Ultra-High Energy Cosmic Ray Study Results by Radio Emission Technique at Yakutsk Array

2019 ◽  
Vol 82 (6) ◽  
pp. 795-799
Author(s):  
I. S. Petrov ◽  
S. P. Knurenko ◽  
Z. E. Petrov
Keyword(s):  
Radio Emission ◽  
Cosmic Ray ◽  
High Energy ◽  
Ultra High Energy ◽  
Yakutsk Array ◽  
Study Results

scholarly journals First analysis of inclined air showers detected by Tunka-Rex

2019 ◽  
Vol 216 ◽  
pp. 02012
Author(s):  
T. Marshalkina ◽  
P.A. Bezyazeekov ◽  
N.M. Budnev ◽  
D. Chernykh ◽  
O. Fedorov ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Radio Emission ◽  
Zenith Angle ◽  
Cosmic Ray ◽  
High Energy ◽  
Ultra High Energy ◽  
Air Showers ◽  
Standard Analysis ◽  
Air Shower ◽  
The Magnetic Field

The Tunka Radio Extension (Tunka-Rex) is a digital antenna array for the detection of radio emission from cosmic-ray air showers in the frequency band of 30 to 80 MHz and for primary energies above 100 PeV. The standard analysis of Tunka-Rex includes events with zenith angle of up to 50?. This cut is determined by the efficiency of the external trigger. However, due to the air-shower footprint increasing with zenith angle and due to the more efficient generation of radio emission (the magnetic field in the Tunka valley is almost vertical), there are a number of ultra-high-energy inclined events detected by Tunka-Rex. In this work we present a first analysis of a subset of inclined events detected by Tunka-Rex. We estimate the energies of the selected events and test the efficiency of Tunka-Rex antennas for detection of inclined air showers.

scholarly journals High energy cosmic ray interactions and UHECR composition problem

2019 ◽  
Vol 210 ◽  
pp. 02001
Author(s):  
Sergey Ostapchenko
Keyword(s):  
Experimental Data ◽  
Monte Carlo ◽  
Cosmic Rays ◽  
Cosmic Ray ◽  
High Energy ◽  
Ultra High Energy ◽  
Hadronic Interactions ◽  
High Energy Cosmic Rays ◽  
Cosmic Ray Interactions ◽  
Composition Problem

The differences between contemporary Monte Carlo generators of high energy hadronic interactions are discussed and their impact on the interpretation of experimental data on ultra-high energy cosmic rays (UHECRs) is studied. Key directions for further model improvements are outlined. The prospect for a coherent interpretation of the data in terms of the UHECR composition is investigated.

AN EMPIRICAL MODEL OF PRODUCTION AND ATTENUATION OF FLUORESCENCE LIGHT IN ATMOSPHERE FOR SATELLITE-BASED ULTRA HIGH ENERGY COSMIC RAY EXPERIMENTS

2011 ◽  
Vol 20 (03) ◽  
pp. 299-317
Author(s):  
E. STRAZZERI ◽  
O. CATALANO ◽  
B. SBARUFATTI
Keyword(s):  
Stratospheric Ozone ◽  
Cosmic Ray ◽  
High Energy ◽  
Fluorescence Yield ◽  
Ultra High Energy ◽  
Atmospheric Conditions ◽  
Atmospheric Transmission ◽  
Emission Point ◽  
Geographical Variations ◽  
Fluorescence Light

In the context of detection of Ultra High Energy Cosmic Ray (UHECR) showers from space the details of fluorescence light production and transmission in the atmosphere are given. An analytical model of the fluorescence yield, in dependence on nitrogen molecular parameters and the atmospheric conditions, is presented. Seasonal and geographical variations of the total fluorescence photon yield between 300 nm and 400 nm in air excited by 0.85 MeV electrons are shown as a function of the altitude, using different atmospheric models. In the frame of a satellite-based UHECR experiment the fluorescence yield has been corrected by the overall atmospheric transmission which takes into account, in the simplest approximation, the wavelength-dependent scattering and absorption of the fluorescence light from air molecules, from stratospheric ozone, and from aerosol. The effect of the atmospheric attenuation on the fluorescence yield is shown as a function of the altitude of the emission point of light.

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