Application of continuous-energy Monte Carlo code as a cross-section generator of BWR core calculations

2005 ◽  
Vol 32 (8) ◽  
pp. 857-875 ◽  
Author(s):  
Masayuki Tohjoh ◽  
Masato Watanabe ◽  
Akio Yamamoto
Keyword(s):  
Monte Carlo ◽  
Cross Section ◽  
Monte Carlo Code ◽  
Continuous Energy

A collision history-based approach to sensitivity/perturbation calculations in the continuous energy Monte Carlo code SERPENT

2015 ◽  
Vol 85 ◽  
pp. 245-258 ◽  
Author(s):  
Manuele Aufiero ◽  
Adrien Bidaud ◽  
Mathieu Hursin ◽  
Jaakko Leppänen ◽  
Giuseppe Palmiotti ◽  
...  
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Code ◽  
Continuous Energy

scholarly journals Analyses of Assay Data of LWR Spent Nuclear Fuels with a Continuous-Energy Monte Carlo Code MVP and JENDL-4.0 for Inventory Estimation of 79Se, 99Tc, 126Sn and 135Cs

2011 ◽  
Vol 2 (0) ◽  
pp. 369-374 ◽  
Author(s):  
Keisuke OKUMURA ◽  
Shiho ASAI ◽  
Yukiko HANZAWA ◽  
Hideya SUZUKI ◽  
Masaaki TOSHIMITSU ◽  
...  
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Code ◽  
Nuclear Fuels ◽  
Continuous Energy

scholarly journals Microscopic cross section calculation methodology in the Serpent 2 Monte Carlo code

2021 ◽  
Vol 164 ◽  
pp. 108603
Author(s):  
Antti Rintala ◽  
Ville Valtavirta ◽  
Jaakko Leppänen
Keyword(s):  
Monte Carlo ◽  
Cross Section ◽  
Monte Carlo Code ◽  
Calculation Methodology

Wolf-Rayet Wind Models: Photometric and Polarimetric Variability

1999 ◽  
Vol 169 ◽  
pp. 57-61
Author(s):  
Cláudia V. Rodrigues ◽  
Antônio Mário Magalhães
Keyword(s):  
Monte Carlo ◽  
Cross Section ◽  
Broad Band ◽  
Variable Structure ◽  
Band Intensity ◽  
Stokes Parameters ◽  
Monte Carlo Code ◽  
Photometric Variability ◽  
Random Variation

AbstractWe have modelled the observed random variation in broad band intensity and polarization of some isolated Wolf-Rayet stars assuming that their winds have localized, enhanced density regions (blobs). Our model is based on a Monte Carlo code that treats all Stokes parameters of the radiation bundle. This study indicates that the blobs must have sizes comparable to the stellar dimension and be near the base of the envelope. These blobs can be interpreted as a variable structure of large geometric cross section causing the observed polarimetric and photometric variability.

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