New Magic Number,<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi mathvariant="italic">N</mml:mi><mml:mspace /><mml:mo>=</mml:mo><mml:mspace /><mml:mn>16</mml:mn><mml:mn /></mml:math>, near the Neutron Drip Line

Ozawa, A.; Kobayashi, Toshio; Suzuki, Toshio; Yoshida, Kôichi; Tanihata, I.

doi:10.1103/physrevlett.84.5493

Cited by 516 publications

(372 citation statements)

References 15 publications

Supporting

Mentioning

343

Contrasting

Unclassified

Order By: Relevance

“…Recently, many experimental and theoretical efforts have been devoted to the study of the structure and the reaction mechanisms in nuclei near the drip lines. Modern radioactive ion beam facilities (RIBFs) and experimental detectors reveal several unexpected phenomena in unstable nuclei such as the existence of haloes and skins [7], the modifications of shell closures [8] and the so-called pygmy resonances in electric dipole transitions [9]. The tensor force plays a role, in particular, in the shell evolution of nuclei far from the stability line [10].…”

Section: Introductionmentioning

confidence: 99%

Tensor interaction in mean-field and density functional theory approaches to nuclear structure

Sagawa

Colò

2014

Progress in Particle and Nuclear Physics

View full text Add to dashboard Cite

The importance of the tensor force for nuclear structure has been recognized long ago. Recently, the interest for this topic has been revived by the study of the evolution of nuclear properties far from the stability line. However, in the context of the effective theories that describe medium-heavy nuclei, the role of the tensor force is still debated. This review focuses on ground-state properties like masses and deformation, on single-particle states, and on excited vibrational and rotational modes. The goal is to assess which properties, if any, can bring clear signatures of the tensor force within the mean-field or density functional theory framework. It will be concluded that, while evidences for a clear neutron-proton tensor force exist despite quantitative uncertainties, the role of the tensor force among equal particles is less well established.

show abstract

Section: Introductionmentioning

confidence: 99%

Tensor interaction in mean-field and density functional theory approaches to nuclear structure

Sagawa

Colò

2014

Progress in Particle and Nuclear Physics

View full text Add to dashboard Cite

show abstract

“…[1] and references therein for a recent review. One of the striking features of nuclei close to the drip line is the adjustment of shell gaps, giving rise to different magic numbers [2]. The way shell closures and single-particle properties evolve as functions of the number of nucleons forms one of the greatest challenges to our understanding of the basic features of nuclei, and thereby the stability of matter.…”

mentioning

confidence: 99%

Closed-shell properties ofO24withab initiocoupled-cluster theory

et al. 2011

View full text Add to dashboard Cite

We present a microscopic calculation of spectroscopic factors for neutron and proton removal from 24 O using the coupled-cluster method and a state-of-the-art chiral nucleon-nucleon interaction at next-to-next-to-next-to-leading order. In order to account for the coupling to the scattering continuum we use a Berggren single-particle basis that treats bound, resonant, and continuum states on an equal footing. We report neutron removal spectroscopic factors for the 23 O states J π = 1/2 + , 5/2 + , 3/2 − and 1/2 − , and proton removal spectroscopic factors for the 23 N states 1/2 − and 3/2 − . Our calculations support the accumulated experimental evidence that 24 O is a closed-shell nucleus.PACS numbers: 21.10.Jx, 21.60. De, 21.10.Pc, 31.15.bw, 24.10.Cn Introduction The study of nuclei far from stability is a leading direction in nuclear physics, experimentally and theoretically. It represents a considerable intellectual challenge to our understanding of the stability of matter itself, with potential implications for the synthesis of elements. An important aspect of this research direction is to understand how magic numbers and shells appear and evolve with increasing numbers of neutrons or protons. The structure and properties of barely stable nuclei at the limits of stability, have been demonstrated to deviate dramatically from the established patterns for ordinary and stable nuclei, see Ref.[1] and references therein for a recent review. One of the striking features of nuclei close to the drip line is the adjustment of shell gaps, giving rise to different magic numbers [2]. The way shell closures and single-particle properties evolve as functions of the number of nucleons forms one of the greatest challenges to our understanding of the basic features of nuclei, and thereby the stability of matter.The chain of oxygen isotopes up to 28 O is particularly interesting since these are the heaviest nuclei for which the drip line is well established. Two out of four stable even-even isotopes exhibit a doubly magic nature, namely 22 O (Z=8,N =14) and 24 O (Z=8, N =16). Several recent experiments [3-6] bring evidence that 24 O is the last stable oxygen isotope. This is remarkable, in particular if one considers the fact that the addition of a single proton on top of the Z = 8 closed shell brings the drip line of the fluorine isotopes to 31 F. Recent measurements [3] also suggest that 24 O has a spherical neutron configuration. The isotopes 25−28 O are all believed to be unstable towards neutron emission, even though 28 O is a doubly magic nucleus within the standard shell-model picture. This indicates that the magic number at the neutron drip line for the oxygen isotopes is not at N = 20 but rather at N = 16.Although spectroscopic factors are not observable quantities [9,10], they can be used to address shell closure properties within the context of a given model. Experimentally, spectroscopic factors are defined as the ratio of the observed reaction rate with respect to the same

show abstract

“…Applying the same shift ∆N ≈ 7 or 9 to 232 Th 142 and 238 U 146 , we could assume a new magic number around N = 150 ∼ 160 which may lead to the fourth abundance peak at A = 230 ∼ 240. Actually, in the very light nuclear systems, a new magic number N = 16 was found [28] in careful experimental studies of the neutron separation energies and interaction cross sections of extremely neutron-rich nuclei. Since these possibilities were not taken into account in the present and previous calculations, the deficiency of actinoids might be improved by modernizing nuclear mass formula including such effects.…”

Section: Quest For Nuclear Physics and Astrophysicsmentioning

confidence: 99%

R-process nucleosynthesis in core-collapse supernova explosion

Kajino¹,

Wanajo²,

Mathews³

2002

Nuclear Physics A

View full text Add to dashboard Cite

We study the r-process nucleosynthesis in neutrino-driven winds of gravitational core collapse SNeII. Appropriate physical conditions are found for successful r-process nucleosynthesis, which meet with several features of heavy elements discovered recently in metal-deficient halo stars. We find also several difficulties which are not explained in the present wind models. We discuss quests for new insights in nuclear physics, astrophysics, and astronomy.

show abstract

New Magic Number,N=16, near the Neutron Drip Line

Cited by 516 publications

References 15 publications

Tensor interaction in mean-field and density functional theory approaches to nuclear structure

Tensor interaction in mean-field and density functional theory approaches to nuclear structure

Closed-shell properties ofO24withab initiocoupled-cluster theory

R-process nucleosynthesis in core-collapse supernova explosion

Contact Info

Product

Resources

About