Impact Of Pairing Correlations On The Chemical Composition Of The Inner Crust Of A Neutron Star

Pastore, Alessandro; Shelley, Matthew; Diget, C.A.

doi:10.22323/1.281.0145

Cited by 5 publications

(3 citation statements)

References 25 publications

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“…In Ref. [78], we have shown that the errors are typically one order of magnitude larger than the value estimated in Eq. 19 when semi-classical methods are adopted (i.e.…”

Section: E Summary Of the Sources Of Errormentioning

confidence: 62%

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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“…In Ref. [78], we have shown that the errors are typically one order of magnitude larger than the value estimated in Eq. 19 when semi-classical methods are adopted (i.e.…”

Section: E Summary Of the Sources Of Errormentioning

confidence: 62%

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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show abstract

“…A further simplification is to solve the HF+BCS equations instead of the full HFB equations. Systematic calculations have recently shown that the error on the total energy amounts to a few keV per nucleon at most [59]. The Wigner-Seitz approximation allows for relatively fast numerical computations, but is unreliable in the densest region of the crust due to the appearance of spurious neutron shell effects [60,61,62].…”

Section: Application To Neutron-star Crustsmentioning

confidence: 99%

Entrainment in Superfluid Neutron-Star Crusts: Hydrodynamic Description and Microscopic Origin

Chamel

2017

J Low Temp Phys

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In spite of the absence of viscous drag, the neutron superfluid permeating the inner crust of a neutron star cannot flow freely, and is entrained by the nuclear lattice similarly to laboratory superfluid atomic gases in optical lattices. The role of entrainment on the neutron superfluid dynamics is reviewed. For this purpose, a minimal hydrodynamical model of superfluidity in neutron-star crusts is presented. This model relies on a fully four-dimensionally covariant action principle. The equivalence of this formulation with the more traditional approach is demonstrated. In addition, the different treatments of entrainment in terms of dynamical effective masses or superfluid density are clarified. The nuclear energy density functional theory employed for the calculations of all the necessary microscopic inputs is also reviewed, focusing on superfluid properties. In particular, the microscopic origin of entrainment and the different methods to estimate its importance are discussed.

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“…The neutronisation of matter leads to the production of very neutron rich nuclei. The process continues until the drip-line is reached and neutrons start dripping off forming a uniform gas [3,4,5,6,7,8,9]. This region of the star is called the inner crust.…”

Section: Introductionmentioning

confidence: 99%

Impact of error analysis on the composition the outer crust of a neutron star

Neill

Medler

Pastore

et al. 2020

J. Phys.: Conf. Ser.

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By means of bootstrap technique, we perform a full error analysis on the Duflo-Zucker mass model. We illustrate the impact of such study on the predicted chemical composition of the outer crust of a non-accreting neutron star. We define an existence probability for each nuclear species as a function of the depth of the crust. We observe that, due to statistical uncertainties, instead of having a well defined transition between two successive layers, we have a mixture of two species.

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Impact Of Pairing Correlations On The Chemical Composition Of The Inner Crust Of A Neutron Star

Cited by 5 publications

References 25 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

Entrainment in Superfluid Neutron-Star Crusts: Hydrodynamic Description and Microscopic Origin

Impact of error analysis on the composition the outer crust of a neutron star

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