Nuclear energy functional with a surface-peaked effective mass: global properties

We derive a zero-range pseudopotential that includes all possible terms up to sixth order in derivatives. Within the Hartree-Fock approximation, it gives the average energy that corresponds to a quasi-local nuclear Energy Density Functional (EDF) built of derivatives of the one-body density matrix up to sixth order. The direct reference of the EDF to the pseudopotential acts as a constraint that divides the number of independent coupling constants of the EDF by two. This allows, e.g., for expressing the isovector part of the functional in terms of the isoscalar part, or vice versa. We also derive the analogous set of constraints for the coupling constants of the EDF that is restricted by spherical, space-inversion, and time-reversal symmetries.

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“…[19]. Nevertheless, studies of particular higher-order EDF terms have already been performed [20,21].…”

Section: Introductionmentioning

confidence: 99%

Effective pseudopotential for energy density functionals with higher-order derivatives

2011

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“…Here, we introduce a correction term to the Skyrme EDF which leads to a SPEM and increases the average s.p. level density [8]. We hereafter present this correction term and then briefly describe the calculations of β-decay rates carried out consistently in the framework of the Hartree-Fock-CERPA approach.…”

Section: The Mean Field Modelsmentioning

confidence: 99%

“…[8], a surface-peaked effective mass correction to the Skyrme-type Hamiltonian was proposed with the form…”

Section: B Surface-peaked Effective Mass Correctionmentioning

confidence: 99%

“…Mean-field predictions around the Fermi energy are, however, known to suffer from their underestimation of the density of states. In this work, we explore a small correction to the mean field models which increases the density of states around the Fermi energy [8]. Here, we compare the predictions of this model to known experimental values such as β half-lives or collective modes, as a first step before using it for astrophysical applications.…”

Section: Introductionmentioning

confidence: 99%

“…strength which increases exponentially at each iteration of the self-consistent method. It has therefore been tried to include these correlations directly in the mean field, either at the level of the interaction with density-dependent gradient terms [18], or, loosing the relation with an interaction, at the level of the nuclear energy density functional (EDF) so as to produce a surface-peaked effective mass (SPEM) which, at the same time, does not strongly modify the mean field [8]. In this study, we will explore the second approach.…”

Section: Introductionmentioning

confidence: 99%

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Sensitivity ofβ-decay rates to the radial dependence of the nucleon effective mass

et al. 2015

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We analyze the sensitivity of β-decay rates in 78 Ni and 100,132 Sn to a correction term in Skyrme energy-density functionals (EDFs) which modifies the radial shape of the nucleon effective mass. This correction is added on top of several Skyrme parametrizations which are selected from their effective mass properties and predictions about the stability properties of 132 Sn. The impact of the correction on high-energy collective modes is shown to be moderate. From the comparison of the effects induced by the surface-peaked effective mass in the three doubly magic nuclei, it is found that 132 Sn is largely impacted by the correction, while 78 Ni and 100 Sn are only moderately affected. We conclude that β-decay rates in these nuclei can be used as a test of different parts of the nuclear EDF: 78 Ni and 100 Sn are mostly sensitive to the particle-hole interaction through the B(GT) values, while 132 Sn is sensitive to the radial shape of the effective mass. Possible improvements of these different parts could therefore be better constrained in the future.

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Nuclear Equation of State for Compact Stars and Supernovae

Burgio

Fantina

2018

Astrophysics and Space Science Library

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The equation of state (EoS) of hot and dense matter is a fundamental input to describe static and dynamical properties of neutron stars, core-collapse supernovae and binary compact-star mergers. We review the current status of the EoS for compact objects, that have been studied with both ab-initio many-body approaches and phenomenological models. We limit ourselves to the description of EoSs with purely nucleonic degrees of freedom, disregarding the appearance of strange baryonic matter and/or quark matter. We compare the theoretical predictions with different data coming from both nuclear physics experiments and astrophysical observations. Combining the complementary information thus obtained greatly enriches our insight into the dense nuclear matter properties. Current challenges in the description of the EoS are also discussed, mainly focusing on the model dependence of the constraints extracted from either experimental or observational data, the lack of a consistent and rigorous many-body treatment at zero and finite temperature of the matter encountered in compact stars (e.g. problem of cluster formation and extension of the EoS to very high temperatures), the role of nucleonic three-body forces, and the dependence of the direct URCA processes on the EoS.

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Nuclear energy functional with a surface-peaked effective mass: global properties

Cited by 12 publications

References 49 publications

Effective pseudopotential for energy density functionals with higher-order derivatives

Effective pseudopotential for energy density functionals with higher-order derivatives

Sensitivity ofβ-decay rates to the radial dependence of the nucleon effective mass

Nuclear Equation of State for Compact Stars and Supernovae

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