Publisher's Note: Semi-classical equation of state and specific-heat expressions with proton shell corrections for the inner crust of a neutron star [Phys. Rev. C 77, 065805 (2008)]

Onsi, M.; Dutta, A. K.; Chatri, H.; Goriely, S.; Chamel, Nicolas

doi:10.1103/physrevc.78.059902

Cited by 53 publications

(133 citation statements)

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“…Note, however, that the values for the speeds of collective excitations indicated in Table II are expected to remain essentially the same for temperatures T < ∼ 10 10 K. Indeed, as shown in Ref. [3], thermal effects have a minor impact on the equilibrium composition of neutron-star crusts in this temperature range. However, the crust of a real neutron star may not necessarily be in full thermodynamic equilibrium, as discussed, e.g., in Sec.…”

Section: Microscopic Model For the Inner Crust Of A Neutron Starmentioning

confidence: 99%

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Low-energy collective excitations in the neutron star inner crust

2013

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We study the low-energy collective excitations in the inner crust of the neutron star, where a neutron superfluid coexists with a Coulomb lattice of nuclei. The dispersion relation of the modes is calculated systematically from a microscopic theory including neutron band structure effects.These effects are shown to lead to a strong mixing between the Bogoliubov-Anderson bosons of the neutron superfluid and the longitudinal crystal lattice phonons. In addition, the speed of the transverse shear mode is greatly reduced as a large fraction of superfluid neutrons are entrained by nuclei. Not only does the much smaller velocity of the transverse mode increase the specific heat of the inner crust, it also decreases its electron thermal conductivity. These results may impact our interpretation of the thermal relaxation in accreting neutron stars. Due to strong mixing, the mean free path of the superfluid mode is found to be greatly reduced. Our results for the collective mode dispersion relations and their damping may also have implications for neutron star seismology.

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Section: Microscopic Model For the Inner Crust Of A Neutron Starmentioning

confidence: 99%

“…[3]. The inner crust was assumed to be made of "cold catalyzed matter", i.e., matter in full thermodynamic equilibrium at zero temperature.…”

Section: Microscopic Model For the Inner Crust Of A Neutron Starmentioning

confidence: 99%

Low-energy collective excitations in the neutron star inner crust

2013

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“…The set of these minima describes a path in the (Z, ρ b , R W S ) configuration space, hence defining in details the evolution of the structure of the inner crust of neutron stars from its outmost to its inmost regions. In the current article, we limit ourselves to the zero-temperature case, but the formalism can be extended to include the non-zero temperature case [41,42]. We investigate a region of the baryonic density that spans 0.0004 fm −3 ≤ ρ b ≤ 0.02 fm −3 .…”

Section: The Methodsmentioning

confidence: 99%

A new statistical method for the structure of the inner crust of neutron stars

Pastore¹,

Shelley²,

Baroni³

et al. 2017

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

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We investigated the structure of the low density regions of the inner crust of neutron stars using the Hartree-Fock-Bogoliubov (HFB) model to predict the proton content Z of the nuclear clusters and, together with the lattice spacing, the proton content of the crust as a function of the total baryonic density ρ b . The exploration of the energy surface in the (Z, ρ b ) configuration space and the search for the local minima require thousands of calculations. Each of them implies an HFB calculation in a box with a large number of particles, thus making the whole process very demanding. In this work, we apply a statistical model based on a Gaussian Process Emulator that makes the exploration of the energy surface ten times faster. We also present a novel treatment of the HFB equations that leads to an uncertainty on the total energy of ≈ 4 keV per particle. Such a high precision is necessary to distinguish neighbour configurations around the energy minima.

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“…Third, effects that act over ranges greater than the unit cell are not consistently accommodated in the CLDM; larger scale self-organization of pasta phases and long-wavelength transport effects are all unaccounted for. Many of these problems are eliminated by more sophisticated models such as Thomas-Fermi (TF), Extended TF (ETF) and ETF + Strutinsky Integral (ETFSI) (e.g., Buchler & Barkat 1971;Oyamatsu 1993;Cheng et al 1997;Onsi et al 2008, where the latter includes a self-consistent treatment of shell effects), the 1D or 3D-Hartree-Fock (HF) methods (e.g., Monrozeau et al 2007;Negele & Vautherin 1973;Montani et al 2004;Baldo et al 2005;Magierski & Heenen 2002;Gögelein et al 2008;Newton & Stone 2009, the latter of which relieves the spherical-WS approximation), and quantum molecular dynamics (QMD) methods (Maruyama et al 1998;Horowitz et al 2004;Watanabe et al 2001;Sonoda et al 2007). Certain of these methods are too computationally demanding for the kind of parameter survey we will present, so as a first step will limit ourselves to the CLDM, with a view to expanding the methodology in future.…”

Section: Introductionmentioning

confidence: 99%

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

Newton

Gearheart

2012

ApJS

115

111

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We present a systematic survey of the range of predictions of the neutron star inner crust composition, crust-core transition densities and pressures, and density range of the nuclear "pasta" phases at the bottom of the crust provided by the compressible liquid drop model in light of the current experimental and theoretical constraints on model parameters. Using a Skyrme-like model for nuclear matter, we construct baseline sequences of crust models by consistently varying the density dependence of the bulk symmetry energy at nuclear saturation density, L, under two conditions: (1) that the magnitude of the symmetry energy at saturation density J is held constant, and (2) J correlates with L under the constraint that the pure neutron matter (PNM) equation of state (EoS) satisfies the results of ab initio calculations at low densities. Such baseline crust models facilitate consistent exploration of the L dependence of crustal properties. The remaining surface energy and symmetric nuclear matter parameters are systematically varied around the baseline, and different functional forms of the PNM EoS at sub-saturation densities implemented, to estimate theoretical "error bars" for the baseline predictions. Inner crust composition and transition densities are shown to be most sensitive to the surface energy at very low proton fractions and to the behavior of the sub-saturation PNM EoS. Recent calculations of the energies of neutron drops suggest that the low-proton-fraction surface energy might be higher than predicted in Skyrme-like models, which our study suggests may result in a greatly reduced volume of pasta in the crust than conventionally predicted.

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Publisher's Note: Semi-classical equation of state and specific-heat expressions with proton shell corrections for the inner crust of a neutron star [Phys. Rev. C 77, 065805 (2008)]

Cited by 53 publications

References 0 publications

Low-energy collective excitations in the neutron star inner crust

Low-energy collective excitations in the neutron star inner crust

A new statistical method for the structure of the inner crust of neutron stars

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

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