Reproduction of true energy spectrum of charged particles with Monte Carlo method

2018 ◽  
Vol 13 (12) ◽  
pp. P12030-P12030 ◽  
Author(s):  
M. Rajput ◽  
P.V. Subhash ◽  
P. Kanth ◽  
S. Vala ◽  
R. Srinivasan
Keyword(s):  
Monte Carlo ◽  
Energy Spectrum ◽  
Monte Carlo Method ◽  
Charged Particles ◽  
True Energy

Simulation on Multiple Scattering of Charged Particles Using Monte Carlo Method

1974 ◽  
Vol 37 (2) ◽  
pp. 454-459 ◽  
Author(s):  
Tetsuo Yamazaki ◽  
Minoru Takasaki ◽  
Seiji Kashioka ◽  
Masakatsu Sakisaka
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Method ◽  
Multiple Scattering ◽  
Charged Particles

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.

Outbursts of comet Schwassmann-Wachmann 1, and the cloud of interplanetary boulders

1974 ◽  
Vol 22 ◽  
pp. 307 ◽  
Author(s):  
Zdenek Sekanina
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Method ◽  
Interplanetary Space ◽  
Porous Matrix ◽  
Maximum Diameter ◽  
Expansion Velocity ◽  
Solid Constituent ◽  
Meteoric Material ◽  
Periodic Comet

AbstractIt is suggested that the outbursts of Periodic Comet Schwassmann-Wachmann 1 are triggered by impacts of interplanetary boulders on the surface of the comet’s nucleus. The existence of a cloud of such boulders in interplanetary space was predicted by Harwit (1967). We have used the hypothesis to calculate the characteristics of the outbursts – such as their mean rate, optically important dimensions of ejected debris, expansion velocity of the ejecta, maximum diameter of the expanding cloud before it fades out, and the magnitude of the accompanying orbital impulse – and found them reasonably consistent with observations, if the solid constituent of the comet is assumed in the form of a porous matrix of lowstrength meteoric material. A Monte Carlo method was applied to simulate the distributions of impacts, their directions and impact velocities.

Structures and crystallization of vacuum-deposited amorphous Se and Sb films

1990 ◽  
Vol 48 (4) ◽  
pp. 140-141
Author(s):  
Makoto Shiojiri ◽  
Toshiyuki Isshiki ◽  
Tetsuya Fudaba ◽  
Yoshihiro Hirota
Keyword(s):  
Monte Carlo ◽  
Electron Microscope ◽  
Monte Carlo Method ◽  
Computer Program ◽  
Radial Distribution ◽  
Film Formation ◽  
Amorphous State ◽  
Two Dimensional ◽  
Amorphous Films ◽  
Binding Condition

In hexagonal Se crystal each atom is covalently bound to two others to form an endless spiral chain, and in Sb crystal each atom to three others to form an extended puckered sheet. Such chains and sheets may be regarded as one- and two- dimensional molecules, respectively. In this paper we investigate the structures in amorphous state of these elements and the crystallization.HRTEM and ED images of vacuum-deposited amorphous Se and Sb films were taken with a JEM-200CX electron microscope (Cs=1.2 mm). The structure models of amorphous films were constructed on a computer by Monte Carlo method. Generated atoms were subsequently deposited on a space of 2 nm×2 nm as they fulfiled the binding condition, to form a film 5 nm thick (Fig. 1a-1c). An improvement on a previous computer program has been made as to realize the actual film formation. Radial distribution fuction (RDF) curves, ED intensities and HRTEM images for the constructed structure models were calculated, and compared with the observed ones.

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