scholarly journals Air shower simulation for background estimation in muon tomography of volcanoes

2013 ◽  
Vol 2 (1) ◽  
pp. 11-15 ◽  
Author(s):  
S. Béné ◽  
P. Boivin ◽  
E. Busato ◽  
C. Cârloganu ◽  
C. Combaret ◽  
...  
Keyword(s):  
Monte Carlo ◽  
Spatial Distribution ◽  
Energy Spectrum ◽  
Charged Particles ◽  
Cosmic Ray ◽  
Background Estimation ◽  
Air Shower ◽  
Muon Tomography ◽  
Background Effect ◽  
Good Agreement

Abstract. One of the main sources of background for the radiography of volcanoes using atmospheric muons comes from the accidental coincidences produced in the muon telescopes by charged particles belonging to the air shower generated by the primary cosmic ray. In order to quantify this background effect, Monte Carlo simulations of the showers and of the detector are developed by the TOMUVOL collaboration. As a first step, the atmospheric showers were simulated and investigated using two Monte Carlo packages, CORSIKA and GEANT4. We compared the results provided by the two programs for the muonic component of vertical proton-induced showers at three energies: 1, 10 and 100 TeV. We found that the spatial distribution and energy spectrum of the muons were in good agreement for the two codes.

scholarly journals Air shower simulation for background estimation in muon tomography of volcanoes

2012 ◽  
Vol 2 (2) ◽  
pp. 563-574 ◽  
Author(s):  
S. Béné
Keyword(s):  
Monte Carlo ◽  
Spatial Distribution ◽  
Energy Spectrum ◽  
Monte Carlo Simulations ◽  
Arrival Time ◽  
Air Showers ◽  
Background Estimation ◽  
Air Shower ◽  
Muon Tomography ◽  
Good Agreement

Abstract. One of the main sources of background for the radiography of volcanoes with atmospheric muons comes from the accidental coincidences produced in the muon telescopes by the air showers. In order to quantify this background, Monte-Carlo simulations of the showers and of the detector are developed by the Tomuvol collaboration. As a first step, the atmospheric showers were simulated and investigated using two Monte-Carlo packages, CORSIKA and GEANT4. We compared the results provided by the two programs for the muonic component of vertical proton-induced showers at three energies: 1, 10 and 100 TeV. We found that the spatial distribution and energy spectrum of the muons were in good agreement for the two codes, while significant differences were observed for the arrival time of the muons.

scholarly journals Atmospheric Muons Measured with IceCube

2019 ◽  
Vol 208 ◽  
pp. 08007 ◽  
Author(s):  
Dennis Soldin
Keyword(s):  
Angular Distribution ◽  
Energy Spectrum ◽  
Cosmic Ray ◽  
Cherenkov Detector ◽  
South Pole ◽  
Lateral Separation ◽  
Hadronic Interactions ◽  
Air Shower ◽  
Shower Development ◽  
Detector Volume

IceCube is a cubic-kilometer Cherenkov detector in the deep ice at the geographic South Pole. The dominant event yield is produced by penetrating atmospheric muons with energies above several 100 GeV. Due to its large detector volume, IceCube provides unique opportunities to study atmospheric muons with large statistics in detail. Measurements of the energy spectrum and the lateral separation distribution of muons offer insights into hadronic interactions during the air shower development and can be used to test hadronic models. We will present an overview of various measurements of atmospheric muons in IceCube, including the energy spectrum of muons between 10 TeV and 1 PeV. This is used to derive an estimate of the prompt contribution of muons, originating from the decay of heavy (mainly charmed) hadrons and unflavored mesons. We will also present measurements of the lateral separation distributions of TeV muons between 150m and 450m for several initial cosmic ray energies between 1 PeV and 16 PeV. Finally, the angular distribution of atmospheric muons in IceCube will be discussed.

EMISSION OF NUCLEI IN COSMIC RAY STARS

1950 ◽  
Vol 28a (6) ◽  
pp. 616-627 ◽  
Author(s):  
E. Pickup ◽  
L. Voyvodic
Keyword(s):  
Excited State ◽  
Energy Spectrum ◽  
Radioactive Decay ◽  
Cosmic Ray ◽  
Cloud Chamber ◽  
Photographic Emulsions ◽  
Chamber Technique ◽  
Good Agreement ◽  
Α Particles

One of the more interesting features of cosmic ray stars is that [Formula: see text] nuclei are ejected occasionally in the nuclear disintegrations. Such nuclei are characterized by the fact that, at the end of their range, they suffer radioactive decay (τ = 0.9 sec.) into [Formula: see text], which immediately splits up into two oppositely directed α-particles, giving what is usually referred to as a hammer track. In this investigation numerous examples have been observed of the emission of such nuclei in stars in photographic emulsions, the stars having from 2 to 60 prongs. In particular, it has been shown that the energy spectrum of the α-particles forming the hammer tracks is in good agreement with that observed by other workers, and also with experiments made, using the cloud chamber technique, indicating that the [Formula: see text] in this disintegration is formed in the excited state. When an electron sensitive emulsion is used it is shown that the hammer track is accompanied by the [Formula: see text] disintegration electron. The energy spectrum of the [Formula: see text] nuclei is plotted, and the mechanism of the formation is discussed for both large and small stars.

Tokyo large air shower project

1968 ◽  
Vol 46 (10) ◽  
pp. S255-S258 ◽  
Author(s):  
T. Matano ◽  
M. Nagano ◽  
K. Suga ◽  
G. Tanahashi
Keyword(s):  
Energy Spectrum ◽  
Particle Density ◽  
Cosmic Ray ◽  
High Energy ◽  
Size Spectrum ◽  
Telemetry System ◽  
Simple Experiment ◽  
Air Showers ◽  
Fundamental Idea ◽  
Air Shower

A preliminary experiment to detect large air showers by means of radio echoes and to study the high-energy end of the primary cosmic-ray energy spectrum has been started at this Institute. The fundamental idea and the first approach of the experiment are presented. Using the telemetry system between two pairs of a simple scintillation array, which has been constructed to identify and calibrate the showers in the above experiment, the decoherence curve of air showers has been measured between 100 and 1 300 m together with the particle density in each detector. This simple experiment will give the power of the size spectrum above 109.

scholarly journals Cosmic Ray Energy Spectrum derived from the Data of EAS Cherenkov Light Arrays in the Tunka Valley

2019 ◽  
Vol 210 ◽  
pp. 01003
Author(s):  
V. Prosin ◽  
I. Astapov ◽  
P. Bezyazeekov ◽  
A. Borodin ◽  
M. Brückner ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Cosmic Rays ◽  
Energy Range ◽  
Cosmic Ray ◽  
Cherenkov Light ◽  
Differential Energy Spectrum ◽  
Extensive Air Shower ◽  
Air Shower

The extensive air shower Cherenkov light array Tunka-133 collected data during 7 winter seasons from 2009 to 2017. From 2175 hours of data taking, we derived the differential energy spectrum of cosmic rays in the energy range 6 · 1015 2 · 1018 eV. The TAIGA-HiSCORE array is in the process of continuous expansion and modernization. Here we present the results obtained with 28 stations of the first HiSCORE stage from 35 clear moonless nights in the winter of 2017-2018. The combined spectrum of two arrays covers a range of 2 · 1014 – 2 · 1018 eV.

The cosmic-ray energy spectrum around the knee measured by the Tibet-III air-shower array

2008 ◽  
Vol 175-176 ◽  
pp. 318-321 ◽  
Author(s):  
M. Amenomori ◽  
S. Ayabe ◽  
X.J. Bi ◽  
D. Chen ◽  
S.W. Cui ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Cosmic Ray ◽  
Air Shower ◽  
Shower Array ◽  
Air Shower Array

Analysis on High-Energy Physical Problems in Monte Carlo Simulation

2014 ◽  
Vol 577 ◽  
pp. 762-766
Author(s):  
Bao Guang Sun ◽  
Xiao Feng Wang
Keyword(s):  
Monte Carlo Simulation ◽  
Monte Carlo ◽  
Energy Spectrum ◽  
High Energy ◽  
Extensive Air Shower ◽  
Air Shower ◽  
Secondary Particles ◽  
Physical Problems ◽  
Strip Pattern ◽  
Detector Simulation

This paper analyzes the data got in two Monte Carlo simulations, namely, extensive air shower simulation and detector simulation. Then, based on the data from experimental arrays, some physical problems have been analyzed and illustrated. Those problems include the distribution of energy spectrum of secondary particles, the distribution of zenith angle, of azimuths, of background noises, and that of strip pattern, as well as the atmospheric absorption.

scholarly journals The cosmic-ray energy spectrum above $\sim 10^{16}$ eV measured with the LOFAR Radboud Air Shower Array

2016 ◽  
Author(s):  
Satyendra Thoudam ◽  
Stijn Buitink ◽  
Arthur Corstanje ◽  
Emilio Enriquez ◽  
Heino Falcke ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Cosmic Ray ◽  
Air Shower ◽  
Shower Array ◽  
Air Shower Array

scholarly journals Monte Carlo simulation of the cosmic muon charge ratio

2021 ◽  
Vol 49 (1) ◽  
Author(s):  
Abd Al Karim Haj Ismail ◽  
◽  
Keyword(s):  
Monte Carlo ◽  
Charged Particles ◽  
Radial Distance ◽  
Cosmic Ray ◽  
Charge Ratio ◽  
Air Showers ◽  
Central European ◽  
Hadronic Interactions ◽  
High Energies ◽  
Deep Underground

The muonic component of air showers is sensitive to the mass and energy of the primary cosmic ray and is the most abundant component of charged particles arriving at the surface, and able to penetrate deep underground. The muon charge ratio, defined as the number of positive over negatively charged muons, is a very interesting quantity for the study of hadronic interactions at high energies and the nature of cosmic ray primaries. Furthermore, Earth's atmosphere is the development medium of cosmic air showers before they arrive at the ground. Therefore, variations in the density of the atmosphere between seasons must be studied. It is also very important to account for the zenith angular dependence of atmospheric muons, in particular for showers penetrating the atmosphere at high zenith angles. We present a study of the muon charge ratio using Monte Carlo simulations of two cosmic primaries, proton, and iron, of 100 TeV and 1 PeV energies, and with a zenith angle of 0° to 60°. The dependence on the direction of extensive air showers EAS and their radial distance appears to be very pronounced. In addition, the muon density is discussed assuming the Central European Atmosphere in June and December.

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