Nuclear matter in the crust of neutron stars

Gögelein, P.; Müther, H.

doi:10.1103/physrevc.76.024312

Cited by 78 publications

(109 citation statements)

References 34 publications

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“…As discussed in Section II A, this suppresses the effect of the non-physical discretisation of the states in the continuum, hence reducing the associated uncertainty on the HFB total energy to ≈ 1 keV per particle. Although more advanced HFB methods are now available to properly treat continuum states [48][49][50][51][52], it is still unclear if these methods can deal with very large WS cells especially in terms of execution time. We leave this analysis for a forthcoming project.…”

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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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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“…The pasta phase has been studied extensively by static methods such as liquid-drop models [9,[11][12][13], Thomas-Fermi approximations [14,15], and the Hartee-Fock method [16,17] as well as using dynamical approaches like classical [3,4,6,[19][20][21][22][23][24][25] and quantum molecular dynamics simulations [28][29][30][31][32][33][34][35][36] and the time-dependent Hartree-Fock method [26,27]. Although several authors [8,[37][38][39] have studied transport properties of the crust, very few studies employed dynamical approach.…”

Section: Introductionmentioning

confidence: 99%

Transport Properties of the Nuclear Pasta Phase with Quantum Molecular Dynamics

Nandi

Schramm

2018

ApJ

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We study the transport properties of nuclear pasta for a wide range of density, temperature and proton fractions, relevant for different astrophysical scenarios adopting a quantum molecular dynamics model. In particular, we estimate the values of shear viscosity as well as electrical and thermal conductivities by calculating the static structure factor S(q) using simulation data. In the density and temperature range where the pasta phase appears, the static structure factor shows irregular behavior. The presence of a slab phase greatly enhances the peak in S(q). However, the effect of irregularities in S(q) on the transport coefficients is not very dramatic. The values of all three transport coefficients are found to have the same orders of magnitude as found in theoretical calculations for the inner crust matter of neutron stars without the pasta phase and therefore, is in contrast to earlier speculations that a pasta layer might be highly resistive, both thermally and electrically.

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“…Moreover, some of these multidimensional computations suggest more complex structures. We remark that pairing effects [28], electron-screening effects [31,32], and fluctuation-induced displacements of pasta nuclei [33][34][35] have also been taken into account in describing the structure of pasta nuclei.…”

Section: Figmentioning

confidence: 99%

“…Beyond the WS approximation, shell effects on bound and unbound nucleons were considered [21][22][23]; the shell effects on unbound nucleons are often referred to as band effects. On the other hand, multidimensional computations without any assumption of geometrical shape were also performed within the framework of the Thomas-Fermi method [24], the quantum molecular dynamics (QMD) method [25][26][27], and the Hartree-Fock theory [22,[28][29][30], which reproduce the five shapes listed above. Moreover, some of these multidimensional computations suggest more complex structures.…”

Section: Figmentioning

confidence: 99%

Curvature effect on nuclear “pasta”: Is it helpful for gyroid appearance?

2011

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In supernova cores and neutron star crusts, nuclei are thought to deform to rodlike and slablike shapes, which are often called nuclear pasta. We study the equilibrium properties of the nuclear pasta by using a liquid drop model with curvature corrections. It is confirmed that the curvature effect acts to lower the transition densities between different shapes. We also examine the gyroid structure, which was recently suggested as a different type of nuclear pasta by analogy with the polymer systems. The gyroid structure investigated in this paper is approximately formulated as an extension of the periodic minimal surface whose mean curvature vanishes. In contrast to our expectations, we find from the present approximate formulation that the curvature corrections act to slightly disfavor the appearance of the gyroid structure. By comparing the energy corrections in the gyroid phase and the hypothetical phases composed of d-dimensional spheres, where d is a general dimensionality, we show that the gyroid is unlikely to belong to a family of the generalized dimensional spheres.

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Nuclear matter in the crust of neutron stars

Cited by 78 publications

References 34 publications

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

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

Transport Properties of the Nuclear Pasta Phase with Quantum Molecular Dynamics

Curvature effect on nuclear “pasta”: Is it helpful for gyroid appearance?

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