Abstract

In this paper, the validity of the shell-evolution picture is investigated on the basis of shell-model calculations for the atomic mass number 25≲A≲55 neutron-rich nuclei. For this purpose, the so-called SDPF-MU interaction is used. Its central, two-body spin–orbit, and tensor forces are taken from a simple Gaussian force, the M3Y (Michigan 3-range Yukawa) interaction, and a π+ρ meson exchange force, respectively. Carrying out almost a complete survey of the predicted effective single-particle energies, it is confirmed here that the present scheme is quite effective for describing shell evolution in exotic nuclei.

Highlights

  • In Ref. [13], shell evolution is described by an interaction that consists of a simple Gaussian central force and a π + ρ meson exchange tensor force, whose choice is supported by “renormalization persistency” [16]

  • This interaction, named the monopole-based universal interaction, VMU, and its variant were successfully applied to constructing effective interactions for shell-model calculations [17,18], whose focuses were placed on many-body properties, such as the onset of deformation due to the tensor force

  • The aim of the present study is to quantitatively examine to what extent the shell evolution is described by such a simple scheme

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Summary

Introduction

Evolution Driven by Central, Spin-Orbit, and Tensor Forces. Publisher’s Note: MDPI stays neutral with regard to jurisdictional claims in published maps and institutional affiliations. [13], shell evolution is described by an interaction that consists of a simple Gaussian central force and a π + ρ meson exchange tensor force, whose choice is supported by “renormalization persistency” [16] This interaction, named the monopole-based universal interaction, VMU , and its variant were successfully applied to constructing effective interactions for shell-model calculations [17,18], whose focuses were placed on many-body properties, such as the onset of deformation due to the tensor force.

Monopole Matrix Elements
Effective Single-Particle Energies
Comparison to Experimental Data
Proton Shell Evolution
Neutron Shell Evolution
C S or occupation number
Conclusions
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