scholarly journals Calculation of Neutron Fluence and Energy Release in WWER-1000 Structural Components Using Monte Carlo Method

2018 ◽  
pp. 11-17
Author(s):  
A. Abdullaiev ◽  
S. Soldatov ◽  
V. Hann ◽  
S. Chernitskyi
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Method ◽  
Energy Release ◽  
Neutron Source ◽  
Neutron Fluence ◽  
Structural Components ◽  
Preliminary Results ◽  
The Core ◽  
Mcnpx Code

The paper describes the methodology for the calculation of neutron fluence and energy release in WWER-1000 reactor cavity and baffle using the Monte Carlo MCNPX code. It formulates an approach to the simulation of a 3-D neutron source and conditions for the transport of neutrons and photons in the core. The research presents preliminary results of neutron fluence and energy release calculation in WWER-1000 reactor cavity and baffle. 

scholarly journals NEUTRON RESPONSE FUNCTION OF BONNER SPHERE SPECTROMETER WITH 6LiI(Eu) DETECTOR

2017 ◽  
Vol 20 (2) ◽  
pp. 65 ◽  
Author(s):  
Rasito Tursinah ◽  
Bunawas Bunawas ◽  
Jungho Kim
Keyword(s):  
Monte Carlo ◽  
Response Function ◽  
Neutron Fluence ◽  
Detector Response ◽  
Response Functions ◽  
Neutron Spectra ◽  
Mcnpx Code ◽  
Bonner Sphere ◽  
Bonner Sphere Spectrometer

Neutron Response Function of Bonner Sphere Spectrometer With 6LiI(Eu) Detector. The detector response function was needed to measure the neutron fluence based on the count rates from Bonner Sphere Spectrometer (BSS). The determination of response function of a BSS with 6LiI(Eu) detector has been performed using Monte Carlo MCNPX code. This calculation was performed for BSS using scintillation detector of 4 mm × 4 mm 6LiI(Eu) which is placed at the center of a set of polyethylene spheres i.e bare, 2", 3", 5", 8", 10", and 12" diameters. The BSS response functions were obtained for neutron energy of 1x10-9 MeV - 1x102  MeV in 111 energy bins and each value has an uncertainty less or equal to 2 %. The response function were compared with two response functions reported in the literature i.e IAEA document in Technical Reports Series 403 (TRS-403) and the calculation from Vega-Carrillo, et al. Also validated with measurement 252Cf neutron spectra, that shown the simulated BSS spectra were quite close to the experimental measured with a differrence of 3%.

Local Ice Loads on the Sakhalin-II Project Structures: Probability Analysis and Comparison by Existing Design Codes

2016 ◽  
Author(s):  
Olga A. Sabodash
Keyword(s):  
Monte Carlo ◽  
Comparative Analysis ◽  
Monte Carlo Method ◽  
Engineering Design ◽  
Probabilistic Analysis ◽  
Design Codes ◽  
Local Pressure ◽  
Preliminary Results ◽  
Ice Loads ◽  
Scale Data

In the study the probabilistic modeling of local ice loads and pressures on wide structure has been carried out. Probabilistic analysis has traditionally been focused on distribution of their maximum values. The “Molikpaq” (PA-A) ice-class platform for “Sakhalin-II” project is considered as an example. The input parameters were modelled by Monte-Carlo method taking into account of full-scale data in the Piltun-Astokhskoe field during 1989÷2002 ice seasons. A comparative analysis of local ice loads and pressures on wide structure has been made on the basis of the Russian and international design codes, standards and recommendations. The obtained local pressure values were compared with public available data collected on the “Molikpaq” (PA-A) platform. Some preliminary results and discussions are presented. Recommendations on the local ice loads and pressures for engineering design of structures on the Sakhalin offshore have been done.

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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