On the possibility of investigation of the mass composition and energy spectra of primary cosmic ray (PCR) in the energy range from 1015 to 1017 eV using EAS data

1991 ◽  
Vol 14 (6) ◽  
pp. 555-568 ◽  
Author(s):  
A. A. Chilingarian ◽  
G. Z. Zazian
Keyword(s):  
Energy Range ◽  
Cosmic Ray ◽  
Energy Spectra ◽  
Mass Composition

scholarly journals Radio detection of cosmic rays with the Auger Engineering Radio Array

2019 ◽  
Vol 210 ◽  
pp. 05011 ◽  
Author(s):  
Tim Huege ◽  
Keyword(s):  
Cosmic Rays ◽  
Energy Range ◽  
Cosmic Ray ◽  
Energy Scale ◽  
Pierre Auger Observatory ◽  
Mass Composition ◽  
Frequency Range ◽  
Radio Detection ◽  
Composition Measurements

The Auger Engineering Radio Array (AERA) complements the Pierre Auger Observatory with 150 radio-antenna stations measuring in the frequency range from 30 to 80 MHz. With an instrumented area of 17 km2, the array constitutes the largest cosmic-ray radio detector built to date, allowing us to do multi-hybrid measurements of cosmic rays in the energy range of 1017 eV up to several 1018 eV. We give an overview of AERA results and discuss the significance of radio detection for the validation of the energy scale of cosmicray detectors as well as for mass-composition measurements.

scholarly journals Cosmic Ray Energy Spectra and Mass Composition at the Knee – Recent Results from KASCADE –

2004 ◽  
Vol 136 ◽  
pp. 273-281 ◽  
Author(s):  
K.-H. Kampert ◽  
T. Antoni ◽  
W.D. Apel ◽  
F. Badea ◽  
K. Bekk ◽  
...  
Keyword(s):  
Cosmic Ray ◽  
Energy Spectra ◽  
Mass Composition

Estimating of Cherenkov Radiation in Extensive Air Showers Using CORSIKA Code for Tunka133 EAS Cherenkov Array

2015 ◽  
Vol 754-755 ◽  
pp. 807-811
Author(s):  
A.A. Al-Rubaiee ◽  
Uda Hashim ◽  
Mohd Khairuddin Md Arshad ◽  
A. Rahim Ruslinda ◽  
R.M. Ayub ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Energy Range ◽  
Cosmic Ray ◽  
High Energy ◽  
Extensive Air Showers ◽  
Cherenkov Light ◽  
Mass Composition ◽  
Air Showers ◽  
Good Ability ◽  
The Given

The simulation of Cherenkov light Lateral distribution function (LDF) in Extensive Air Showers (EAS) initiated primary particles such as primary calcium, argon, proton iron nuclei, neutron and nitrogen have been performed using CORSIKA program for conditions and configurations of Tunka133 EAS Cherenkov array. The simulation was fulfilled at the high energy range 1014-1016eV for four different zenith angles 0o, 10o, 15oand 30o. The results of the simulated Cherenkov light LDF are compared with the measurements of Tunka133 EAS array for the same particles and energy range mentioned above. This comparison may give the good ability to reconstruct the energy spectrum and mass composition of the primary cosmic ray particles in EAS. The main feature of the given approach consists of the possibility to make a library of Cherenkov light LDF samples which could be utilized for analysis of real events which can be detected with different EAS arrays and reconstruction of the primary cosmic rays energy spectrum and mass composition of EAS particles.

ENERGY SPECTRA AND MASS COMPOSITION OF COSMIC RAYS IN THE FRACTAL-LIKE GALACTIC MEDIUM

2005 ◽  
Vol 20 (29) ◽  
pp. 6834-6836 ◽  
Author(s):  
A. A. LAGUTIN ◽  
A. G. TYUMENTSEV ◽  
A. V. YUSHKOV
Keyword(s):  
Cosmic Rays ◽  
Cosmic Ray ◽  
Energy Spectra ◽  
Mass Composition ◽  
Primary Spectrum ◽  
Composition Variation ◽  
Region 10 ◽  
Basic Features ◽  
Galactic Sources ◽  
Knee Problem

We consider the problem of the cosmic ray spectrum formation assuming that cosmic rays are produced by galactic sources. The fractional diffusion equation proposed in our recent papers is used to describe the cosmic rays propagation in interstellar medium. We show that in the framework of this approach it is possible to explain the locally observed basic features of the cosmic rays in the energy region 1010 ÷ 1020 eV : difference between spectral exponents of protons and other nuclei, mass composition variation, "knee" problem, flattening of the primary spectrum for E ≥ 1018 ÷ 1019 eV .

Low-energy cosmic-ray heavy nuclei during the time of solar minimum

1968 ◽  
Vol 46 (10) ◽  
pp. S598-S600
Author(s):  
E. Tamai ◽  
M. Tsubomatsu ◽  
K. Ogura
Keyword(s):  
Energy Range ◽  
Solar Minimum ◽  
Cosmic Ray ◽  
Low Energy ◽  
Energy Spectra ◽  
Solar Modulation ◽  
Atmospheric Depth ◽  
Heavy Nuclei ◽  
Multiply Charged ◽  
Α Particles

Nuclear emulsions were exposed at 2.3 g cm−2 atmospheric depth over Fort Churchill in 1965. These emulsions have been examined for the tracks of multiply-charged [Formula: see text] nuclei, with emphasis being paid particularly to those particles that stopped in the emulsions. Differential energy spectra of α particles and [Formula: see text], [Formula: see text]and [Formula: see text] nuclei were obtained in the energy interval 60–550 MeV/nucleon. They represent experimental results during the period when solar modulation effects were at a minimum. The fluxes of α particles and L, M, and H nuclei for energy intervals of 60–170, 100–400, 100–525, and 140–550 MeV/nucleon were found to be 20.9 ± 1.2, 2.4 ± 0.4, 4.8 ± 0.6, and 2.5 ± 0.4 particles m−2 sr−1 s−1, respectively. The results also show that the L/M and H/M ratios at the top of the atmosphere were 0.56 ± 0.16 and 0.34 ± 0.13 respectively, in the energy range from 140 to 350 MeV/nucleon. These values are appreciably greater than those observed at higher energies.

Primary protons and alpha particles in the energy range 70–240 MeV/nucleon observed during 1966

1968 ◽  
Vol 46 (10) ◽  
pp. S900-S902
Author(s):  
G. D. Badhwar ◽  
C. L. Deney ◽  
B. R. Dennis ◽  
M. F. Kaplon
Keyword(s):  
Energy Range ◽  
Solar Minimum ◽  
Cosmic Ray ◽  
Alpha Particles ◽  
Energy Spectra ◽  
Modulation Function ◽  
Residual Material ◽  
Acceptance Range

The differential energy spectra of cosmic-ray protons and helium nuclei were measured on two balloon flights from Fort Churchill, Canada, during late July and early August of 1966. The measurements were made using a double dE/dx vs. E detector with an energy-independent (for stopping particles) acceptance aperture of 6 cm2 sr. The detector floated for a total of 25 hours under 2.7 g/cm2 of residual material. The acceptance range of energies is 70–240 MeV/nucleon for protons and 4He. Both the proton and 4He differential spectra are depressed from solar minimum and appear similar to 1963 results. The P/He ratio over the energy range is 4.3 ± 1. The spectra are compared to those obtained in 1965. It is found that the modulation function is proportional to either R or Rβ.

scholarly journals THE TUNKA EXPERIMENT: TOWARDS A 1-KM2 CHERENKOV EAS ARRAY IN THE TUNKA VALLEY

2005 ◽  
Vol 20 (29) ◽  
pp. 6796-6798 ◽  
Author(s):  
D. V. CHERNOV ◽  
N. N. KALMYKOV ◽  
E. E. KOROSTELEVA ◽  
L. A. KUZMICHEV ◽  
V. V. PROSIN ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Energy Range ◽  
Cosmic Ray ◽  
Mass Composition

The project of an EAS Cherenkov array in the Tunka Valley/Siberia with an area of about 1 km2 is presented. The new array will have a ten times bigger area than the existing TUNKA-25 array and will permit a detailed study of the cosmic ray energy spectrum and the mass composition in the energy range from 1015 to 1018 eV.

Composition and energy spectra of cosmic-ray primaries in the energy range 1013–1015 eV/particle observed by Japanese–Russian joint balloon experiment

2001 ◽  
Vol 16 (1) ◽  
pp. 13-46 ◽  
Author(s):  
A.V. Apanasenko ◽  
V.A. Sukhadolskaya ◽  
V.A. Derbina ◽  
M. Fujii ◽  
V.I. Galkine ◽  
...  
Keyword(s):  
Energy Range ◽  
Cosmic Ray ◽  
Energy Spectra ◽  
Balloon Experiment
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