Nuclear skin and the curvature of the symmetry energy

Raduta, Ad. R.; Gulminelli, F.

doi:10.1103/physrevc.97.064309

Cited by 11 publications

(7 citation statements)

References 74 publications

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“…Closer values between bulk and saturation densities are obtained towards the dripline, where more unbound nuclei tend to have more diluted profiles. Again, these results are in good agreement with previous ETF works [43,44,48,51]. Diffuseness parameters of the proton and neutron density profiles (left) and total bulk density (right) for nuclei in the vacuum as a function of the isospin asymmetry, for the same isotopic chains as in figures 2 and 1, respectively.…”

Section: 22supporting

confidence: 90%

“…The optimal diffusivities are displayed on the left part of figure 3 for the same isotopic chains as in figure 2. As already observed in previous works [48,51], the diffusivities are almost independent of the nuclear mass, but they strongly depend on the isospin, giving the most important contribution to the nuclear skin in the case of light nuclei. This underlines the complexity of the surface tension.…”

Section: 22supporting

confidence: 80%

“…Even in the simplified approximation of spherical symmetry, the resulting equations can only be solved numerically. A simpler approach that has been often employed in the literature [6,32,35,36,47,48], and which has shown to give satisfactory results in spherical symmetry, is to write the densities as parametrized profiles and to perform the minimization with respect to the parameters. We use Fermi-Dirac (FD) profiles:…”

Section: Variational Equationsmentioning

confidence: 99%

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Parametrization of the surface energy in the ETF approximation

Furtado¹,

Gulminelli²

2020

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

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We perform extended Thomas–Fermi calculations in the Wigner–Seitz cell below and above neutron drip with realistic functionals. The resulting energy density is decomposed as a sum of bulk terms and a surface term, and a compressible liquid drop analytical formula is used to fit the surface tension. The effect of curvature terms and neutron skin is studied in detail. A very good reproduction of the microscopic data is obtained using an expression that depends only on the mass and charge of the cluster, showing that the in-medium modifications of the nuclear energy in the presence of an external neutron gas can be effectively accounted for in the isospin dependence of the surface tension. In this first application, aimed at establishing the fitting protocol, we concentrate on the Sly4 energy functional, but the study can be easily generalized to different functionals, and the resulting parametrizations can be used for direct applications in pasta calculations in neutron star crusts and supernova matter.

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Section: 22supporting

confidence: 90%

Section: 22supporting

confidence: 80%

Section: Variational Equationsmentioning

confidence: 99%

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Parametrization of the surface energy in the ETF approximation

Furtado¹,

Gulminelli²

2020

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

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“…The density dependence of symmetry energy C 2 (ρ) around the saturation density can be well expressed in terms of its slope L 0 , curvature K 0 sym and skewness Q 0 sym evaluated at the saturation density (ρ 0 ≃ 0.16 fm −3 ). These quantities have received a great deal of attention in recent times [9][10][11][12][13][14][15]. Another quantity of topical interest is the isovector splitting of effective nucleon masses, ∆m * 0 ( measure of the difference between neutron and proton effective masses) for asymmetric nuclear matter defined at ρ 0 .…”

Section: Introductionmentioning

confidence: 99%

Correlations among symmetry energy elements in Skyrme models

Mondal

Agrawal

et al. 2018

Int. J. Mod. Phys. E

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Motivated by the interrelationships found between the various symmetry energy elements of the energy density functionals (EDF) based on the Skyrme forces, possible correlations among them are explored. A total of 237 Skyrme EDFs are used for this purpose. As some of these EDFs yield values of a few nuclear observables far off from the present acceptable range, studies are done also with a subset of 162 EDFs that comply with a conservative set of constraints on the values of nuclear matter incompressibility coefficient, effective mass of the nucleon and the isovector splitting of effective nucleon masses to see the enhancement of the correlation strength, if any. The curvature parameter K 0 sym and the skewness parameter Q 0 sym of the symmetry energy are found to be very well correlated with the linear combination of the symmetry energy coefficient and its density derivative L0. The isovector splitting of the effective nucleon mass, however, displays a somewhat meaningful correlation with a linear combination of the symmetry energy, its slope and its curvature parameter.

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“…All ensembles of neutron star EOSs constructed with EDFs have allowed, at most, J and L to vary independently. However, there is significant uncertainty in the higher order parameters such as K sym [70,71,72,73]. There has been some limited exploration of J, L, K sym space using a Skyrme EDF [62], but a not a large systematic generation of ensembles of such models.…”

Section: Introductionmentioning

confidence: 99%

Ensembles of unified crust and core equations of state in a nuclear-multimessenger astrophysics environment

Newton,

Balliet,

Budimir

et al. 2021

Preprint

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We present an ensemble of unified neutron star crust and core equations of state, constructed using an extended Skyrme energy density functional through the crust and outer core, and appended by two piecewise polytropes at higher densities. The equations of state are parameterized by the first three coefficients in the density expansion of the symmetry energy J, L and Ksym, the moment of inertia of a 1.338 M star I1.338 and the maximum neutron star mass Mmax. We construct an ensemble with uniform priors on all five parameters, and then apply data filters to the ensemble to explore the effect of combining neutron skin data from PREX with astrophysical measurements of radii and tidal deformabilities from NICER and LIGO/VIRGO. Neutron skins are calculated directly using the EDFs. We demonstrate that both the nuclear data and astrophysical data play a role in constraining crust properties such as the mass, thickness and moment of inertia of the crust and the nuclear pasta layers therein, and that astrophysical data better constrains Ksym than PREX data.

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Nuclear skin and the curvature of the symmetry energy

Cited by 11 publications

References 74 publications

Parametrization of the surface energy in the ETF approximation

Parametrization of the surface energy in the ETF approximation

Correlations among symmetry energy elements in Skyrme models

Ensembles of unified crust and core equations of state in a nuclear-multimessenger astrophysics environment

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