Neutron-star matter within the energy-density functional theory and neutron-star structure

Fantina, Anthea; Chamel, Nicolas; Goriely, S.

doi:10.1063/1.4909563

Cited by 9 publications

(7 citation statements)

References 54 publications

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“…Although the different states of dense matter encountered in this interval require different types of treatments (as described below, see also Ref. [64]), these calculations are performed using the same EDF. The transitions are thus described selfconsistently.…”

Section: Unified Equations Of State Of Dense Mattermentioning

confidence: 99%

Giant pulsar glitches and the inertia of neutron star crusts

et al. 2016

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Giant pulsar frequency glitches as detected in the emblematic Vela pulsar have long been thought to be the manifestation of a neutron superfluid permeating the inner crust of a neutron star. However, this superfluid has been recently found to be entrained by the crust, and as a consequence it does not carry enough angular momentum to explain giant glitches. The extent to which pulsartiming observations can be reconciled with the standard vortex-mediated glitch theory is studied considering the current uncertainties on dense-matter properties. To this end, the crustal moment of inertia of glitching pulsars is calculated employing a series of different unified dense-matter equations of state.PACS numbers: 95.30. Sf, 26.60.Kp, 97.10.Kc, 97.60.Gb

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Section: Unified Equations Of State Of Dense Mattermentioning

confidence: 99%

Giant pulsar glitches and the inertia of neutron star crusts

et al. 2016

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“…The peculiar prediction of model HFB-22 could be purely accidental. As a matter of fact, in the recent series of Brussels-Montreal mass models [19], HFB-22 (HFB-24) was found to be in worst (best) agreement with various constraints coming from both nuclear physics and astrophysics [27,28]. More importantly, corrections due to electron exchange and polarization are found to be much smaller than the uncertainties related to nuclear masses, as can be seen in Table I.…”

Section: B Nonaccreting Neutron Starsmentioning

confidence: 97%

Electron exchange and polarization effects on electron captures and neutron emissions by nuclei in white dwarfs and neutron stars

Chamel

Fantina

2016

Phys. Rev. D

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International audienceIn dense stellar environments, nuclei may become unstable against electron captures and/or neutronemissions. These processes are of particular importance for determining the internal constitution ofwhite-dwarf cores and neutron-star crusts. In this paper, the role of electron exchange and polarizationeffects is studied. In particular, the instability condition for the onset of electron captures and neutronemissions is extended so as to account for electron exchange and polarization. Moreover, generalanalytical expressions for the corresponding density and pressure are derived. The corrections to theelectron-capture threshold in white-dwarf cores are found to be very small. Likewise, the neutrondripdensity and pressure in the crusts of accreting and nonaccreting neutron stars are only slightlyshifted. Depending on the nuclear mass model employed, electron polarization may change thecomposition of the crust of nonaccreting neutron stars. On the other hand, the current uncertaintiesin the masses of neutron-rich Kr and Sr isotopes are found to be more important than electron exchangeand polarization effects

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“…Further studies on this subject is interesting. In fact, the crust of neutron star with typical density 10 4 g• cm −3 ∼ 10 11 g• cm −3 [38] indicates that the number density of degenerate electrons is about 10 25 cm −3 ∼ 10 31 cm −3 in the fully ionized case (It is believed that the crust is constituted by iron elements). In addition, white dwarfs also have extremely high density FIG.…”

Section: Longitudinal Wave Dispersion Relationmentioning

confidence: 99%

Background Field Method in Thermo Field Dynamics Theory for Wave Propagation in Unmagnetized Spinor QED Plasmas

Wu,

Zhang

2019

Preprint

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In this work, a many body relativistic quantum field theory for the collective modes of spinor quantum electrodynamic theory (QED) plasmas is developed. We introduce the thermo field dynamics into the QED plasma study. The nontrivial background field method is used to take account of the non-perturbativity of background charged plasma particles and radiation field. It is an extension of "Furry picture" which is first introduced by Yuan Shi, et al. [Phys. Rev. A 94, 012124 (2016)] in their scalar QED plasma study. However, their wave function method in evaluating the background field of ideal system is hard to extend to the general many body cases. We propose a classical limit method that most perturbative high energy and quantum many body aspects can be included in a practical way. As an example, the wave propagation in unmagnetized electronpositron plasma is discussed. In the low energy limit case, the well known wave dispersion relations for non-relativistic degenerate plasma are recovered. In addition, mass increase of plasma particles due to the relativity, effective charge decrease due to the vacuum polarization, finite light velocity influence on the dispersion relation, and temperature influence on plasma system are discussed. Besides, new phenomenons including the zero sound of the electron-positron pair plasma and the particle production induced by the plasma oscillation are first reported. At last, the high energy limit case is studied.

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Neutron-star matter within the energy-density functional theory and neutron-star structure

Cited by 9 publications

References 54 publications

Giant pulsar glitches and the inertia of neutron star crusts

Giant pulsar glitches and the inertia of neutron star crusts

Electron exchange and polarization effects on electron captures and neutron emissions by nuclei in white dwarfs and neutron stars

Background Field Method in Thermo Field Dynamics Theory for Wave Propagation in Unmagnetized Spinor QED Plasmas

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