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Research Papers

Cross-Section Influence on Monte Carlo-Based Burn-Up Codes Applied to a GFR-Like Configuration

[+] Author and Article Information
Davide Chersola

GeNERG—DIME/TEC University of Genova,
Via all’Opera Pia, 15/A, 16145 Genova, Italy;
INFN,
Via Dodecaneso, 33, 16146 Genova, Italy
e-mail: davide.chersola@edu.unige.it

Guglielmo Lomonaco

Mem. ASME
GeNERG—DIME/TEC University of Genova,
Via all’Opera Pia, 15/A, 16145 Genova, Italy;
INFN,
Via Dodecaneso, 33, 16146 Genova, Italy
e-mail: guglielmo.lomonaco@unige.it

Guido Mazzini

Centrum výzkumu Řež,
25068 Husinec-Rez, Czech Republic
e-mail: guido.mazzini@cvrez.cz

1Corresponding author.

Manuscript received July 24, 2014; final manuscript received January 4, 2015; published online May 20, 2015. Assoc. Editor: Jay F. Kunze.

ASME J of Nuclear Rad Sci 1(3), 031004 (May 20, 2015) (15 pages) Paper No: NERS-14-1027; doi: 10.1115/1.4029521 History: Received July 24, 2014; Accepted January 07, 2015; Online May 20, 2015

This paper reports the results of a comparison among JEFF and ENDF/B data sets when used by SERPENT and MONTEBURNS codes on a gas-cooled fast reactor (GFR)-like configuration. Particularly, it shows a comparison between the two Monte Carlo-based codes, each one adopting three different cross-section data sets, namely, JEFF-3.1, JEFF-3.1.2, and ENDF/B-VII.1. Calculations have been carried out on the Allegro reactor, i.e., an experimental GFR-like facility that could be built in the European Union as a GFR demonstration. Results include nuclear parameters, such as the effective multiplication factor and fluxes, as well as the atomic densities for some important nuclides versus burn-up.

Copyright © 2015 by ASME
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References

Figures

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Fig. 1

Allegro radial (left) and axial (right) geometrical cross sections (created by SERPENT geometry plotter)

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Fig. 2

Fuel S/As: MOX24 pin S/A (left) and experimental S/A (right)

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Fig. 3

SERPENT, trends of keff versus burn-up

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Fig. 4

MONTEBURNS, trends of keff versus burn-up

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Fig. 5

SERPENT, 69-group spectra for the whole core

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Fig. 6

MONTEBURNS, 69-group spectra for the whole core

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Fig. 7

SERPENT, 69-group spectra in fuel pin S/As

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Fig. 8

MONTEBURNS, 69-group spectra in fuel pin S/As

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Fig. 9

SERPENT, 69-group spectra in fuel slab S/As

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Fig. 10

MONTEBURNS, 69-group spectra in fuel slab S/As

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Fig. 11

SERPENT, flux along radial direction

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Fig. 12

MONTEBURNS, flux along radial direction

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Fig. 13

SERPENT, flux along axial direction

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Fig. 14

MONTEBURNS, flux along axial direction

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Fig. 15

SERPENT, U235 atomic density versus burn-up

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Fig. 16

MONTEBURNS, U235 atomic density versus burn-up

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Fig. 17

SERPENT, Pu238 atomic density versus burn-up

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Fig. 18

MONTEBURNS, Pu238 atomic density versus burn-up

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Fig. 19

SERPENT, Pu239 atomic density versus burn-up

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Fig. 20

MONTEBURNS, Pu239 atomic density versus burn-up

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Fig. 21

SERPENT, Pu242 atomic density versus burn-up

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Fig. 22

MONTEBURNS, Pu242 atomic density versus burn-up

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Fig. 23

SERPENT, Am241 atomic density versus burn-up

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Fig. 24

MONTEBURNS, Am241 atomic density versus burn-up

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Fig. 25

SERPENT, Am243 atomic density versus burn-up

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Fig. 26

MONTEBURNS, Am243 atomic density versus burn-up

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Fig. 27

SERPENT, Cm244 atomic density versus burn-up

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Fig. 28

MONTEBURNS, Cm244 atomic density versus burn-up

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Fig. 29

SERPENT, Tc99 atomic density versus burn-up

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Fig. 30

MONTEBURNS, Tc99 atomic density versus burn-up

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Fig. 31

SERPENT, U235 fission reaction rate versus burn-up

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Fig. 32

MONTEBURNS, U235 fission reaction rate versus burn-up

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Fig. 33

SERPENT, Cm244 fission reaction rate versus burn-up

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Fig. 34

MONTEBURNS, Cm244 fission reaction rate versus burn-up

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