Approximation of the lateral distribution function of the Cherenkov light from extensive air showers in the primary energy region 1-100 PeV.

Latypova, Vasilisa; Azra, Clemence; Bonvech, E. A.; Чернов, Д. В.; Галкин, В. И.; Ivanov, V.; Подгрудков, Д.; Роганова, Т. М.

doi:10.22323/1.423.0069

Cited by 2 publications

(1 citation statement)

References 14 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…While these charged CRs propagate, they deflect in the stochastic galactic magnetic field. Due to this deflection, it is not possible to directly trace the celestial bodies from which they originate based on their direction (Latypova & Azra, 2023). CRs interact with an interstellar medium in the source region and during their propagation to produce neutral γ-rays, and the origins of CRs can be traced by directly observing the γ-rays.…”

Section: Introductionmentioning

confidence: 99%

Lateral Density Distributions of Cherenkov Photons at Different Altitudes

Li,

Chen,

Feng

et al. 2023

Preprint

View full text Add to dashboard Cite

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.

show abstract

Section: Introductionmentioning

confidence: 99%