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Auchampaugh, G.F.; Halperin, J.; Macklin, R. L.; Howard, W. M.

doi:10.1103/physrevc.12.1126

Cited by 28 publications

(15 citation statements)

References 10 publications

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“…The present result solves the problem of the large difference between the measurements of Auchampaugh et al [23] and of Wagemans et al [22], where stellar cross sections of 690+170 and 227+20 mb at 30 keV were reported, respectively. There is also agreement with the cross section of 224 mb calculated via the statistical model [24].…”

Section: A S Measurementsupporting

confidence: 48%

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Stellar cross sections forS33(n,α)30<

et al. 1995

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The cross section of the S(n, n) Si reaction was measured in a neutron energy spectrum yielding the stellar rate for a thermal energy of kT=25 keV. For the Cl(n, p) S reaction, the experiment was performed in the neutron energy range from 10 to 260 keV. Our new result for S resolves the problem of a large discrepancy between two previous experiments. In case of Cl it could be shown that the (n, cx) channel is negligibly small compared to the (n, p) reaction at s-process conditions. The present results are used for a detailed discussion of a possible s-process origin of the rare neutron-rich isotope S. PACS number(s): 25.40.Ny, 97.10.Cv, 27.30.+t, 29.40.Cs

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Section: A S Measurementsupporting

confidence: 48%

“…The influence of the S(n, n) rate was examined with respect to the four times larger value of [23]. The present cross section leads to a 30% increase in the S abundance due to the reduced recycling to Si.…”

Section: B Results Of the Network Calculationsmentioning

confidence: 97%

Stellar cross sections forS33(n,α)30<

et al. 1995

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“…The production of thin sulfur samples is difficult because sulfur adheres poorly to most materials and sublimates at room temperature in a vacuum [6,9,13]. Previous experiments reported problems related to 33 S loss [6,9]. Six 33 S samples were prepared by the vacuum surface coatings (VSC) group of the Technology Department at CERN.…”

Section: B the Samplesmentioning

confidence: 99%

“…In fact, the research carried out on 33 S(n,α) 30 Si has originally been linked to nuclear astrophysics due to its role in the origin of the neutron-rich isotope 36 S, which remains an open question. The experimental results of Wagemans et al [6] and Auchampaugh et al [9] were applied to explosive scenarios showing a 36 S overproduction in the solar system incompatible with the stellar models. Later, the s-process contribution to the total 36 S abundance was drastically reduced by the 34 S(n,γ ) reaction, which acts as a bottleneck because of its very low stellar cross-section [10].…”

Section: Introductionmentioning

confidence: 99%

Measurement and resonance analysis of the S33(n,α)Si30 cross section at the CERN n_TOF facility in the energy

Praena¹,

Sabaté-Gilarte²,

Porras³

et al. 2018

Phys. Rev. C

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The 33 S(n,α) 30 Si cross section has been measured at the neutron time-of-flight (n_TOF) facility at CERN in the neutron energy range from 10 to 300 keV relative to the 10 B(n,α) 7 Li cross-section standard. Both reactions were measured simultaneously with a set of micromegas detectors. The flight path of 185 m has allowed us to obtain the cross section with high-energy resolution. An accurate description of the resonances has been performed by means of the multilevel multichannel R-matrix code SAMMY. The results show a significantly higher area of the biggest resonance (13.45 keV) than the unique high-resolution (n,α) measurement. The new parametrization of the 13.45-keV resonance is similar to that of the unique transmission measurement. This resonance is a matter of research in neutron-capture therapy. The 33 S(n,α) 30 Si cross section has been studied in previous works because of its role in the production of 36 S in stars, which is currently overproduced in stellar models compared to observations.

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“…The calculation for 34S is based on data from BNL 325 [1]. For 33S only total neutron widths are given [19]. Resonances designed as s-wave resonances with spin J =2 could cause a resonance scattering length b r of about -0.2 fm.…”

Section: Sulfurmentioning

confidence: 99%

Scattering and resonance properties of the interaction of slow neutrons with the isotopes of silicon and sulfur

1979

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Neutron scattering lengths and, partly, absorption and free scattering cross sections were determined for natural silicon and sulfur and for their isotopes with the masses 28, 29, 30, 32, 33 and 34 Transmission experiments with neutrons of 510 geV, 1.26 eV and 5.19 eV energy resulted in data for the absorption and free scattering cross sections of the natural elements Si and S. From all these results a complete set of scattering parameters could be deduced for each nucleus. By comparing these data with resonance parameters we obtained additional information about resonance properties and potential scattering.

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KilovoltS33(n, α0)

Cited by 28 publications

References 10 publications

Stellar cross sections forS33(n,α)30<

Stellar cross sections forS33(n,α)30<

Measurement and resonance analysis of the S33(n,α)Si30 cross section at the CERN n_TOF facility in the energy

Scattering and resonance properties of the interaction of slow neutrons with the isotopes of silicon and sulfur

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