benchmark test with oktavian data and comment on kerma factor

Benchmark test with OKTAVIAN data and

Comment on kerma factor

Yukinobu Watanabe

Department of Advanced Energy Engineering Science,

Kyushu University

3nd RCM of CRP on FENDL-3, 6-10 December 2011

Contents

• Action assignment in 2nd RCM : Si and Sn

• Benchmark test using OKTAVIAN data (by C. Konno)

• Comment on KERMA factor in FENDL/MC-2.1 & FENDL/MG-2.1 (from C. Konno)

Assignment-1: Si isotopes

Keep from ENDF/B-VII, but check and consider using the new JENDL evaluation due to unsatisfactory benchmark results.

In summary report from the 2nd RCM; INDC(NDS)-0567 (2010)

C. Konno et al., “Benchmark Test of JENDL-4.0 Based on Integral Experiments at JAEA/FNS” presented at Joint Int. Conf. on Supercomputing in Nuclear Applications + Monte Carlo 2010, October 17-21, 2010, Tokyo, Japan.

JAEA/FNS

FNS SiC TOF Experiment - (1)

10-7

10-6

10-5

10-4

10-6 10-5 10-4 10-3 10-2 10-1 100 101

Expt.ENDF/B-VII.0JEFF-3.1FENDL-2.1JENDL-3.3JENDL-4

Neutron spectra at depth of 279 mm

Neu

tro

n F

lux

[n

/cm

2/L

eth

arg

y/S

ou

rce]

Neutron Energy [MeV]

JAEA/FNS

FNS SiC TOF Experiment - (2)

0.4

0.6

0.8

1.0

1.2

1.4

0 200 400 600

ENDF/B-VII.0JEFF-3.1FENDL-2.1JENDL-3.3JENDL-4

Ca

lc. /

Ex

pt.

Depth in the assembly [mm]

En > 10 MeV

Expt. Error

0.4

0.6

0.8

1.0

1.2

1.4

0 200 400 600


Ca

lc. /

Ex

pt.


0.1 < En < 1 MeV

Expt. Error

0.4

0.6

0.8

1.0

1.2

1.4

0 200 400 600


Ca

lc. /

Ex

pt.


10 < En < 100 keV

Expt. Error

0.4

0.6

0.8

1.0

1.2

1.4

0 200 400 600


Ca

lc. /

Ex

pt.


10 < En < 100 eV

Expt. Error

JAEA/FNS

FNS SiC In-situ Experiment - (3)

0.4

0.6

0.8

1.0

1.2

1.4

0 200 400 600


Ca

lc. /

Ex

pt.


93Nb(n,2n)92mNb

Expt. Error

0.4

0.6

0.8

1.0

1.2

1.4

0 200 400 600


Ca

lc. /

Ex

pt.


27Al(n,)24Na

Expt. Error

0.4

0.6

0.8

1.0

1.2

1.4

0 200 400 600


Ca

lc. /

Ex

pt.


115In(n,n')115mIn

Expt. Error

0.4

0.6

0.8

1.0

1.2

1.4

0 200 400 600


Ca

lc. /

Ex

pt.


197Au(n,)198Au

Expt. Error

JAEA/FNS

FNS SiC In-situ Experiment - (4)

0.4

0.6

0.8

1.0

1.2

1.4

0 200 400 600


Ca

lc. /

Ex

pt.


235U(n,fission)

Expt. Error

0.0

0.5

1.0

1.5

2.0

0 200 400 600


Ca

lc. /

Ex

pt.


-Ray Heating Rate

Expt. Error

Reference : C. Konno et al., “Benchmark Test of JENDL-4.0 Based on Integral Experiments at JAEA/FNS” presented at Joint Int. Conf. on Supercomputing in Nuclear Applications + Monte Carlo 2010, October 17-21, 2010, Tokyo, Japan.

Conclusion on Si

From the result of this benchmark, I cannot find a reasonable reason to adapt JENDL-4.0 instead of ENDF/B-VII. Therefore, it would be better to keep ENDF/B-VII for Si isotopes in FENDL-3.0.

By YW Jan. 18, 2011

Si

FENDL-3 (SLIB2) :ENDF/B-VII.0

0.6

0.8

1.0

1.2

10-1 100 101

Ca

lc. /

Ex

pt.


10-2

10-1

100

101

OKTAVIAN Si 60cm

Expt.JEFF-3.1ENDF-B/VII.0JENDL-3.3JENDL-4.0

Ne

utr

on

Flu

x [

1/le

tha

rgy

/so

urc

e]

JENDL-4 is slightly better than the others.

Assigment-2: Sn isotopes

Isotopic evaluations from RUSFOND files (or JENDL-4 if available) to be joined to TENDL at E > 20 MeV. Otherwise use TENDL only. Action on Watanabe to justify switch to JENDL-4.

In summary report from the 2nd RCM; INDC(NDS)-0567 (2010)

The data of Sn isotopes in RUSFOND are taken from ENDF/B-VII and both data are same.

Sn isotopes

Since there is no integral benchmark test for Sn isotopes, our optimum selection of evaluated library should be based on only comparison of differential data.

Here we focus on g-ray production cross sections, because they are important to estimate the influence of g-ray heating on superconducting coil (Nb3Sn) for nuclear fusion technology.

ENDF/B-VII.0, RUSFOND, TENDL-2010, and JENDL-4.0 are compared with available experimental data.

114Sn(n,g)

115Sn(n,g)

116Sn(n,g)

117Sn(n,g)

118Sn(n,g)

119Sn(n,g)

120Sn(n,g)

122Sn(n,g)

124Sn(n,g)

g-ray emission spectra of natural Sn

Results

JENDL-4.0 is in slightly better agreement with the experimental (n,g) data of 112,114,116Sn than the other evaluations.

All the evaluations for 118,120Sn reproduce the measurements to similar extent.

As for 122,124Sn, JENDL-4.0 is better than RUSFOND (i.e., ENDF/B-VII.0). Thus, as far as the (n,g) cross sections are concerned, the JENDL-4.0 looks superior to RUSFOND and TENDL-2010.

Gamma-ray emission spectra of natural Sn at 4.75 and 13.05 MeV incident energies are shown with JENDL-4 data and measurements. A comparison with TENDL-2010 is also presented. The data of JENDL-4 agrees with the measurements better than that of TENDL-2010.

Conclusion on Sn

I recommend that we should adapt JENDL-4.0 instead of RUSFOND at energies below 20 MeV. Since there is no high energy data of JENDL for Sn isotopes, TENDL-2010 should be connected with JENDL-4.0 at 20 MeV.

By YW Jan. 18, 2011

Contents

• Action assignment in 2nd RCM : Si and Sn

• Benchmark test using OKTAVIAN data (by C. Konno)

• Comment on KERMA factor in FENDL/MC-2.1 & FENDL/MG-2.1 (from C. Konno)

Benchmark Test using OKTAVIAN data

Benchmark test was done by FNS/JAEA using MCNP-5.14 code Presented at 2011 symposium on nuclear data, 16-17 Nov. 2011, Tokai, Japan

Measurement of leakage neutron spectrum from a spherical pile with incident 14 MeV neutrons

Si

FENDL-3 (SLIB2):ENDF/B-VII.0

0.6

0.8

1.0

1.2

10-1 100 101

Ca

lc. /

Ex

pt.


10-2

10-1

100

101

OKTAVIAN Si 60cm


Ne

utr

on

Flu

x [

1/le

tha

rgy

/so

urc

e]

Cu

10-1

100

100 101

Cu 61cm

Expt.JEFF-3.1ENDF-B/VII.0JENDL-3.3JENDL-4.0N

eutr

on

Flu

x [1

/leth

arg

y/s

ou

rce]

0.80.91.01.11.21.3

10-1 100 101

Cal

c. /

Exp

t.


FENDL-3 (SLIB2)ENDF/B-VII

Zr

FENDL-3 (SLIB2):JENDL/HE

10-1

100

100 101

Zr 61cm


Neu

tro

n F

lux

[1/le

thar

gy/

sou

rce]

0.8

1.0

1.2

1.4

10-1 100 101

Cal

c. /

Exp

t.


Nb


10-1

100

101

100 101

Nb 28cmExpt.JEFF-3.1ENDF-B/VII.0JENDL-3.3JENDL-4.0

Neu

tro

n F

lux

[1/le

thar

gy/

sou

rce]

0.8

1.0

1.2

1.4

10-1 100 101

Cal

c. /

Exp

t.


Mo


10-1

100

101

100 101

Mo 60cmExpt.JEFF-3.1ENDF-B/VII.0JENDL-3.3JENDL-4.0

Neu

tro

n F

lux

[1/le

thar

gy/

sou

rce]

0.8

0.9

1.0

1.1

10-1 100 101

Cal

c. /

Exp

t.


W

FENDL-3 (SLIB2):IAEA

10-1

100

101

100 101

W 40cmExpt.JEFF-3.1ENDF-B/VII.0JENDL-3.3JENDL-4.0

Neu

tro

n F

lux

[1/le

thar

gy/

sou

rce]

0.60.70.80.91.01.1

10-1 100 101

Cal

c. /

Exp

t.


Contents

• Reply to assignments in 2nd RCM : Si and Sn

• Benchmark test using OKTAVIAN data

• KERMA factor in FENDL/MC-2.1 & FENDL/MG-2.1

JAEA/FNS

KERMA factor in FENDL/MC-2.1

and FENDL/MG-2.1

JAEA C. Konno

JAEA/FNSNeutron KERMA in FENDL-2.1

Neutron KERMA factors are stored in FENDL/MC-2.1 (ACE file) and FENDL/MG-2.1 (MATXS file), not in FENDL/E-2.1.

Pointwise neutron KERMA factors in FENDL/MC-2.1 are deduced with the energy balance method in the heatr module of the NJOY code. They are used for tally F6 in MCNP.

Two neutron KERMA factors of 175 groups, “heat” and “kerma”, are stored in FENDL/MG-2.1. “heat” is deduced with the energy balance method in NJOY heatr, while “kerma” is deduced with the kinematic method in NJOY heatr. Note that “kerma” is an upper limit of KERMA and that “heat” should be less than “kerma”. They are extracted with the TRANSX code and are used as response data for heating calculation with Sn codes.

JAEA/FNSProblem in Neutron KERMA in FENDL-2.1

As well known, the energy balance method gives inadequate KERMA, e.g. negative KERMA, if the total energy is not conserved inside nuclear data. In this case the kinematic method should be adopted.

This problem appears in 28 nuclei of FENDL/MC-2.1 (see next slides). - Au-197, Bi-209, Fe-56, Ga-nat, Mn-55, Mo-92, Mo-

94, Mo-95, Mo-96, Mo-97, Mo-98, Mo-100, N-14, Nb-93, P-31, Sn-nat, Ta-181, Ti-46, Ti-47, Ti-48, Ti-49, Ti-50, V-nat, W-182, W-183, W-184, W-186, Zn-96

We would like to propose that this problem should be resolved in FENDL/MC-3.0.

JAEA/FNS

Inadequate KERMA in FENDL-2.1 -(1)

10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101

Energy balance (MATXS)Kinematic (MATXS)ACE

KE

RM

A f

acto

r [M

eV b

arn

]

Neutron energy [MeV]

Au-19710-7

10-6

10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Bi-209

10-6

10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Fe-5610-5

10-3

10-1

101

103

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Ga-nat

JAEA/FNS


10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Mn-5510-7

10-5

10-3

10-1

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Mo-92

10-7

10-6

10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Mo-9410-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Mo-95

JAEA/FNS


10-6

10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Mo-9610-6

10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Mo-97

10-6

10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Mo-9810-6

10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Mo-100

JAEA/FNS


10-3

10-2

10-1

100

101

102

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


N-1410-6

10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Nb-93

10-6

10-5

10-4

10-3

10-2

10-1

100

101

102

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


P-3110-6

10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Sn-nat

JAEA/FNS


10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Ta-18110-5

10-4

10-3

10-2

10-1

100

101

102

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Ti-46

10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Ti-4710-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Ti-48

JAEA/FNS


10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Ti-4910-6

10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Ti-50

10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


V-nat10-5

10-4

10-3

10-2

10-1

100

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


W-182

JAEA/FNS


10-5

10-4

10-3

10-2

10-1

100

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


W-18310-6

10-5

10-4

10-3

10-2

10-1

100

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


W-184

10-6

10-5

10-4

10-3

10-2

10-1

100

101

102

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


W-18610-6

10-5

10-4

10-3

10-2

10-1

100

101

10-11 10-9 10-7 10-5 10-3 10-1 101


KE

RM

A f

acto

r [M

eV b

arn

]


Zr-nat

JAEA/FNSProposal concerning neutron KERMA

The energy balance method gives inadequate KERMA, e.g. negative KERMA, if the total energy is not conserved inside nuclear data. In this case the kinematic method should be adopted.

This problem appears in 28 nuclei of FENDL/MC-2.1 :

- Au-197, Bi-209, Fe-56, Ga-nat, Mn-55, Mo-92, Mo-94, Mo-95, Mo-96, Mo-97, Mo-98, Mo-100, N-14, Nb-93, P-31, Sn-nat, Ta-181, Ti-46, Ti-47, Ti-48, Ti-49, Ti-50, V-nat, W-182, W-183, W-184, W-186, Zn-96

This problem should be resolved in processing of FENDL/MC-3.0.

Appendix

114Sn(n,tot)

118Sn(n,tot)

120Sn(n,tot)

benchmark test with oktavian data and comment on kerma factor

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