Systematic analysis of inner crust composition using the extended Thomas-Fermi approximation with pairing correlations

Shelley, Matthew; Pastore, Alessandro

doi:10.1103/physrevc.103.035807

Cited by 13 publications

(9 citation statements)

References 89 publications

(177 reference statements)

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“…It is shown that the proton content of the WS cells is correlated to the soft or stiff character of the slope of the pure neutron matter EoS for low average densities below 0.05 fm −3 . In this region the D1M and D1M* interactions predict a relatively stiff neutron matter EoS, which favors Z = 40 in the minimal energy configuration (see Figure 7 and Table II of [53]) in agreement with the conclusions drawn in [86]. In Figure 8 we show the neutron (red solid line) and proton (blue dashed line) density profiles inside the WS cell at different ρ av in the inner crust calculated with the D1M* interaction.…”

Section: Inner Crustsupporting

confidence: 82%

“…With the increase in the average density some of these shell closures like Z = 28 and 50 are washed away (see the panel with ρ av = 0.07 fm −3 ). A systematic study of the inner crust composition performed using the extended TF approach including pairing correlations with a large set of Skyrme forces has been very recently reported [86]. It is shown that the proton content of the WS cells is correlated to the soft or stiff character of the slope of the pure neutron matter EoS for low average densities below 0.05 fm −3 .…”

Section: Inner Crustmentioning

confidence: 99%

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Unified Equation of State for Neutron Stars Based on the Gogny Interaction

et al. 2021

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The effective Gogny interactions of the D1 family were established by D. Gogny more than forty years ago with the aim to describe simultaneously the mean field and the pairing field corresponding to the nuclear interaction. The most popular Gogny parametrizations, namely D1S, D1N and D1M, describe accurately the ground-state properties of spherical and deformed finite nuclei all across the mass table obtained with Hartree–Fock–Bogoliubov (HFB) calculations. However, these forces produce a rather soft equation of state (EoS) in neutron matter, which leads to predict maximum masses of neutron stars well below the observed value of two solar masses. To remove this limitation, we built new Gogny parametrizations by modifying the density dependence of the symmetry energy predicted by the force in such a way that they can be applied to the neutron star domain and can also reproduce the properties of finite nuclei as good as their predecessors. These new parametrizations allow us to obtain stiffer EoS’s based on the Gogny interactions, which predict maximum masses of neutron stars around two solar masses. Moreover, other global properties of the star, such as the moment of inertia and the tidal deformability, are in harmony with those obtained with other well tested EoSs based on the SLy4 Skyrme force or the Barcelona–Catania–Paris–Madrid (BCPM) energy density functional. Properties of the core-crust transition predicted by these Gogny EoSs are also analyzed. Using these new Gogny forces, the EoS in the inner crust is obtained with the Wigner–Seitz approximation in the Variational Wigner–Kirkwood approach along with the Strutinsky integral method, which allows one to estimate in a perturbative way the proton shell and pairing corrections. For the outer crust, the EoS is determined basically by the nuclear masses, which are taken from the experiments, wherever they are available, or by HFB calculations performed with these new forces if the experimental masses are not known.

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Section: Inner Crustsupporting

confidence: 82%

Section: Inner Crustmentioning

confidence: 99%

Unified Equation of State for Neutron Stars Based on the Gogny Interaction

et al. 2021

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“…Further constraints would be moreover advisable in order to possibly disentangle and recover also the thermal effects connected to the temperature evolution of the pairing correlations, whose importance within this context has been recently addressed (see Refs. [70,71]).…”

Section: Discussionmentioning

confidence: 99%

Finite-temperature infinite matter with effective-field-theory-inspired energy-density functionals

Burrello

Grasso

2022

Eur. Phys. J. A

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Finite-temperature infinite matter is analyzed with the recently introduced effective-field-theory(EFT)-inspired YGLO (Yang–Grasso–Lacroix–Orsay) and ELYO (extended Lee–Yang, Orsay) functionals, which are designed to describe very low-density regimes in symmetric (YGLO) and in pure neutron (YGLO and ELYO) matter. The article deals with neutron matter and aims to verify whether the use of these functionals allows us to correctly incorporate finite-temperature effects. We compare our results for some relevant thermodynamical quantities with the corresponding ones computed with a chosen reference ab-initio model, namely the many-body-perturbation-theory scheme. We validate the reliability of both EFT-inspired functionals at least at rather low densities and not too high temperatures and we discuss the effects related to the effective mass. We conclude that, at the present stage, the ELYO functional, having a higher neutron effective mass around saturation (closer to ab-initio values), allows us to describe finite-temperature properties more satisfactorily, in better agreement with ab-initio predictions up to higher densities and temperatures, compared to YGLO.

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“…Figures 4-6 thus show that it is essential to verify the compatibility with the ab initio calculations down to very low densities to obtain realistic predictions for the properties of the NS crust. Incidentally, Shelley & Pastore (2021), who performed a systematic study of the NS inner-crust composition using several Skyrme functionals, also pointed out the importance of constraining the low-density part of the equation of state. The low-density EFT constraints and the arrows corresponding to the predictions of selected models are the same as in Fig.…”

Section: The Influence Of the Bulk Functionalmentioning

confidence: 99%

Uncertainties in the pasta-phase properties of catalysed neutron stars

Thi

Carreau

Fantina

et al. 2021

A&A

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Context. The interior of a neutron star is expected to exhibit different states of matter. In particular, complex non-spherical configurations known as ‘pasta’ phases may exist at the highest densities in the inner crust, potentially having an impact on different neutron-star phenomena. Aims. We study the properties of the pasta phase and the uncertainties in the pasta observables which are due to our incomplete knowledge of the nuclear energy functional. Methods. To this aim, we employed a compressible liquid-drop model approach with surface parameters optimised either on experimental nuclear masses or theoretical calculations. To assess the model uncertainties, we performed a Bayesian analysis by largely varying the model parameters using uniform priors, and generating posterior distributions with filters accounting for both our present low-density nuclear physics knowledge and high-density neutron-star physics constraints. Results. Our results show that the nuclear physics constraints, such as the neutron-matter equation of state at very low density and the experimental mass measurements, are crucial in determining the crustal and pasta observables. Accounting for all constraints, we demonstrate that the presence of pasta phases is robustly predicted in an important fraction of the inner crust. We estimate the relative crustal thickness associated with pasta phases as Rpasta/Rcrust = 0.128 ± 0.047 and the relative moment of inertia as Ipasta/Icrust = 0.480 ± 0.137. Conclusions. Our findings indicate that the surface and curvature parameters are more influential than the bulk parameters for the description of the pasta observables. We also show that using a surface tension that is inconsistent with the bulk functional leads to an underestimation of both the average values and the uncertainties in the pasta properties, thus highlighting the importance of a consistent calculation of the nuclear functional.

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Systematic analysis of inner crust composition using the extended Thomas-Fermi approximation with pairing correlations

Cited by 13 publications

References 89 publications

Unified Equation of State for Neutron Stars Based on the Gogny Interaction

Unified Equation of State for Neutron Stars Based on the Gogny Interaction

Finite-temperature infinite matter with effective-field-theory-inspired energy-density functionals

Uncertainties in the pasta-phase properties of catalysed neutron stars

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