Improvements and Extensions of the Neutron Cross Section and Fluence Standards

Carlson, A.D.; Pronyaev, V.G.; Capote, R.; Hambsch, F. J.; Käppeler, F.; Lederer, C.; Mannhart, W.; Mengoni, A.; Nelson, R. O.; Plompen, A.; Schillebeeckx, P.; Simakov, S.P.; Talou, P.; Tagesen, S.; Vonach, H.; Vorobyev, A. S.; Wallner, A.

doi:10.1016/j.nds.2014.04.017

Cited by 11 publications

(15 citation statements)

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“…For the resonance analysis reported here, the uncertainty of the gold reference cross section had to be considered though. It is interesting to note that the presently recommended (n,γ ) cross section of 197 Au at keV neutron energies [24] is in pretty good agreement with the previously used evaluation from the ENDF/B-IV data library [25]. Therefore, the (n,γ ) cross sections of the Ne isotopes could be adopted without changes.…”

Section: Cross Section Datasupporting

confidence: 55%

See 1 more Smart Citation

Erratum: Stellar neutron capture cross sections ofNe20,21,22[Phys. Rev. C90, 045804 (2014)]

Heil¹,

Plag²,

Uberseder³

et al. 2015

Phys. Rev. C

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The stellar (n,γ ) cross sections of the Ne isotopes are important for a number of astrophysical quests, i.e., for the interpretation of abundance patterns in presolar material or with respect to the s-process neutron balance in red giant stars. This paper presents resonance studies of experimental data in the keV range, which had not been fully analyzed before. The analyses were carried out with the R-matrix code SAMMY. With these results for the resonant part and by adding the components due to direct radiative capture, improved Maxwellian-averaged cross sections (MACS) could be determined. At kT = 30 keV thermal energy we obtain MACS values of 240 ± 29, 1263 ± 160, and 53.2 ± 2.7 μbarn for

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Section: Cross Section Datasupporting

confidence: 55%

“…At the end of the convective C-burning shell the most abundant isotopes are 16 O, 20 Ne, 23 Na, and 24 Mg. The impact of the new MACS values for the Ne isotopes on the weak s process in massive stars was investigated by means of a 25 M model with an initial metal content Z = 0.02 [46].…”

Section: Massive Starsmentioning

confidence: 99%

Erratum: Stellar neutron capture cross sections ofNe20,21,22[Phys. Rev. C90, 045804 (2014)]

Heil¹,

Plag²,

Uberseder³

et al. 2015

Phys. Rev. C

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“…For the gold reference cross section in the energy range of the 25 keV quasi-MB spectrum we used the new standard value for kT = 30 keV. An evaluation of neutron standards was recently published giving a cross-section value for 197 Au(n, γ ) of (620 ± 11) mb, which was defined as a standard for kT = 30 keV [59,60]. This standard value was normalized to the experimental neutron spectrum resulting in a spectrum-averaged gold cross-section value for the 25 keV quasi-Maxwellian spectrum of 640 ± 11 mb.…”

Section: A Determination Of Neutron Fluencementioning

confidence: 99%

Stellar and thermal neutron capture cross section of Be9

et al. 2019

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The neutron capture cross section of 9 Be for stellar energies was measured via the activation technique using the Karlsruhe Van de Graaff accelerator in combination with accelerator mass spectrometry at the Vienna Environmental Research Accelerator. To characterize the energy region of interest for astrophysical applications, activations were performed in a quasistellar neutron spectrum of kT = 25 keV and for a spectrum at E n = 473 ± 53 keV. Despite the very small cross section, the method used provided the required sensitivity for obtaining fairly accurate results of 10.4 ± 0.6 and 8.4 ± 1.0 μb, respectively. With these data it was possible to constrain the cross section shape up to the first resonances at 622 and 812 keV, thus allowing for the determination of Maxwellian-averaged cross sections at thermal energies between kT = 5 and 100 keV. In addition, we report a new experimental cross section value at thermal energy of σ th = 8.31 ± 0.52 mb.

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“…Another motivation comes from the fact that the first transition in 48 Ti (E γ = 983.5 keV) is investigated in order to establish a possible γ -ray reference cross section for neutron-induced reactions [4][5][6]. Looking in the experimental nuclear reaction database EXFOR [7] we observe that most of the neutron inelastic scattering experiments on the titanium isotopes were performed between 1960 and 1980 in a limited energy range.…”

Section: Introductionmentioning

confidence: 99%

Neutron inelastic cross section measurements for^natTi

et al. 2017

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Abstract.A neutron inelastic scattering experiment was performed at the GELINA (Geel Electron LINear Accelerator) neutron source of the European Commission Joint Research Centre Geel (EC-JRC Geel) with the aim of determining the reaction cross sections for the stable isotopes of natural titanium. A 235 U fission chamber was used to monitor neutrons with energies up to 20 MeV. The GAINS (Gamma Array for Inelastic Neutron Scattering) spectrometer was employed to detect the γ rays resulting from the decay of the excited nuclei. We determined the γ -ray production cross sections of the first transitions in the 46,48,49,50 Ti isotopes. The experimental values were compared with previous reported results and also with theoretical calculations performed with the TALYS 1.8 code using the default input parameters. Uncertainties of around 5% were obtained for the strongest observed transitions.

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Improvements and Extensions of the Neutron Cross Section and Fluence Standards

Cited by 11 publications

References 0 publications

Erratum: Stellar neutron capture cross sections ofNe20,21,22[Phys. Rev. C90, 045804 (2014)]

Erratum: Stellar neutron capture cross sections ofNe20,21,22[Phys. Rev. C90, 045804 (2014)]

Stellar and thermal neutron capture cross section of Be9

Neutron inelastic cross section measurements for^natTi

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Improvements and Extensions of the Neutron Cross Section and Fluence Standards

Cited by 11 publications

References 0 publications

Erratum: Stellar neutron capture cross sections ofNe20,21,22[Phys. Rev. C90, 045804 (2014)]

Erratum: Stellar neutron capture cross sections ofNe20,21,22[Phys. Rev. C90, 045804 (2014)]

Stellar and thermal neutron capture cross section of Be9

Neutron inelastic cross section measurements fornatTi

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Neutron inelastic cross section measurements for^natTi