Erratum: High-resolution neutron capture and transmission measurements, and the stellar 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>88</mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math>Sr [Phys. Rev. C<b>62</b>, 055803 (2000)]

Koehler, P.; Winters, R. R.; Guber, K. H.; Rauscher, T.; Harvey, J. A.; Raman, S.; Spencer, R.R.; Blackmon, J. C.; Larson, D.C.; Bardayan, D. W.; Lewis, T. A.

doi:10.1103/physrevc.63.049901

Cited by 20 publications

(25 citation statements)

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“…Maxwellian averaged cross section (b) TOF technique Activation method 58 Fe 12.1±1.1 (Käppeler et al, 1983) 13.5±0.7 (Heil et al, 2008c) 59 Co 38±3 (Spencer and Macklin, 1976) 39.6±2.7 (Heil et al, 2008c) (Koehler et al, 2000 6.13±0.18 (Käppeler et al, 1990b) Musgrove et al, 1978) 19.0±0.6 (Käppeler et al, 1990b) Bao et al (2000). …”

Section: Target Isotopementioning

confidence: 99%

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: Target Isotopementioning

confidence: 99%

Thesprocess: Nuclear physics, stellar models, and observations

et al. 2011

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“…The consequences of this background, mainly coming from the neutron scattering in the sample, have been illustrated by Koehler et al [5] in the example of a high resolution TOF measurement on 88 Sr, and further investigated by Plag et al [6], who discussed in detail the various components contributing to the neutron sensitivity and reported on a C 6 D 6 detector with the lowest neutron sensitivity that has ever been achieved. A. Borella et al benchmarked the entire device in ref.…”

Section: Neutron Sensitivitymentioning

confidence: 97%

A new high efficiency array of C₆D₆ detectors for capture cross section measurements at GELINA

Sage

Berthoumieux

Bouland

et al. 2007

Nd2007

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Abstract. Neutron capture cross section measurements at the Geel Electron Linear Accelerator (GELINA) rely on the use of H-free deuterated benzene C 6 D 6 liquid scintillators. A new design of Aluminium canned C 6 D 6 detectors was studied to improve the performances (high gamma efficiency vs. low neutron sensitivity) of the cylindrical previous ones: on the basis of a truncated 5-sides pyramid, the new detectors were developed and tested in Geel, and used in a preliminary capture cross section measurement on 197 Au in a 4 detectors setup.

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“…Although there have been successful calculations incorporating all reaction mechanisms [102,103,104] and explaining differences between resonance and activation measurements [105,106] without modification of the potential, this conceivable complication should be kept in mind. In consequence, it is very important to have measurements directly in the relevant energy range.…”

Section: Transition Regions With Intermediate Level Densitiesmentioning

confidence: 99%

Cross section predictions for hydrostatic and explosive burning

Descouvemont

Rauscher

2006

Nuclear Physics A

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We review different models used for reactions involved in nuclear astrophysics. The reaction rate is defined for resonant as well as for non-resonant processes. For lowdensity nuclei, we describe the DWBA method, the potential model, the R-matrix method, and microscopic cluster models. The statistical model is developed for high-level densities. Details of calculations in the low-and high-density regimes are illustrated with new results concerning transfer reactions and level densities.

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Erratum: High-resolution neutron capture and transmission measurements, and the stellar neutron-capture cross section of88Sr [Phys. Rev. C62, 055803 (2000)]

Cited by 20 publications

References 0 publications

Thesprocess: Nuclear physics, stellar models, and observations

Thesprocess: Nuclear physics, stellar models, and observations

A new high efficiency array of C₆D₆ detectors for capture cross section measurements at GELINA

Cross section predictions for hydrostatic and explosive burning

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Erratum: High-resolution neutron capture and transmission measurements, and the stellar neutron-capture cross section of88Sr [Phys. Rev. C62, 055803 (2000)]

Cited by 20 publications

References 0 publications

Thesprocess: Nuclear physics, stellar models, and observations

Thesprocess: Nuclear physics, stellar models, and observations

A new high efficiency array of C6D6 detectors for capture cross section measurements at GELINA

Cross section predictions for hydrostatic and explosive burning

Contact Info

Product

Resources

About

A new high efficiency array of C₆D₆ detectors for capture cross section measurements at GELINA