Theoretical aspects of science with radioactive nuclear beams

Dobaczewski, J.; Nazarewicz, W.

doi:10.1098/rsta.1998.0261

Cited by 81 publications

(26 citation statements)

References 154 publications

(246 reference statements)

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“…Understanding the properties of unstable nuclei is one of the most interesting subjects of nuclear physics [1]. It is also important for astrophysics; for example, determination of the precise position of a neutron drip line is crucial for the r-process nucleosynthesis [2].…”

Section: Introductionmentioning

confidence: 99%

Improved microscopic-macroscopic approach incorporating the effects of continuum states

2010

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The Woods-Saxon-Strutinsky method (the microscopic-macroscopic method) combined with the Kruppa prescription for positive-energy levels, which is necessary to treat neutron-rich nuclei, is studied to clarify the reason for its success and to propose improvements for its shortcomings. The reason why the plateau condition is met for the Nilsson model but not for the Woods-Saxon model is understood in a new interpretation of the Strutinsky smoothing procedure as a low-pass filter. Essential features of the Kruppa level density is extracted in terms of the Thomas-Fermi approximation modified to describe spectra obtained from diagonalization in truncated oscillator bases. A method is proposed, which weakens the dependence on the smoothing width by applying the Strutinsky smoothing only to the deviations from a reference level density. The BCS equations are modified for the Kruppa spectrum, which is necessary to treat the pairing correlation properly in the presence of a continuum. The potential depth is adjusted for the consistency between the microscopic and macroscopic Fermi energies. It is shown, with these improvements, that the microscopic-macroscopic method is now capable to reliably calculate binding energies of nuclei far from stability.

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Section: Introductionmentioning

confidence: 99%

Improved microscopic-macroscopic approach incorporating the effects of continuum states

2010

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“…Apart from intrinsic nuclear structure interest, properties of these nuclei are crucial for our understanding of astrophysical processes responsible for cooking of elements in stars. From a theoretical point of view, the major challenge is to achieve a consistent picture of structure and reaction aspects of weakly bound and unbound nuclei, which requires an accurate description of the particle continuum [1]. Here, the tool of choice is the continuum shell model (see Ref.…”

Section: Introductionmentioning

confidence: 99%

Proton-neutron coupling in the Gamow shell model: The lithium chain

2004

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The shell model in the complex k-plane (the so-called Gamow Shell Model) has recently been formulated and applied to structure of weakly bound, neutron-rich nuclei. The completeness relations of Newton and Berggren, which apply to the neutron case, are strictly valid for finite-range potentials. However, for long-range potentials, such as the Coulomb potential for protons, for which the arguments based on the Mittag-Leffler theory do not hold, the completeness still needs to be demonstrated. This has been done in this paper, both analytically and numerically. The generalized Berggren relations are then used in the first Gamow Shell Model study of nuclei having both valence neutrons and protons, namely the lithium chain. The single-particle basis used is that of the Hartree-Fock-inspired potential generated by a finite-range residual interaction. The effect of isospin mixing in excited unbound states is discussed

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“…A large number of theoretical studies have been devoted to exploring the properties of neutron-rich nuclei on the basis of microscopic approaches, such as the HartreeFock-Bogolyubov (HFB) method or the HartreeFock (HF) method [2][3][4][5] implemented with effective forces or relativistic Hartree-Bogolyubov (RHB) theory [6]. The question of whether islands or peninsulas of nuclei stable against the emission of one or two neutrons could exist beyond the neutron drip line has not been specially addressed so far, since it is usually assumed [7] that, beyond the neutron drip line, nuclei cannot be stable against the emission of one or two neutrons. The extensive calculations of the properties of thousands of nuclei in [8] HFB method with effective Gogny forces of the D1S type revealed the unexpected fact of neutron-stability restoration beyond the neutron drip line for nuclei whose (Z, N ) values are close to (60, 130) and (90,190).…”

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confidence: 99%

Peninsulas of the neutron stability of nuclei in the vicinity of neutron magic numbers

et al. 2012

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On the basis of the Hartree-Fock method as implemented with Skyrme forces (Ska, SkM * , Sly4, and SkI2) and with allowance for an axial deformation and nucleon pairing in the Bardeen-CooperSchrieffer approximation, the properties of extremely neutron-rich even-even nuclei were calculated beyond the neutron drip line known earlier from theoretical calculations. It was shown that the chains of isotopes beyond the neutron drip line that contain N = 32, 58, 82, 126, and 184 neutrons form peninsulas of nuclei stable against the emission of one neutron and, in some cases, peninsulas of nuclei stable against the emission of two neutrons. The neutron-and proton-density distributions in nuclei forming stability peninsulas were found to be spherically symmetric. A mechanism via which the stability of nuclei might be restored beyond the neutron drip line was discussed. A comparison with the results of calculations by the Hartree-Fock-Bogolyubov method was performed for long chains of sulfur and gadolinium isotopes up to the neutron drip line.

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Theoretical aspects of science with radioactive nuclear beams

Cited by 81 publications

References 154 publications

Improved microscopic-macroscopic approach incorporating the effects of continuum states

Improved microscopic-macroscopic approach incorporating the effects of continuum states

Proton-neutron coupling in the Gamow shell model: The lithium chain

Peninsulas of the neutron stability of nuclei in the vicinity of neutron magic numbers

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