SIMULATION OF THE ATMOSPHERIC MUON FLUX WITH CORSIKA

2005 ◽  
Vol 20 (29) ◽  
pp. 6950-6952 ◽  
Author(s):  
T. DJEMIL ◽  
R. ATTALLAH ◽  
J. N. CAPDEVIELLE
Keyword(s):  
Lower Energy ◽  
High Energy ◽  
Primary Energy ◽  
Muon Flux ◽  
Hadronic Interaction ◽  
Extensive Air Shower ◽  
Air Shower ◽  
Atmospheric Muon ◽  
Simulation Package ◽  
Different Altitudes

We present in this paper the results of 3D-calculation of the atmospheric muon flux at different altitudes. We have used for this purpose the extensive air shower simulation package CORSIKA (v. 6.031) in combination with the hadronic interaction models VENUS (v. 4.12) at high energy (beyond 80 GeV) and GHEISHA (v. 2002) and UrQMD (v. 1.1) at lower energy. Our results are compared to data from different experiments (CAPRICE, BESS and HEAT). The correlation of the atmospheric muon flux to the primary zenith angle and primary energy is also investigated.

scholarly journals DETECTION OF A CHANGE OF SLOPE IN THE SPECTRUM OF HEAVY MASS COSMIC RAYS PRIMARIES BY THE KASCADE-GRANDE EXPERIMENT

2013 ◽  
Vol 53 (A) ◽  
pp. 728-731
Author(s):  
A. Chiavassa ◽  
W. D. Apel ◽  
J. C. Arteaga-Velázquez ◽  
K. Bekk ◽  
M. Bertaina ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Energy Range ◽  
Interaction Model ◽  
Primary Energy ◽  
Air Showers ◽  
Hadronic Interaction ◽  
Extensive Air Shower ◽  
Air Shower ◽  
Two Samples ◽  
Shower Size

KASCADE-Grande is an extensive air shower experiment devoted to the study of cosmic rays in the 1016 ÷ 1018 eV energy range. The array is composed by different detectors allowing independent measurements of the number of muons (Nμ) and charged particles (Nch) of extensive air showers (EAS). These two observables are then used to study the primary energy spectrum, separating the events in two samples, on the basis of the shower size ratio, corrected for attenuation in the atmosphere, lnNμ/ lnNch. The two samples represent the light and heavy mass groups of the primaries. In the studied energy range only the spectrum of heavy primaries shows a significant change of slope, the energy (estimated using the QGSJET II hadronic interaction model) of this feature is in agreeement with the expectations of a rigidity dependent knee feature.

scholarly journals Recent results from the LHCf and RHICf experiments

2019 ◽  
Vol 208 ◽  
pp. 05004
Author(s):  
Y. Itow ◽  
K. Masuda ◽  
H. Menjo ◽  
Y. Muraki ◽  
K. Ohashi ◽  
...  
Keyword(s):  
Hadron Collider ◽  
Cosmic Ray ◽  
Heavy Ion ◽  
High Energy ◽  
Relativistic Heavy Ion Collider ◽  
Hadronic Interaction ◽  
Extensive Air Shower ◽  
Neutral Particles ◽  
Air Shower ◽  
Energy Hadron

The Large Hadron Collider forward and the Relativistic Heavy Ion Collider forward experiments measured forward particles produced in high-energy hadron collisions at the LHC and RHIC. Using compact calorimeters neutral particles produced in pseudorapidities η >8.4 and η >6.0 are observed by the respective experiments. Because the collision energies ranging from 0.51 TeV to 13 TeV correspond to the cosmic-ray equivalent energies of 1014 to 1017 eV, the measurements are important to understand the hadronic interaction relevant to extensive air shower measurements. This paper reviews recent results of LHCf and initial performance of RHICf that took data in the 2017 RHIC operation.

scholarly journals An investigation of mass composition of ultra-high energy cosmic rays with energies above 1019 eV via the study of extensive air showers

2012 ◽  
pp. 87-92 ◽  
Author(s):  
S. Doostmohammadi ◽  
S.J. Fatemi
Keyword(s):  
Size Dependence ◽  
Galactic Plane ◽  
High Energy ◽  
Primary Energy ◽  
Mass Composition ◽  
Air Showers ◽  
Extensive Air Shower ◽  
High Energy Cosmic Rays ◽  
Air Shower ◽  
Shower Size

The electron and muon components of extensive air shower (EAS) with energies above 1019 eV are analyzed via various giant EAS arrays. A varying property of showers is observed for two energy ranges; higher and lower than (3 ? 4) x 1019 eV. The age parameter, zenith angle, shower size dependence on muon size and shower size dependence on primary energy show an increment of mass composition (MC) above (3?4)x 1019eV. Comparison of the observed EAS results with the simulations of Capdevielle et al. (2000) and Shinozaki et al. (2005) gives at most 20% photon fraction for primary energies above 1019 eV. The arrival directions of showers above 4x1019 eV indicate an increasing concentration towards the super galactic plane.

scholarly journals Improving the prediction of the Atmospheric neutrino flux using the atmospheric muon flux

2019 ◽  
Vol 208 ◽  
pp. 07001
Author(s):  
Morihiro Honda
Keyword(s):  
Energy Range ◽  
Energy Region ◽  
Test Bench ◽  
Atmospheric Neutrino ◽  
Neutrino Flux ◽  
Interaction Model ◽  
Muon Flux ◽  
Atmospheric Neutrinos ◽  
Hadronic Interaction ◽  
Atmospheric Muon

It is well known that the correlation of atmospheric neutrinos and muons are simply correlated in the energy region of 1–10 GeV, and used for the test bench of the hadronic interaction model used for the calculation of the atmospheric neutrino flux. However, the correlation becomes unclear for neutrinos in the energy range below 1 GeV, which is important for the study of mass ordering of neutrino and CP phase of the neutrino mass. We extend the study of the correlation to the lower neutrino energies and find that the atmospheric muon flux observed at high altitude shows a good correlation to the atmospheric neutrino flux, and could be used to calibrate the hadronic interaction model.

scholarly journals High Energy γ-Rays from the Direction of the Crab Pulsar

1981 ◽  
Vol 94 ◽  
pp. 327-328
Author(s):  
T. Dzikowski ◽  
B. Grochalska ◽  
J. Gawin ◽  
J. Wdowczyk
Keyword(s):  
High Energy ◽  
Crab Pulsar ◽  
Muon Detector ◽  
Extensive Air Shower ◽  
Air Shower ◽  
Very High Energy ◽  
Γ Rays ◽  
Shower Array ◽  
Very High ◽  
Air Shower Array

A search has been made for very high energy photons from the direction of the Crab Pulsar using the Lodz extensive air shower array. This device is particularly suitable for such a study because it consists of a large muon detector which can be used to search for the characteristic muon poor showers.

scholarly journals Test of the hadronic interaction models SIBYLL2.3, EPOS-LHC and QGSJETII- 04 with Tibet EAS core data

2019 ◽  
Vol 208 ◽  
pp. 08013
Author(s):  
M. Amenomori ◽  
X. J. Bi ◽  
D. Chen ◽  
T. L. Chen ◽  
W. Y. Chen ◽  
...  
Keyword(s):  
Experimental Data ◽  
Energy Region ◽  
Interaction Model ◽  
Systematic Errors ◽  
High Energy ◽  
Forward Region ◽  
Hadronic Interaction ◽  
Interaction Models ◽  
Air Shower ◽  
Shower Array

A hybrid experiment has been started by the ASγ experiment at Yangbajing (4300m a.s.l.) in Tibet since May 2009, that consists of a high-energy air-shower-core array (YAC-I) and a high-density air-shower array (Tibet-III). In this paper, we report our results to check the hadronic interaction models SIBYLL2.3, SIBYLL2.1, EPOS-LHC and QGSJETII-04 in the multi-tens TeV energy region using YAC-I+Tibet-III experimental data from May 2009 through January 2010. The effective live time is calculated as 106.05 days. The results show that the description of transverse momentum, inelastic cross-section and inelasticity for the 4 hadronic interaction models is consistent with YAC-I experimental data within 15% systematic errors range in the forward region below 100 TeV. Among them, the EPOS-LHC model is the best hadronic interaction model. Furthermore, we find that the H4a composition model is the best one below the 100 TeV energy region.

Detection of high energy showers by the Astroneu extensive air shower array

New Astronomy ◽  
2021 ◽  
Vol 82 ◽  
pp. 101448 ◽  
Author(s):  
A. Leisos ◽  
T. Avgitas ◽  
G. Bourlis ◽  
G.K. Fanourakis ◽  
I. Gkialas ◽  
...  
Keyword(s):  
High Energy ◽  
Extensive Air Shower ◽  
Air Shower ◽  
Shower Array ◽  
Air Shower Array

scholarly journals High-energy atmospheric muon flux calculations in comparison with recent measurements

2019 ◽  
Vol 1181 ◽  
pp. 012054 ◽  
Author(s):  
A A Kochanov ◽  
A D Morozova ◽  
T S Sinegovskaya ◽  
S I Sinegovsky
Keyword(s):  
High Energy ◽  
Muon Flux ◽  
Atmospheric Muon

Hisparc cosmic ray detector’s response to heavy rain

2020 ◽  
Author(s):  
Alexander P. J. van Deursen ◽  
David Fokkema ◽  
Kasper van Dam ◽  
Bob van Eijk
Keyword(s):  
Cosmic Ray ◽  
Heavy Rain ◽  
High Energy ◽  
Process Time ◽  
Extensive Air Shower ◽  
Air Shower ◽  
Washing Process ◽  
Energy Gamma ◽  
Gas Molecules ◽  
Summer Storm

<p>Cosmic ray particles have extreme energies, 10<sup>16</sup> eV/nucleon and up. Upon arrival at the higher atmosphere and collisions with the gas molecules there, the cosmic ray particles convert into an cascade of different secondary particles that finally arrive at soil level in the form of an extensive air shower (EAS): high-energy gamma’s, electrons and muons. In the HIgh School Project on Astrophysics Research with Cosmics (Hisparc, www.hisparc.nl) about 100 EAS detector stations are distributed over the Netherlands and several neighboring countries. These stations are mostly placed on the roof of secondary schools, where they have been built by pupils to attract them towards STEM studies.</p><p>Each station consists of two or four detectors with 0.5 m<sup>2</sup> plastic scintillator plates to record the passage of the EAS. At coincidence, the scintillator signals are individually recorded, accurately timed with GPS. All data are sent to and collected at the NIKHEF institute (www.nikhef.nl) and made available (open-access) for further analysis by pupils and scientists.</p><p>The sensitivity of the detectors is commonly adjusted such that each detector records a few hundred hits per second. The number of coincidences within 1.5 μs is then about 1 in 3 seconds, in part due to an actual EAS, in part due to random local radioactive processes.</p><p>During intense rainfall of a particular summer storm several two-detector systems recorded an increase in the coincidence frequency of up to a factor of 7. When comparing different stations we could follow the associated storm front moving northwards over NL. Within the coincidence interval of 1.5 μs the increased individual signals of both detectors were evenly distributed. Actual EAS signals tend to be synchronous to within 100 ns. We therefor attribute the increase to random signals. As possible source we suggest gamma radiation due to radon daughters in the atmosphere that are washed out by the rain and accumulate on the roof close to the detectors. The delay between rain and signal increase is noted and in accordance with the washing process time.</p>

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