with the QGSJET II-03 model for proton-induced showers. The same feature was also obtained for other hadronic interaction models, such as QGSJET II-04.

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

EPJ Web of Conferences ◽

10.1051/epjconf/201921602004 ◽

2019 ◽

Vol 216 ◽

pp. 02004 ◽

Cited By ~ 1

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.

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RECONSTRUCTION OF TOTAL MUON NUMBER IN KASCADE-GRANDE

International Journal of Modern Physics A ◽

10.1142/s0217751x05030302 ◽

2005 ◽

Vol 20 (29) ◽

pp. 6855-6857

Author(s):

◽

J. VAN BUREN ◽

T. ANTONI ◽

W. D. APEL ◽

F. BADEA ◽

...

Keyword(s):

Simulated Data ◽

Mass Composition ◽

Size Spectrum ◽

Air Showers ◽

Muon Component ◽

Extensive Air Shower ◽

Additional Information ◽

Air Shower ◽

First Results ◽

Charged Component

The KASCADE-Grande experiment extends the existing extensive air shower experiment KASCADE by an array of 37 detector stations spread over an area of 0.5 km2. The new Grande array measures the charged component of the showers. To reconstruct the mass composition of the cosmic rays, additional information from the muon component of air showers is required. Using observables from the new Grande array together with the muon detectors of the original KASCADE array provides a possibility to reconstruct also the total muon number of each air shower. The quality of reconstruction based on comparison with simulated data, as well as first results of a reconstructed muon size spectrum are presented.

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Estimating of Cherenkov Radiation in Extensive Air Showers Using CORSIKA Code for Tunka133 EAS Cherenkov Array

Applied Mechanics and Materials ◽

10.4028/www.scientific.net/amm.754-755.807 ◽

2015 ◽

Vol 754-755 ◽

pp. 807-811

Author(s):

A.A. Al-Rubaiee ◽

Uda Hashim ◽

Mohd Khairuddin Md Arshad ◽

A. Rahim Ruslinda ◽

R.M. Ayub ◽

...

Keyword(s):

Energy Spectrum ◽

Energy Range ◽

Cosmic Ray ◽

High Energy ◽

Extensive Air Showers ◽

Cherenkov Light ◽

Mass Composition ◽

Air Showers ◽

Good Ability ◽

The Given

The simulation of Cherenkov light Lateral distribution function (LDF) in Extensive Air Showers (EAS) initiated primary particles such as primary calcium, argon, proton iron nuclei, neutron and nitrogen have been performed using CORSIKA program for conditions and configurations of Tunka133 EAS Cherenkov array. The simulation was fulfilled at the high energy range 1014-1016eV for four different zenith angles 0o, 10o, 15oand 30o. The results of the simulated Cherenkov light LDF are compared with the measurements of Tunka133 EAS array for the same particles and energy range mentioned above. This comparison may give the good ability to reconstruct the energy spectrum and mass composition of the primary cosmic ray particles in EAS. The main feature of the given approach consists of the possibility to make a library of Cherenkov light LDF samples which could be utilized for analysis of real events which can be detected with different EAS arrays and reconstruction of the primary cosmic rays energy spectrum and mass composition of EAS particles.

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