(γ, p) cross sections and isospin splitting of the giant dipole resonance in N = 50 nuclei

Shoda, K.; Miyase, H.; Sugawara, M.; Saito, T.; Oikawa, S.; Suzuki, A.; Uegaki, J.

doi:10.1016/0375-9474(75)90374-7

Cited by 33 publications

(8 citation statements)

References 18 publications

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“…A large enhancement of σ −2 values is found for 45 Sc and 56 Fe and 153 Sm as compared with semi-magic nuclei 51 V and 139 La. If these predictions of f (E γ ) for E γ min → 0 MeV are consistent with experimental findings, reaction rates in nucleosynthesis following rapid-neutron capturethe r-process -may strongly be affected together with the predicted abundances of nuclei [40,[69][70][71].…”

Section: Low-energy Enhancement Of the Photon Strength Functionsupporting

confidence: 60%

How do we infer shell effects at high-excitation energies? A new spectroscopic probe to search for magic numbers

Ngwetsheni

Orce

2019

EPJ Web Conf.

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The nuclear dipole polarizability is mainly governed by the dynamics of the giant dipole resonance and, assuming validity of the brink-Axel hypothesis, has been investigated along with the effects of the low-energy enhancement of the photon strength function for nuclides in medium- and heavy-mass nuclei. Cubic-polynomial fitsto both data sets extrapolated down to a gamma-ray energy of 0.1 MeV show a significantreduction of the nuclear dipole polarizability for semi-magic nuclei, with magic numbers N =28, 50 and 82, which supports shell effects at high-excitation energies in the the quasi-continuum region. This work assigns σ-2 values as sensitive measures of long-range correlations of the nuclear force and provides a new spectroscopic probe to search for “old” and “new” magic numbers at high-excitation energies.

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Section: Low-energy Enhancement Of the Photon Strength Functionsupporting

confidence: 60%

How do we infer shell effects at high-excitation energies? A new spectroscopic probe to search for magic numbers

Ngwetsheni

Orce

2019

EPJ Web Conf.

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“…[33,34] were applied, as well as the requirement that the γSF below S n should be compatible with data from other experiments above S n . It has long been suspected that the neutron strength only accounts for part of the total giant dipole resonance (GDR) strength [46,47]. According to the Thomas-Reiche-Kuhn (TRK) sum rule [48][49][50] for the GDR strength, σ γ (E)dE = 60N Z/A MeV mb, the total strength of the GDR varies little within a given isotopic chain.…”

Section: Formentioning

confidence: 99%

Completing the nuclear reaction puzzle of the nucleosynthesis ofMo92

et al. 2016

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One of the greatest questions for modern physics to address is how elements heavier than iron are created in extreme, astrophysical environments. A particularly challenging part of that question is the creation of the so-called p-nuclei, which are believed to be mainly produced in some types of supernovae. The lack of needed nuclear data presents an obstacle in nailing down the precise site and astrophysical conditions.In this work, we present for the first time measurements on the nuclear level density and average γ strength function of 92 Mo. State-of-the-art p-process calculations systematically underestimate the observed solar abundance of this isotope. Our data provide stringent constraints on the 91 Nb(p, γ) 92 Mo reaction rate, which is the last unmeasured reaction in the nucleosynthesis puzzle of 92 Mo. Based on our results, we conclude that the 92 Mo abundance anomaly is not due to the nuclear physics input to astrophysical model calculations.

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“…The aim of this study is to elucidate the systematics of isospin splitting of the electric dipole giant resonance as predicted by Fallieros and Goulard (1970) and others (e.g. Akyuz and Fallieros 1971) and tentatively reported by Shoda et al (1975). Of additional interest are the deformation effects as the shell is filled.…”

Section: Introductionmentioning

confidence: 81%