Photon Strength Functions at the Low-Energy Tail of GEDR

Krtička, M.; Bečvář, F.

doi:10.1051/epjconf/20100203002

Cited by 7 publications

(7 citation statements)

References 10 publications

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“…[46], the efficiency corrected ELBE experimental spectra seem to be reasonably consistent with γ-ray spectra coming directly from dicebox simulations with no pygmy dipole resonance, i.e., a resonance structure in f E1 at E γ ≈ 6 MeV. This finding might indicate that the "iterative" method used in Ref.…”

Section: Conclusion On Psfs In 98 Mosupporting

confidence: 73%

Measurement of theMo97(n,γ)reaction with the DANCEγcalorimeter array

et al. 2015

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Spectra of γ rays following the 97 Mo(n, γ) reaction were measured as a function of incident neutron energy with the DANCE (Detector for Advanced Neutron Capture Experiments) array of 160 BaF2 scintillation detectors at the Los Alamos Neutron Science Center using an enriched 97 Mo target. These spectra were used for the assignment of spins of the 97 Mo resonances up to neutron energy En = 1.7 keV, as well as in the study of photon strength functions (PSFs) in 98 Mo. Analysis of the spectra with the nuclear statistical model showed that they can be well reproduced with the same PSF models which well described the γ decay following slow neutron capture in 95 Mo. On the other hand, the spectra are inconsistent with PSFs describing some other experimental data in 98 Mo.

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Section: Conclusion On Psfs In 98 Mosupporting

confidence: 73%

Measurement of theMo97(n,γ)reaction with the DANCEγcalorimeter array

et al. 2015

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“…Neutron-capture experiments often have indicated an overshoot of the Lorentzian over the observed E1 strength at the low-energy tail of the GDR. 100,156,157,158 On the basis of these data theoretical explanations have been proposed to explain the differences. 100,159,160,158 smooth Lorentzian was found consistently and denoted as pygmy dipole resonance (PDR).…”

Section: Electromagnetic Transitionsmentioning

confidence: 99%

“…158 Recent investigations have shown that the E1 strength can be described by Lorentzians for a large range of nuclei 162,163,164. It was also shown that indirect determinations of PDFs are prone to large uncertainties due to the experimental difficulties and some claims of enhancement165,166 at low E γ have been premature.100,158,167,168 However, in some nuclei extra strength at low energy with respect to the The Path to Improved Reaction Rates for Astrophysics 65…”

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confidence: 99%

The Path to Improved Reaction Rates for Astrophysics

Rauscher

2011

Int. J. Mod. Phys. E

144

337

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This review focuses on nuclear reactions in astrophysics and, more specifically, on reactions with light ions (nucleons and α particles) proceeding via the strong interaction. It is intended to present the basic definitions essential for studies in nuclear astrophysics, to point out the differences between nuclear reactions taking place in stars and in a terrestrial laboratory, and to illustrate some of the challenges to be faced in theoretical and experimental studies of those reactions. The discussion revolves around the relevant quantities for astrophysics, which are the astrophysical reaction rates. The sensitivity of the reaction rates to the uncertainties in the prediction of various nuclear properties is explored and some guidelines for experimentalists are also provided.Caminante, son tus huellas el camino, y nada más; Caminante, no hay camino, se hace camino al andar.Al andar se hace camino y al volver la vista atrás se ve la senda que nunca se ha de volver de pisar. Caminante, no hay camino sino estelas en la mar.

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“…The situation below or near the particle separation threshold is illustrated in Figure 2 for 98 Mo [7]: one can see the discrepant results from the different experimental methods used to determine PSFs.…”

Section: Below or Near Particle Thresholdmentioning

confidence: 99%