Asymmetry of the angular distribution of Cherenkov photons of extensive air showers induced by the geomagnetic field

Homola, P.; Engel, R.; Wilczyński, H.

doi:10.1016/j.astropartphys.2014.05.008

Cited by 10 publications

(5 citation statements)

References 32 publications

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“…6. The azimuthal symmetry is indeed almost restored after the application of the described procedure (however, this may not be the case for low-energy (E <1 PeV) or highly inclined (θ >1 rad) showers, see [51]). A part of the spatial histogram that became empty due to the shrinkage of the LDF was filled by the minimal value inside the shrinked part of the histogram.…”

Section: Eas Cherenkov Light Signal At the Ground Levelmentioning

confidence: 97%

Spatial and temporal structure of EAS reflected Cherenkov light signal

Antonov

Bonvech

Чернов

et al. 2019

Astroparticle Physics

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A compact device lifted over the ground surface might be used to observe optical radiation of extensive air showers (EAS). Here we consider spatial and temporal characteristics of Vavilov-Cherenkov radiation ("Cherenkov light") reflected from the snow surface of Lake Baikal, as registered by the SPHERE-2 detector. We perform detailed full direct Monte Carlo simulations of EAS development and present a dedicated highly modular code intended for detector response simulations. Detector response properties are illustrated by example of several model EAS events. The instrumental acceptance of the SPHERE-2 detector was calculated for a range of observation conditions. We introduce the concept of "composite model quantities", calculated for detector responses averaged over photoelectron count fluctuations, but retaining EAS development fluctuations. The distortions of EAS Cherenkov light lateral distribution function (LDF) introduced by the SPHERE-2 telescope are understood by comparing composite model LDF with the corresponding function as would be recorded by an ideal detector situated at the ground surface. We show that the uncertainty of snow optical properties does not change our conclusions, and, moreover, that the expected performance of the SPHERE experiment in the task of cosmic ray mass composition study in the energy region ∼10 PeV is comparable with other contemporary experiments. Finally, we compare the reflected Cherenkov light method with other experimental techniques and briefly discuss its prospects. (T.A. Dzhatdoev) include CASA-BLANCA [16], BASJE [17], TACT [18] and the optical part of the Yakutsk array [19]. EAS fluorescent light was observed with HiRes [20] and the optical detectors of TA [21, 22] TALE [23] and PAO [15]. EAS radio emission is also studied in various experiments, such as LOPES [24], PAO [25], and LORA [26].The size of ground-based EAS detector arrays and their complexity is growing with time, and so does the difficulty of their deployment, calibration, and operation. Indeed, in order to work as an ensemble, the detectors must be distributed over a large area, sometimes hundreds [13] or thousands [15] square kilometers, and, moreover, they must be constantly power-supplied, be able to transfer information obtained with them, and kept fairly well timesynchronized.A long time ago it was pointed out that a compact device lifted over the snow-covered Earth surface is able to register reflected Cherenkov light [27]. This method is free from the above-mentioned difficulties of ground-based experiments. Moreover, a detector looking down at reflected Cherenkov light typically has a quasi-continious spatial sensitivity, i.e. it can observe light emitted from a substantial fraction of the snow-covered surface. This allows

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Section: Eas Cherenkov Light Signal At the Ground Levelmentioning

confidence: 97%

Spatial and temporal structure of EAS reflected Cherenkov light signal

Antonov

Bonvech

Чернов

et al. 2019

Astroparticle Physics

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“…To evaluate the angular resolution and effective area of HADAR in the 10 GeV to 100 TeV, we used the Cosmic Ray Simulations for Kascade (CORSIKA) program to generate a large number of extensive air shower samples, using the QGSJETII-04 and FLUKA models, respectively (Homola et al 2015), as shown in Figure 1.…”

Section: Experimental Sensitivitymentioning

confidence: 99%

Study of the Observation Sensitivity of Gamma-Ray Bursts for the HADAR Project

Zhang,

Chen,

Feng

et al. 2024

ApJ

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The High Altitude Detection of Astronomical Radiation (HADAR) is a novel wide-field Cherenkov Telescope. It is designed for gamma-ray astronomy in the energy range of 10 GeV to 100 TeV, with gamma-ray bursts (GRBs) being one of its primary research focuses. To assess its complementary capabilities, this study first presents the Crab sensitivity of HADAR. Then, to compare the sensitivity of GRBs, the observation time for all experiments is standardized to 100 s. To clearly demonstrate HADAR’s advantages, we estimate its observational results with a 221009A-like GRB. The study found that HADAR is capable of more comprehensively recording the bending and absorption of self-Compton radiation, which is expected to fill observational gaps in space- and ground-based experiments. We anticipate that this facility will ensure a large statistical GRB sample and advance our understanding of GRBs.

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“…The initiation of electromagnetic cascade showers was simulated using CORSIKA (Version 74100). The simulations considered primary incident γ-rays with different energies and at various zenith angles, traveling through an atmospheric medium at altitudes of 4300, 5300, and 6300 m. Specifically, high-and low-energy strong interaction models were established using QGSJETII-04 and FLUKA, respectively (Homola & Engel, 2015). To simulate Cherenkov radiation and the electromagnetic components in an EAS, an electromagnetic interaction model was established.…”

Section: Simulation Of Atmospheric Cherenkov Photonsmentioning

confidence: 99%

Lateral Density Distributions of Cherenkov Photons at Different Altitudes

Li,

Chen,

Feng

et al. 2023

Preprint

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Astrophysical very high energy (VHE) gamma-rays (with energies > 30 GeV) are believed to result almost exclusively from the interactions of populations of highly relativistic particles with ambient matter or photon ﬁelds. The study of these VHE photons therefore allows us to examine the processes of particle acceleration in the Universe, and the extreme environments in which they occur. Gamma-rays are also highly directional, making them useful for studying the origin, acceleration, propagation, and composition of cosmic rays. This study uses the Monte Carlo method to simulate the process of extensive air showers being initiated when primary incident γ-rays interact with the atmosphere. The ultimate goal is to investigate and analyze the properties and lateral density distributions of Cherenkov light at different altitudes. The simulation considers various energies and zenith angles. The results show that a hump in the lateral density distribution of Cherenkov light is a distinctive feature of a γ-initiated shower, with the hump becoming less prominent at higher energy levels and altitudes. These significant findings not only facilitate better fitting of experimental data obtained from actual extensive air showers but also assist with estimating readings from detectors, thus advancing our understanding of these processes.

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Asymmetry of the angular distribution of Cherenkov photons of extensive air showers induced by the geomagnetic field

Cited by 10 publications

References 32 publications

Spatial and temporal structure of EAS reflected Cherenkov light signal

Spatial and temporal structure of EAS reflected Cherenkov light signal

Study of the Observation Sensitivity of Gamma-Ray Bursts for the HADAR Project

Lateral Density Distributions of Cherenkov Photons at Different Altitudes

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