A Skyrme parametrization from subnuclear to neutron star densities Part II. Nuclei far from stabilities

Chabanat, E.; Bonche, P.; Haensel, P.; Meyer, J.; Schaeffer, R.

doi:10.1016/s0375-9474(98)00180-8

Cited by 1,936 publications

(1,356 citation statements)

References 61 publications

Supporting

Mentioning

1,326

Contrasting

Unclassified

Order By: Relevance

“…The energy of the atomic nucleus can be expressed by means of an energy density functional [47][48][49][50], containing five parts: the kinetic energy, a Skyrme potential energy functional modeling the strong force in the particle-hole channel, a pairing energy functional, a Coulomb energy functional, and terms to approximately correct for the spurious-motion caused by broken symmetries E = E kin + E Sk + E pairing + E Coulomb + E corr . (1) For the kinetic energy and the Coulomb energy functional comprising a direct term and the exchange term in Slater approximation we use the same expressions as presented in Ref.…”

Section: The Self-consistent Mean-field Methodsmentioning

confidence: 99%

“…(1) For the kinetic energy and the Coulomb energy functional comprising a direct term and the exchange term in Slater approximation we use the same expressions as presented in Ref. [48]. For all parameterizations used throughout this Article, the center-of-mass recoil effect is approximately taken into account by subtracting E corr = k p 2 k /2mA from the total energy, which amounts to an A-dependent renormalization of the nucleon mass.…”

Section: The Self-consistent Mean-field Methodsmentioning

confidence: 99%

“…In Article I, a set of 36 parameterizations for the Skyrme interaction including a zero-range tensor force has been determined using a fitting protocol almost identical to the one used for the SLyx parameterizations [47,48]. These parameterizations, labeled TIJ, systematically cover a wide range of the C J t ≡ −C T t + 1 2 C F t coupling constants of the tensor terms in spherical symmetry, see Articles I and II for further details.…”

Section: F Parameterizationsmentioning

confidence: 99%

See 2 more Smart Citations

Tensor part of the Skyrme energy density functional. III. Time-odd terms at high spin

2012

View full text Add to dashboard Cite

This article extends previous studies on the effect of tensor terms in the Skyrme energy density functional by breaking of time-reversal invariance. We have systematically probed the impact of tensor terms on properties of superdeformed rotational bands calculated within the cranked HartreeFock-Bogoliubov approach for different parameterizations covering a wide range of values for the isoscalar and isovector tensor coupling constants. We analyze in detail the contribution of the tensor terms to the energies and dynamical moments of inertia and study their impact on quasi-particle spectra. Special attention is devoted to the time-odd tensor terms, the effect of variations of their coupling constants and finite-size instabilities.

show abstract

Section: The Self-consistent Mean-field Methodsmentioning

confidence: 99%

Section: The Self-consistent Mean-field Methodsmentioning

confidence: 99%

Section: F Parameterizationsmentioning

confidence: 99%

See 1 more Smart Citation

Tensor part of the Skyrme energy density functional. III. Time-odd terms at high spin

2012

View full text Add to dashboard Cite

show abstract

“…[46,47] is obtained from many body calculations with simple two-nucleon potential. For completeness, we have also considered the AP4 EoS [48] which hosts a three-nucleon potential and Argonne 18 potential with UIX potential;…”

Section: Realistic Equations Of Statementioning

confidence: 99%

The realistic models of relativistic stars in f ( R ) = R + αR ² gravity

Astashenok

Odintsov

Cruz-Dombriz

2017

Class. Quantum Grav.

165

104

View full text Add to dashboard Cite

The realistic models of relativistic stars in f (R) = R + αR 2 gravity In the context of f (R) = R + αR 2 gravity, we study the existence of neutron and quark stars for various α with no intermediate approximation in the system of equations. Analysis shows that for positive α the scalar curvature does not drop to zero at the star surface (as in General Relativity) but exponentially decreases with distance. Also the stellar mass bounded by star surface decreases when the value α increases. Nonetheless distant observers would observe a gravitational mass due to appearance of a so-called gravitational sphere around the star. The non-zero curvature contribution to the gravitational mass eventually is shown to compensate the stellar mass decrease for growing α's. We perform our analysis for several equations of state including purely hadronic configurations as well as hyperons and quark stars. In all cases, we assess that the relation between the parameter α and the gravitational mass weakly depends upon the chosen equation of state. Another interesting feature is the increase of the star radius in comparison with General Relativity for stars with masses close to maximal, whereas for intermediate masses 1.4 − 1.6M⊙ the radius of star depends upon α very weakly. Also the decrease in the mass bounded by star surface may cause the surface redshift to decrease in R 2 -gravity when compared to Einsteinian predictions. This effect is shown to hardly depend upon the observed gravitational mass. Finally, for negative values of α our analysis shows that outside the star the scalar curvature has damped oscillations but the contribution of the gravitational sphere into the gravitational mass increases indefinitely with radial distance putting into question the very existence of such relativistic stars.

show abstract

“…In Fig. 1 we display the self-consistent ground-state densities of 20 Ne, calculated with two widely used functionals that are representative for the two classes of nuclear EDFs: the non-relativistic Skyrme SLy4 [22], and the relativistic functional DD-ME2 [23]. The equilibrium shape of 20 Ne is a prolate, axially symmetric quadrupole ellipsoid.…”

mentioning

confidence: 99%

How atomic nuclei cluster

Ebran

Khan

Nikšić

et al. 2012

Nature

176

244

View full text Add to dashboard Cite

Nucleonic matter displays a quantum liquid structure, but in some cases finite nuclei behave like molecules composed of clusters of protons and neutrons. Clustering is a recurrent feature in light nuclei, from beryllium to nickel. For instance, in 12 C the Hoyle state, crucial for stellar nucleosynthesis, can be described as a nuclear molecule consisting of three alpha-particles. The mechanism of cluster formation, however, has not yet been fully understood. We show that the origin of clustering can be traced back to the depth of the confining nuclear potential. By employing the theoretical framework of energy density functionals that encompasses both cluster and quantum liquid-drop aspects of nuclei, it is shown that the depth of the potential determines the energy spacings between single-nucleon orbitals, the localization of the corresponding wave functions and, therefore, the degree of nucleonic density clustering. Relativistic functionals, in particular, are characterized by deep single-nucleon potentials. When compared to non-relativistic functionals that yield similar ground-state properties (binding energy, deformation, radii), they predict the occurrence of much more pronounced cluster structures. More generally, clustering is considered as a transitional phenomenon between crystalline and quantum liquid phases of fermionic systems.The occurrence of molecular states in atomic nuclei and the formation of clusters of nucleons were already predicted in the 30's by von Weizsäcker and Wheeler [1,2]. Even though the description of nuclear dynamics became predominantly based on the concept of independent nucleons in a mean-field potential, a renewed interest in clustering phenomena in the 60's led to the development of dedicated theoretical methods [3]. Numerous experimental studies have revealed a wealth of data on clustering phenomena in light nuclei [4], and modern theoretical approaches use microscopic models that fully take into account single-nucleon degrees of freedom [5][6][7]. Clustering gives rise to nuclear molecules. For instance, in 12 C the second 0 + state the Hoyle state that plays a critical role in stellar nucleosynthesis, is predicted to display a three-α structure [8,9]. The binding energy of the α-particle, formed from two protons and two neutrons, is much larger than in other light nuclei. Cluster radioactivity [10], discovered in the 80's, is another manifestation of clustering in atomic nuclei. Experimental signatures of clustering are usually indirect. Quasi-molecular resonances are probed by scattering one cluster on another, such as in the 12 C+ 12 C system [4,11], and cluster structures are also discernible in the breakup of nuclei. Evidence has been reported for the formation of clusters in ground and excited states of a number of α-conjugate nuclei [4], that is nuclei with an equal even number of protons and neutrons, from 8 Be to 56 Ni.The mechanism of cluster formation in nuclei has not yet been fully understood. Deformation plays an important role because it removes the degenera...

show abstract

A Skyrme parametrization from subnuclear to neutron star densities Part II. Nuclei far from stabilities

Cited by 1,936 publications

References 61 publications

Tensor part of the Skyrme energy density functional. III. Time-odd terms at high spin

Tensor part of the Skyrme energy density functional. III. Time-odd terms at high spin

The realistic models of relativistic stars in f ( R ) = R + αR ² gravity

How atomic nuclei cluster

Contact Info

Product

Resources

About

A Skyrme parametrization from subnuclear to neutron star densities Part II. Nuclei far from stabilities

Cited by 1,936 publications

References 61 publications

Tensor part of the Skyrme energy density functional. III. Time-odd terms at high spin

Tensor part of the Skyrme energy density functional. III. Time-odd terms at high spin

The realistic models of relativistic stars in f ( R ) = R + αR 2 gravity

How atomic nuclei cluster

Contact Info

Product

Resources

About

The realistic models of relativistic stars in f ( R ) = R + αR ² gravity