A Survey of the Parameter Space of the Compressible Liquid Drop Model as Applied to the Neutron Star Inner Crust

Newton, William; Gearheart, Michael; Li, Bao-An

doi:10.1088/0067-0049/204/1/9

Cited by 115 publications

(125 citation statements)

References 89 publications

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“…A similar relation has been verified recently by the authors of Ref. [60], although a different slope coefficient is obtained, which they attribute to the different method used to determine the transition point.…”

Section: Correlations Between Transition Pressure and Gldm Coefficiensupporting

confidence: 81%

Imprint of the symmetry energy on the inner crust and strangeness content of neutron stars

et al. 2014

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Abstract. In this work we study the effect of the symmetry energy on several properties of neutron stars. First, we discuss its effect on the density, proton fraction and pressure of the neutron star crust-core transition. We show that whereas the first two quantities present a clear correlation with the slope parameter L of the symmetry energy, no satisfactory correlation is seen between the transition pressure and L. However, a linear combination of the slope and curvature parameters at ρ = 0.1 fm −3 is well correlated with the transition pressure.In the second part we analyze the effect of the symmetry energy on the pasta phase. It is shown that the size of the pasta clusters, number of nucleons and the cluster proton fraction depend on the density dependence of the symmetry energy: a small L gives rise to larger clusters. The influence of the equation of state at subsaturation densities on the extension of the inner crust of the neutron star is also discussed. Finally, the effect of the effect of the density dependence of the symmetry energy on the strangeness content of neutron stars is studied in the last part of the work. It is found that charged (neutral) hyperons appear at smaller (larger) densities for smaller values of the slope parameter L. A linear correlation between the radius and the strangeness content of a star with a fixed mass is also found.PACS. 26.60.-c Nuclear matter aspects of neutron stars -21.65.-f Nuclear matter

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Section: Correlations Between Transition Pressure and Gldm Coefficiensupporting

confidence: 81%

Imprint of the symmetry energy on the inner crust and strangeness content of neutron stars

et al. 2014

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“…- (1) Newton et al (2013) strict ourselves to high mass (compactness) NS. We thus add 14 more EoS which are indicated within the Figure. The full set of 18 EoS considered hereafter is listed in Table 2.…”

Section: Model Relationsmentioning

confidence: 99%

Constraining Models of Twin-Peak Quasi-Periodic Oscillations With Realistic Neutron Star Equations of State

Török

Goluchová

Urbanec

et al. 2016

ApJ

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Twin-peak quasi-periodic oscillations (QPOs) are observed in the X-ray power-density spectra of several accreting low-mass neutron star (NS) binaries. In our previous work we have considered several QPO models. We have identified and explored mass-angular-momentum relations implied by individual QPO models for the atoll source 4U 1636-53. In this paper we extend our study and confront QPO models with various NS equations of state (EoS). We start with simplified calculations assuming Kerr background geometry and then present results of detailed calculations considering the influence of NS quadrupole moment (related to rotationally induced NS oblateness) assuming Hartle-Thorne spacetimes. We show that the application of concrete EoS together with a particular QPO model yields a specific mass-angular-momentum relation. However, we demonstrate that the degeneracy in mass and angular momentum can be removed when the NS spin frequency inferred from the X-ray burst observations is considered. We inspect a large set of EoS and discuss their compatibility with the considered QPO models. We conclude that when the NS spin frequency in 4U 1636-53 is close to 580Hz we can exclude 51 from 90 of the considered combinations of EoS and QPO models. We also discuss additional restrictions that may exclude even more combinations. Namely, there are 13 EOS compatible with the observed twin peak QPOs and the relativistic precession model. However, when considering the low frequency QPOs and Lense-Thirring precession, only 5 EOS are compatible with the model.

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“…Neutron star crusts have been studied using phenomenological liquid drop models [43][44][45] and the Thomas-Fermi approximation [46,47]. Nuclear pasta phases resulting from the competition between the Coulomb interaction and nuclear surface tension were also treated in the liquid drop and Thomas-Fermi methods.…”

Section: Introductionmentioning

confidence: 99%

Structure of neutron star crusts from new Skyrme effective interactions constrained by chiral effective field theory

Lim

Holt

2017

Phys. Rev. C

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We investigate the structure of neutron star crusts, including the crust-core boundary, based on new Skyrme mean field models constrained by the bulk-matter equation of state from chiral effective field theory and the ground-state energies of doubly-magic nuclei. Nuclear pasta phases are studied using both the liquid drop model as well as the Thomas-Fermi approximation. We compare the energy per nucleon for each geometry (spherical nuclei, cylindrical nuclei, nuclear slabs, cylindrical holes, and spherical holes) to obtain the ground state phase as a function of density. We find that the size of the Wigner-Seitz cell depends strongly on the model parameters, especially the coefficients of the density gradient interaction terms. We employ also the thermodynamic instability method to check the validity of the numerical solutions based on energy comparisons.

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A Survey of the Parameter Space of the Compressible Liquid Drop Model as Applied to the Neutron Star Inner Crust

Cited by 115 publications

References 89 publications

Imprint of the symmetry energy on the inner crust and strangeness content of neutron stars

Imprint of the symmetry energy on the inner crust and strangeness content of neutron stars

Constraining Models of Twin-Peak Quasi-Periodic Oscillations With Realistic Neutron Star Equations of State

Structure of neutron star crusts from new Skyrme effective interactions constrained by chiral effective field theory

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