scholarly journals Reconstruction of Air-Shower Parameters through Lateral Distribution Function of Ultra-High Energy Particles

2021 ◽  
Vol 140 (4) ◽  
pp. 344-349
Author(s):  
KadhomF. Fadhel ◽  
A.A. Al-Rubaiee
Keyword(s):  
Distribution Function ◽  
High Energy ◽  
Lateral Distribution ◽  
Ultra High Energy ◽  
Lateral Distribution Function ◽  
Air Shower ◽  
High Energy Particles

scholarly journals Cygnus X-3 and Other Ultra-High-Energy γ-Ray Sources

1987 ◽  
Vol 125 ◽  
pp. 521-533
Author(s):  
John J. Barnard
Keyword(s):  
Theoretical Models ◽  
High Energy ◽  
Current Status ◽  
Ultra High Energy ◽  
X Ray ◽  
Air Shower ◽  
Γ Rays ◽  
Γ Ray ◽  
High Energy Particles

Recently, several binary X-ray sources have been found to be sources of ultra high energy γ-ray emission. Air shower observations indicate photon energies >∼ 1015 eV. We review the current status of observations from the source Cygnus X-3, and compare this data with that from the sources Hercules X-1, Vela X-1, and LMC X-4. Current theoretical models for the production of γ-rays and the acceleration of high energy particles are discussed and the consequences for the evolution of such systems are examined.

SPECTRUM OF COSMIC RAYS WITH ENERGY ABOVE 1017 EV

2005 ◽  
Vol 20 (29) ◽  
pp. 6878-6880 ◽  
Author(s):  
V. P. EGOROVA ◽  
A. V. GLUSHKOV ◽  
A. A. IVANOV ◽  
S. P. KNURENKO ◽  
V. A. KOLOSOV ◽  
...  
Keyword(s):  
Distribution Function ◽  
Energy Spectrum ◽  
Cosmic Rays ◽  
Time Distribution ◽  
Arrival Time ◽  
Lateral Distribution ◽  
Arrival Time Distribution ◽  
Array Data ◽  
Lateral Distribution Function ◽  
High Energies

The energy spectrum of primary cosmic rays with ultra-high energies based on the Yakutsk EAS Array data is presented. For the largest events values of S600 and axis coordinates have been obtained using revised lateral distribution function. The effect of the arrival time distribution at several axis distance on estimated density for Yakutsk and AGASA is considered.

scholarly journals Search for point sources of ultra-high-energy photons with the Telescope Array surface detector

2020 ◽  
Vol 492 (3) ◽  
pp. 3984-3993 ◽  
Author(s):  
R U Abbasi ◽  
M Abe ◽  
T Abu-Zayyad ◽  
M Allen ◽  
R Azuma ◽  
...  
Keyword(s):  
Point Source ◽  
Cosmic Ray ◽  
High Energy ◽  
Point Sources ◽  
Ultra High Energy ◽  
Telescope Array ◽  
Air Shower ◽  
Upper Limits ◽  
Surface Detector ◽  
Blind Search

ABSTRACT The surface detector (SD) of the Telescope Array (TA) experiment allows us to detect indirectly photons with energies of the order of 1018 eV and higher, and to separate photons from the cosmic ray background. In this paper, we present the results of a blind search for point sources of ultra-high-energy (UHE) photons in the Northern sky using the TA SD data. The photon-induced extensive air showers are separated from the hadron-induced extensive air shower background by means of a multivariate classifier based upon 16 parameters that characterize the air shower events. No significant evidence for the photon point sources is found. The upper limits are set on the flux of photons from each particular direction in the sky within the TA field of view, according to the experiment’s angular resolution for photons. The average 95 per cent confidence level upper-limits for the point-source flux of photons with energies greater than 1018, 1018.5, 1019, 1019.5 and 1020 eV are 0.094, 0.029, 0.010, 0.0073 and 0.0058 km−2yr−1, respectively. For energies higher than 1018.5 eV, the photon point-source limits are set for the first time. Numerical results for each given direction in each energy range are provided as a supplement to this paper.

Development of the Buckland Park Cosmic Ray Air Shower Array for Ultra High Energy Gamma Ray Astronomy

1986 ◽  
Vol 6 (3) ◽  
pp. 335-338 ◽  
Author(s):  
D. Ciampa ◽  
R. W. Clay ◽  
C. L. Corani ◽  
P. G. Edwards ◽  
J. R. Patterson
Keyword(s):  
Gamma Ray ◽  
Cosmic Ray ◽  
High Energy ◽  
Ultra High Energy ◽  
Gamma Ray Astronomy ◽  
Air Shower ◽  
High Energy Gamma ◽  
Energy Gamma ◽  
Shower Array ◽  
Air Shower Array

AbstractThe Buckland Park air shower array is being developed particularly for use as an ultra-high-energy gamma ray astronomy telescope. The properties of this instrument are described with an emphasis on improvements being made to its angular resolution. Some early data are presented to illustrate the way in which the data obtained will be used.

scholarly journals Prospects for detecting ultra-high-energy particles with FAST

2019 ◽  
Vol 19 (2) ◽  
pp. 019 ◽  
Author(s):  
Clancy W. James ◽  
Justin D. Bray ◽  
Ronald D. Ekers
Keyword(s):  
High Energy ◽  
Ultra High Energy ◽  
High Energy Particles

scholarly journals Direct measurement of the muonic content of extensive air showers between $$\mathbf { 2\times 10^{17}}$$ and $$\mathbf {2\times 10^{18}}~$$eV at the Pierre Auger Observatory

2020 ◽  
Vol 80 (8) ◽  
Author(s):  
A. Aab ◽  
◽  
P. Abreu ◽  
M. Aglietta ◽  
J. M. Albury ◽  
...  
Keyword(s):  
Direct Measurement ◽  
High Energy ◽  
Extensive Air Showers ◽  
Pierre Auger Observatory ◽  
Ultra High Energy ◽  
Air Showers ◽  
Fluorescence Detector ◽  
High Energy Cosmic Rays ◽  
Air Shower ◽  
Attenuation Corrected

Abstract The hybrid design of the Pierre Auger Observatory allows for the measurement of the properties of extensive air showers initiated by ultra-high energy cosmic rays with unprecedented precision. By using an array of prototype underground muon detectors, we have performed the first direct measurement, by the Auger Collaboration, of the muon content of air showers between $$2\times 10^{17}$$2×1017 and $$2\times 10^{18}$$2×1018 eV. We have studied the energy evolution of the attenuation-corrected muon density, and compared it to predictions from air shower simulations. The observed densities are found to be larger than those predicted by models. We quantify this discrepancy by combining the measurements from the muon detector with those from the Auger fluorescence detector at $$10^{{17.5}}\, {\mathrm{eV}} $$1017.5eV and $$10^{{18}}\, {\mathrm{eV}} $$1018eV. We find that, for the models to explain the data, an increase in the muon density of $$38\%$$38%$$\pm 4\% (12\%)$$±4%(12%)$$\pm {}^{21\%}_{18\%}$$±18%21% for EPOS-LHC, and of $$50\% (53\%)$$50%(53%)$$\pm 4\% (13\%)$$±4%(13%)$$\pm {}^{23\%}_{20\%}$$±20%23% for QGSJetII-04, is respectively needed.

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