ABOUT ONE WAY OF ORGANIZATION UNIFIED SYSTEM FOR REGISTRATION OF SPACE RAYS

2021 ◽  
Vol 75 (3) ◽  
pp. 64-69
Author(s):  
К.М. Mukashev ◽  
◽  
A.V. Stepanov ◽  
T.Kh. Sadykov ◽  
A. К. Argynova ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Modern Technology ◽  
Mass Composition ◽  
Energy Structure ◽  
High Mountain ◽  
Scientific Station ◽  
Electron Photon ◽  
Time Of Operation ◽  
High Degree ◽  
Photon Component

At present, at the high-mountain scientific station for the study of the physics of cosmic rays, various, independently operating unique experimental installations are used. The article discusses the ways and methods of combining these installations into a single system, which includes networks of scintillation detectors of the "carpet" type for registration of the electron-photon component, ground and underground monitors for registration of neutron components, calorimeters, Cherenkov detectors, a scintillation spectrometer and a number of other subsystems. The newly created unified system for registering cosmic rays based on the achievements of modern technology and scientific thought will have a high resolution, with a common databank with synchronization in time of operation of separate, independently operating experimental installations. The solution to this problem will make it possible to perform a detailed analysis of the recorded events from a single position, to carry out complex calculations of the spatial distribution, mass composition, and also the energy structure of cosmic rays with a high degree of accuracy.

scholarly journals INFLUENCE OF PRIMARY COSMIC RADIATION MASS COMPOSITION ON THE ESTIMATION OF EAS ENERGY

2005 ◽  
Vol 20 (29) ◽  
pp. 6897-6899 ◽  
Author(s):  
S. P. KNURENKO ◽  
A. A. IVANOV ◽  
V. A. KOLOSOV ◽  
Z. E. PETROV ◽  
I. YE. SLEPTSOV ◽  
...  
Keyword(s):  
Cosmic Radiation ◽  
Cherenkov Radiation ◽  
Charged Particles ◽  
Mass Composition ◽  
Mixed Composition ◽  
Radiation Data ◽  
Primary Particles ◽  
Primary Cosmic Radiation ◽  
Electron Photon ◽  
Photon Component

Fraction of energy, E em /E0, transferred to the electron-photon component of EAS at E0 = 1015 ± 1019 eV was estimated by using the Cherenkov radiation data and the data on charged particles obtained at the Yakutsk EAS array. The results are compared with predictions of different models for energy dissipation into the EAS electron-photon component and with calculations performed with different primary nuclei content. In the energy ranges 1015 ± 1016 eV and 1018 ± 1019 eV , the ratio E em /E0 is equal to (77 ± 2)% and (88 ± 2)%, respectively, that does not contradict to a mixed composition of primary particles in the first energy interval and purely proton composition in the second one.

scholarly journals 5. Study of Cosmic Rays by Rockets and Sputniks in the U.S.S.R.

1960 ◽  
Vol 10 ◽  
pp. 710-712
Author(s):  
S. N. Vernov ◽  
A. E. Chudakov
Keyword(s):  
Cosmic Rays ◽  
Charged Particles ◽  
Light Elements ◽  
Primary Particles ◽  
In The Beginning ◽  
Electron Photon ◽  
Photon Component

In the U.S.S.R. the study of cosmic rays by rockets was started in 1947.In the beginning, with the help of Geiger counters the number of charged particles was measured, and the formation of the electron-photon component in the interaction of primary particles of cosmic rays with nuclei of light elements was investigated.

scholarly journals 6. Rocket and satellite investigation of meteors

1960 ◽  
Vol 10 ◽  
pp. 713-714
Author(s):  
I. N. Nazarova
Keyword(s):  
Cosmic Rays ◽  
Charged Particles ◽  
High Energy ◽  
Light Elements ◽  
Primary Particles ◽  
In The Beginning ◽  
Electron Photon ◽  
Photon Component

In the U.S.S.R. the study of cosmic rays by rockets was started in 1947. In the beginning, with the help of Geiger counters the number of charged particles was measured, and the formation of the electron-photon component in the interaction of primary particles of cosmic rays with nuclei of light elements was investigated. It was shown that in 1947,1948,1949 and 1951 the intensity of cosmic rays at altitudes up to 75 km was the same and did not change more than by 5 %. In 1949 the data on the photon intensities outside the atmosphere were obtained. In order to measure the number of high-energy photons, one of us (A. E. Chudakov) proposed a method permitting these measurements to be made with a strong background of charged particles.

scholarly journals Depth of shower maximum and mass composition of cosmic rays from 50 PeV to 2 EeV measured with the LOFAR radio telescope

2021 ◽  
Vol 103 (10) ◽  
Author(s):  
A. Corstanje ◽  
S. Buitink ◽  
H. Falcke ◽  
B. M. Hare ◽  
J. R. Hörandel ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Radio Telescope ◽  
Mass Composition ◽  
Shower Maximum

Energy spectrum and mass composition of high-energy cosmic rays

2003 ◽  
Vol 66 (7) ◽  
pp. 1145-1206 ◽  
Author(s):  
Andreas Haungs ◽  
Heinigerd Rebel ◽  
Markus Roth
Keyword(s):  
Energy Spectrum ◽  
Cosmic Rays ◽  
High Energy ◽  
Mass Composition ◽  
High Energy Cosmic Rays

The promise of the Tunka-Grande scintillation experiment for studying the mass composition of primary cosmic rays

2015 ◽  
Vol 70 (2) ◽  
pp. 160-165 ◽  
Author(s):  
N. M. Budnev ◽  
A. L. Ivanova ◽  
N. N. Kalmykov ◽  
L. A. Kuzmichev ◽  
V. P. Sulakov ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Mass Composition ◽  
Primary Cosmic Rays

Low-energy muons in extensive air showers at 800 g cm−2

1968 ◽  
Vol 46 (10) ◽  
pp. S131-S135 ◽  
Author(s):  
B. K. Chatterjee ◽  
N. V. Gopalakrishnan ◽  
G. T. Murthy ◽  
S. Naranan ◽  
B. V. Sreekantan ◽  
...  
Keyword(s):  
Size Range ◽  
Low Energy ◽  
Extensive Air Showers ◽  
Air Showers ◽  
Average Total Number ◽  
The Right ◽  
Electron Photon ◽  
Photon Component ◽  
Lateral Structure ◽  
Right Ascension

The following results on the low-energy (> 0.6 GeV and > 1.0 GeV) muons in air showers of size 105 to 2 × 107 at Ootacamund (800 g cm−2) are obtained: (1) The average total number of muons [Formula: see text] varies as Ne0.32 ± 0.2 for 105 < Ne < 106, and as Ne0.8 ± 0.15for 106 < Ne < 2 × 107. (2) In showers showing flat electron lateral structure, the [Formula: see text] variation with Ne is similar to (1). However, in steep showers, [Formula: see text] varies as Ne0.75 ± 0.15 in the whole size range 105 to 2 × 107. (3) "Muon-rich" showers of size < 106 have less energy in the electron–photon component compared to "normal" showers. No such difference is found for showers of size > 106. (4) There is a slight indication of a deficiency of muon-rich showers having a flat lateral distribution of electrons in the right ascension interval 15–21 hours for showers of size 106–107. A similar deficit of showers was observed by the Tokyo group for muon-rich showers in the same RA interval.

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