Nuclear shell structure at particle drip lines

Dobaczewski, J.; Hamamoto, I.; Nazarewicz, W.; Sheikh, J. A.

doi:10.1103/physrevlett.72.981

Cited by 368 publications

(351 citation statements)

References 18 publications

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“…The description of shell closure and its disappearance for exotic nuclei, the so-called shell quenching [1,2], is one main issue in each nuclear theory. As the number of valence nucleons increases, the shapes of the nuclei tend to turn from a spherical configuration (doubly-magic) to extreme deformations.…”

Section: Introductionmentioning

confidence: 99%

Mass measurements on neutron-deficient Sr and neutron-rich Sn isotopes with the ISOLTRAP mass spectrometer

et al. 2005

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The atomic masses of 76,77,80,81 Sr and 129,130,131,132 Sn were measured by means of the Penning trap mass spectrometer ISOLTRAP at ISOLDE/CERN. 76 Sr is now the heaviest N = Z nucleus for which the mass is measured to a precision better than 35 keV. For the tin isotopes in the close vicinity of the doubly magic nucleus 132 Sn, mass uncertainties below 20 keV were achieved. An atomic mass evaluation was carried out taking other experimental mass values into account by performing a least-squares adjustment. Some discrepancies between older experimental values and the ones reported here emerged and were resolved. The results of the new adjustment and their impact will be presented.

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Section: Introductionmentioning

confidence: 99%

Mass measurements on neutron-deficient Sr and neutron-rich Sn isotopes with the ISOLTRAP mass spectrometer

et al. 2005

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“…At present, efforts are devoted to investigate with such probes highly unstable isotopes at radioactive nuclear beam (RNB) facilities. Since the first experiments [1][2][3][4][5][6], it has been found from analyses of total interaction cross sections that weakly-bound neutron-rich light nuclei, e.g., 6,8 He, 11 Li,14 Be, 17,19 B, have increased sizes that deviate substantially from the R ∼ A 1/3 rule. It was realized (e.g., Refs.…”

Section: Introductionmentioning

confidence: 99%

“…It was realized (e.g., Refs. [7][8][9]) that such a new phenomenon is due to the weak binding of the last few nucleons which form a diffuse nuclear cloud due to quantum-mechanical penetration (the so-called "nuclear halo"). Another effect is that the nucleons can form a "neutron skin" [10] when the neutrons are on average less bound than the protons.…”

Section: Introductionmentioning

confidence: 99%

Charge and matter distributions and form factors of light, medium, and heavy neutron-rich nuclei

et al. 2005

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Results of charge form factors calculations for several unstable neutron-rich isotopes of light, medium, and heavy nuclei (He, Li, Ni, Kr, Sn) are presented and compared to those of stable isotopes in the same isotopic chain. For the lighter isotopes (He and Li) the proton and neutron densities are obtained within a microscopic large-scale shell-model, while for heavier ones Ni, Kr, and Sn the densities are calculated in deformed self-consistent mean-field Skyrme HF+BCS method. We also compare proton densities to matter densities together with their rms radii and diffuseness parameter values. Whenever possible comparison of form factors, densities and rms radii with available experimental data is also performed. Calculations of form factors are carried out both in plane wave Born approximation (PWBA) and in distorted wave Born approximation (DWBA). These form factors are suggested as predictions for the future experiments on the electron-radioactive beam colliders where the effect of the neutron halo or skin on the proton distributions in exotic nuclei is planned to be studied and thereby the various theoretical models of exotic nuclei will be tested.

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“…We have investigated the structure of 8 B in the framework of the Skyrme HartreeFock (SkHF) model which has been used successfully to describe the ground-state properties of both stable [12,13] as well as exotic nuclei [14]. The SkHF method with density-dependent pairing correlation and SLy4 interaction parameters has been successful in reproducing the binding energies and rms radii [14] in the light neutron halo nuclei 6 He, 8 He, 11 Li and 14 Be.…”

Section: Introductionmentioning

confidence: 99%

Structure of⁸B and astrophysicalS₁₇factor

Dhiman

Shyam

2005

J. Phys. G: Nucl. Part. Phys.

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Abstract. Nuclear structure data are of crucial importance in order to address important astrophysical problems such as the origin of chemical elements, the inner working of our Sun, and the evolution of stars. We demonstrate this by investigating the ground state structure of 8 B and 7 Be nuclei within the Skyrme Hartree-Fock framework and by calculating the overlap integral of 8 B and 7 Be wave functions. The latter is used to calculate the astrophysical S factor (S 17 ) for the solar fusion reaction 7 Be(p, γ) 8 B.

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Nuclear shell structure at particle drip lines

Cited by 368 publications

References 18 publications

Mass measurements on neutron-deficient Sr and neutron-rich Sn isotopes with the ISOLTRAP mass spectrometer

Mass measurements on neutron-deficient Sr and neutron-rich Sn isotopes with the ISOLTRAP mass spectrometer

Charge and matter distributions and form factors of light, medium, and heavy neutron-rich nuclei

Structure of⁸B and astrophysicalS₁₇factor

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Nuclear shell structure at particle drip lines

Cited by 368 publications

References 18 publications

Mass measurements on neutron-deficient Sr and neutron-rich Sn isotopes with the ISOLTRAP mass spectrometer

Mass measurements on neutron-deficient Sr and neutron-rich Sn isotopes with the ISOLTRAP mass spectrometer

Charge and matter distributions and form factors of light, medium, and heavy neutron-rich nuclei

Structure of8B and astrophysicalS17factor

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Structure of⁸B and astrophysicalS₁₇factor