Neutron capture cross section of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow /><mml:mrow><mml:mn>139</mml:mn></mml:mrow></mml:msup></mml:mrow><mml:mi mathvariant="normal">La</mml:mi></mml:math>

O'Brien, Sean G.; Dababneh, S.; Heil, M.; Käppeler, F.; Plag, R.; Reifarth, R.; Gallino, R.; Pignatari, M.

doi:10.1103/physrevc.68.035801

Cited by 34 publications

(36 citation statements)

References 19 publications

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“…Because La is easily detectable by stellar spectroscopy, it can be used as an indicator for the onset of the s process in low-metallicity stars, which were formed early in galactic history. It is interesting to note that the 139 La cross section was accurately confirmed by independent activation measurements (O'Brien et al, 2003;Winckler et al, 2006). The position of 90 Zr in the s-process reaction chain is exactly located at the matching point between the mass regions dominated by the weak and main s process.…”

Section: Time-of-flight Methodsmentioning

confidence: 83%

Thesprocess: Nuclear physics, stellar models, and observations

et al. 2011

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Nucleosynthesis in the s process takes place in the He burning layers of low mass AGB stars and during the He and C burning phases of massive stars. The s process contributes about half of the element abundances between Cu and Bi in solar system material. Depending on stellar mass and metallicity the resulting s-abundance patterns exhibit characteristic features, which provide comprehensive information for our understanding of the stellar life cycle and for the chemical evolution of galaxies. The rapidly growing body of detailed abundance observations, in particular for AGB and post-AGB stars, for objects in binary systems, and for the very faint metal-poor population represents exciting challenges and constraints for stellar model calculations. Based on updated and improved nuclear physics data for the s-process reaction network, current models are aiming at ab initio solution for the stellar physics related to convection and mixing processes. Progress in the intimately related areas of observations, nuclear and atomic physics, and stellar modeling is reviewed and the corresponding interplay is illustrated by the general abundance patterns of the elements beyond iron and by the effect of sensitive branching points along the sprocess path. The strong variations of the s-process efficiency with metallicity bear also interesting consequences for Galactic chemical evolution.

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Section: Time-of-flight Methodsmentioning

confidence: 83%

Thesprocess: Nuclear physics, stellar models, and observations

et al. 2011

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“…Since the n TOF results cover only part of this spectrum, only the partial contribution to MACS can be accurately determined, as indicated by P-MACS in Table VI. In view of the remaining differences between the n TOF data and JENDL-3.3, the accurate experimental result of the MACS measured at kT = 25 keV with the activation method by O'Brien et al [10] at Forschungszentrum Karlsruhe (FZK) has been considered. The MACS calculated at kT = 25 keV using the n TOF data and the JENDL cross section is 5% higher than the FZK MACS.…”

Section: A Resonance Parametersmentioning

confidence: 99%

“…MACS at 25 keV (in parentheses) is adopted from Ref. [10] and was used for normalization. propagating the errors of the capture cross section used in the folding procedure.…”

Section: A Resonance Parametersmentioning

confidence: 99%

“…Recently, several activation measurements [9][10][11] have provided evidence for substantial systematic uncertainties in the previous TOF data. The serious astrophysical consequences resulting from discrepancies of up to 40% among the experimental data motivated a new capture cross section measurement at the innovative neutron time-of-flight (n TOF) facility at CERN.…”

Section: Introductionmentioning

confidence: 99%

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TheLa139(n,γ) cross section: Key for the onset of the
Terlizzi¹,
Abbondanno²,
Aerts³
et al. 2007
Phys. Rev. C
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The nuclear resonance parameters and the capture cross section of the neutron magic isotope 139 La have been measured relative to 197 Au in the energy range of 0.6 eV to 9 keV at the neutron time-of-flight (n TOF) facility at CERN. We describe the experimental apparatus and the data analysis procedures, which concerned mainly the efficiency correction by means of the pulse height weighting function technique and the determination of different background components. We extracted the resonance parameters and the main nuclear quantities such as the resonance integral RI = 10.8 ± 1.0 b, the average γ widths for s and p waves γ l=0 = 50.7 ± 5.4 meV and γ l=1 = 33.6 ± 6.9 meV, the nuclear level densities D l=0 = 252 ± 22 eV and D l=1 < 250 eV, and the neutron strength functions S 0 = (0.82 ± 0.05) × 10 −4 and S 1 = (0.55 ± 0.04) × 10 −4 . These results represent a significant improvement over previous data. The deduced Maxwellian-averaged capture cross sections are important for the interpretation of the most recent spectroscopic observations in low-metallicity stars.

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“…For example, their measurement yields a value of 106.9±5.3 mb at kT = 5 keV after normalization to the value for 25 keV from Ref. [46].…”

Section: Macs(mb)mentioning

confidence: 99%

Neutron capture reactions near theN=82shell-closure

et al. 2016

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Neutron capture cross-sections have been calculated in nuclei near the N = 82 neutron shell closure. These nuclei are of astrophysical interest, participating in s-process and p-process. A semi-microscopic optical model have been used with the potential being obtained through folding the target density with the DDM3Y nucleon nucleon interaction. Theoretical density values have been calculated in the relativistic mean field approach. The calculated cross-section, as a function of neutron energy, agree reasonably well with experimental measurements. Maxwellian averaged cross-sections, important for astrophysical processes, have been calculated.

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Neutron capture cross section of139La

Cited by 34 publications

References 19 publications

Thesprocess: Nuclear physics, stellar models, and observations

Thesprocess: Nuclear physics, stellar models, and observations

TheLa139(n,γ) cross section: Key for the onset of the
Terlizzi¹,
Abbondanno²,
Aerts³
et al. 2007
Phys. Rev. C
Self Cite

Neutron capture reactions near theN=82shell-closure

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Neutron capture cross section of139La

Cited by 34 publications

References 19 publications

Thesprocess: Nuclear physics, stellar models, and observations

Thesprocess: Nuclear physics, stellar models, and observations

TheLa139(n,γ) cross section: Key for the onset of theTerlizzi1, Abbondanno2, Aerts3 et al. 2007Phys. Rev. CSelf Cite

Neutron capture reactions near theN=82shell-closure

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TheLa139(n,γ) cross section: Key for the onset of the
Terlizzi¹,
Abbondanno²,
Aerts³
et al. 2007
Phys. Rev. C
Self Cite