Study of extensive air showers at Mount Norikura. I. Measurement of lateral structure

1968 ◽  
Vol 46 (10) ◽  
pp. S17-S20 ◽  
Author(s):  
S. Miyake ◽  
K. Hinotani ◽  
N. Ito ◽  
S. Kino ◽  
H. Sasaki ◽  
...  
Keyword(s):  
Density Distribution ◽  
Charged Particles ◽  
High Energy ◽  
Extensive Air Showers ◽  
Two Dimensional ◽  
Air Showers ◽  
Complicated Structure ◽  
Unit Distance ◽  
Lateral Density Distribution ◽  
Lateral Structure

The lateral density distribution of charged particles in EAS is one of the essential parameters for the analysis of individual EAS. To measure the lateral density distribution in detail, 100 ¼-m2 scintillators were arranged in a lattice configuration with a unit distance of 5 m or 2.5 m. The conventional EAS array of 20 scintillators was also used to obtain densities up to about 100 m from the center. These observations are much more accurate than those obtained previously, and it has been found that there are various types of structure functions which can be approximated by the functions for single cascades of age parameter from 0.6 to 1.6. It was difficult in some instances to fit the lateral distribution by a unique function, especially for small EAS.The two-dimensional map obtained by means of the above 100 detectors shows that individual EAS have rarely a complicated structure within a range of about 20 m from the axis. The results are discussed in relation to the character of high-energy interactions as well as to fluctuations in the development of EAS.

scholarly journals Study of themuon content of high-energy air showers with KASCADE-Grande

2019 ◽  
Vol 208 ◽  
pp. 06003
Author(s):  
J.C. Arteaga-Velázquez ◽  
D. Rivera-Rangel ◽  
W.D. Apel ◽  
K. Bekk ◽  
M. Bertaina ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Density Distribution ◽  
Charged Particles ◽  
High Energy ◽  
Primary Energy ◽  
Measured Data ◽  
Attenuation Length ◽  
Air Showers ◽  
Hadronic Interaction ◽  
Lateral Density Distribution

In this work, we report measurements on the muon content (Eth > 230 MeV) of extensive air showers (EAS) induced by cosmic rays with primary energy from 10 PeV up to 1 EeV performed with the KASCADE-Grande experiment. The measurements are confronted with SIBYLL 2.3. The results are focused on the dependence of the total muon number and the lateral density distribution of muons in EAS on the zenith angle and the total number of charged particles in the shower. We also present updated results of a detailed study of the attenuation length of shower muons, which reveal a deviation between the measured data and the predictions of the post-LHC hadronic interaction models SIBYLL 2.3, QGSJET-II-04 and EPOS-LHC.

Study of extensive air showers at Mount Norikura. III. Core structure and high-energy events

1968 ◽  
Vol 46 (10) ◽  
pp. S25-S29 ◽  
Author(s):  
S. Miyake ◽  
K. Hinotani ◽  
N. Ito ◽  
S. Kino ◽  
H. Sasaki ◽  
...  
Keyword(s):  
Energy Flow ◽  
Particle Density ◽  
High Energy ◽  
Flow Density ◽  
Water Tank ◽  
Air Showers ◽  
Charged Particle Density ◽  
Lateral Density Distribution ◽  
Plastic Scintillators ◽  
Lateral Structure

An area of 3 × 4 m2 is covered by 48 plastic scintillators above and below a water tank 2 m in depth. From maps of the charged-particle density and the energy-flow density in the core region, properties of EAS cores and of the high-energy nucleon component have been studied. About 25% of observed cores show the complicated structure of a "multiple core". These can be understood as due to effects of high-energy nuclear particles having large transverse momenta of several GeV/c to a few tens of GeV/c. The frequency of occurrence of such events increases with the size of EAS only slowly, but it decreases rapidly with increasing distance between the main cores and subcores. There is no clear distinction in the average lateral density distribution of charged particles between these multiple-core EAS and ordinary EAS at points distant from the cores.Comparing the particle density in both layers of detectors (top and bottom), the activity of cores has been studied. This fluctuates more than would be expected from the lateral structure of the showers.

scholarly journals Tests of the SIBYLL 2.3 high-energy hadronic interaction model using the KASCADE-Grande muon data

2018 ◽  
Vol 172 ◽  
pp. 07003 ◽  
Author(s):  
J.C. Arteaga-Velázquez ◽  
D. Rivera-Rangel ◽  
W.D. Apel ◽  
K. Bekk ◽  
M. Bertaina ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Charged Particles ◽  
Interaction Model ◽  
High Energy ◽  
Attenuation Length ◽  
Air Showers ◽  
Hadronic Interaction ◽  
Air Shower ◽  
Lateral Density Distribution ◽  
Shower Array

The KASCADE-Grande observatory was a ground-based air shower array dedicated to study the energy and composition of cosmic rays in the energy interval E = 1 PeV –1 EeV. The experiment consisted of different detector systems which allowed the simultaneous measurement of distinct components of air showers (EAS), such as the muon content. In this contribution, we study the total muon number and the lateral density distribution of muons in EAS detected by KASCADE-Grande as a function of the zenith angle and the total number of charged particles. The attenuation length of the muon content of EAS is also measured. The results are compared with the predictions of the SIBYLL 2.3 high-energy hadronic interaction model.

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.

Monte Carlo studies on electromagnetic cascades in extensive air showers

1968 ◽  
Vol 46 (10) ◽  
pp. S189-S196 ◽  
Author(s):  
K. O. Thielheim ◽  
E. K. Schlegel ◽  
R. Beiersdorf
Keyword(s):  
Monte Carlo ◽  
Electron Density ◽  
Three Dimensional ◽  
High Energy ◽  
Extensive Air Showers ◽  
Air Showers ◽  
Energy Distributions ◽  
The Core ◽  
Fragmentation Mechanisms ◽  
Monte Carlo Studies

Three-dimensional Monte Carlo calculations have been performed on the trajectories of high-energy hadrons in extensive air showers. The central electron density and gradient of distribution are obtained for individual electromagnetic cascades together with coordinates at the level of observation. Various assumptions concerning primary mass number and energy, distributions of strong interaction parameters, and fragmentation mechanisms are discussed with respect to the production of steep maxima of electron density by single electromagnetic cascades in the core region of extensive air showers.

scholarly journals Determination of the invisible energy of extensive air showers from the data collected at Pierre Auger Observatory

2019 ◽  
Vol 210 ◽  
pp. 02010
Author(s):  
Analisa G. Mariazzi ◽  
Keyword(s):  
High Energy ◽  
Primary Energy ◽  
Energy Scale ◽  
Extensive Air Showers ◽  
Pierre Auger Observatory ◽  
Mass Composition ◽  
Air Showers ◽  
Systematic Uncertainties ◽  
Muon Production ◽  
The Invisible

In order to get the primary energy of cosmic rays from their extensive air showers using the fluorescence detection technique, the invisible energy should be added to the measured calorimetric energy. The invisible energy is the energy carried away by particles that do not deposit all their energy in the atmosphere. It has traditionally been calculated using Monte Carlo simulations that are dependent on the assumed primary particle mass and on model predictions for neutrino and muon production. In this work the invisible energy is obtained directly from events detected by the Pierre Auger Observatory. The method applied is based on the correlation of the measurements of the muon number at the ground with the invisible energy of the showers. By using it, the systematic uncertainties related to the unknown mass composition and to the high energy hadronic interaction models are significantly reduced, improving in this way the estimation of the energy scale of the Observatory.

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