Erratum: Dynamics of the inner crust of neutron stars: Hydrodynamics, elasticity, and collective modes [Phys. Rev. C 
<b>87</b>
, 055803 (2013)]

Kobyakov, Dmitry; Pethick, C. J.

doi:10.1103/physrevc.94.059902

Cited by 32 publications

(73 citation statements)

References 1 publication

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“…This has previously been applied to the superfluid neutrons in the inner crust of neutron stars [11][12][13]. In the present context, when both neutrons and protons are superfluid, it is natural to treat them symmetrically, as we have done in the text.…”

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confidence: 99%

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Dispersion and decay of collective modes in neutron star cores

et al. 2017

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We calculate the frequencies of collective modes of neutrons, protons and electrons in the outer core of neutron stars. The neutrons and protons are treated in a hydrodynamic approximation and the electrons are regarded as collisionless. The coupling of the nucleons to the electrons leads to Landau damping of the collective modes and to significant dispersion of the low-lying modes. We investigate the sensitivity of the mode frequencies to the strength of entrainment between neutrons and protons, which is not well characterized. The contribution of collective modes to the thermal conductivity is evaluated.

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confidence: 99%

“…In the Appendix we demonstrate that the approach adopted in this paper, where we work in terms of the nucleon momenta per particle in the condensates, is equivalent to the traditional two-fluid formalism [11][12][13], where one works in terms of the momentum per particle in the neutron condensate and the velocity of the charged particles.…”

Section: Introductionmentioning

confidence: 99%

Dispersion and decay of collective modes in neutron star cores

et al. 2017

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“…The former has amplitude around the surface region r ≈ 3 − 8 fm of the cluster while the latter does not penetrate into r < 7fm, hence the overlap integral could become small. This might lead to a SPH-LPH coupling weaker than that evaluated in macroscopic approaches [2,[5][6][7][8], where this effect is not taken into account.…”

Section: Dipole Superfluid Phonon Modementioning

confidence: 99%

“…Many of the previous studies of the SPH in the inner crust have been performed in the framework of the macroscopic effective theory or the hydrodynamical approaches [2,[5][6][7][8]. However, inhomogeneity of inner crust matter may affect the character of the SPH and the coupling to the lattice phonon, and therefore nuclear many-body approaches are required to provide microscopic information on SPH in the inner crust.…”

Section: Introductionmentioning

confidence: 99%

“…Aguilera et al [2] pointed out that the SPH may play a role of another heat carrier besides electrons. An important point is that the SPH couples to the lattice phonon (LPH), and the coupling governs mean free path of this mode and the thermal conductivity [2,[5][6][7][8]. The thermal conductivity by SPH can be comparable to that by electrons under strong magnetic field and at low temperature [2].…”

Section: Introductionmentioning

confidence: 99%

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Density Functional Approach to Superfluid Phonon in Inner Crust of Neutron Stars

Inakura

2018

Proceedings of the Workshop on Quarks and Compact Stars 2017 (QCS2017)

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We investigate superfluid phonon emerging in inner crust of neutron stars by means of the nuclear density functional theory. Adopting the Wigner-Seitz approximation and a single spherical cell, we describe low-lying collective excitation with the dipole multipolarity. It is found that the superfluid phonon standing on the low-density neutron superfluid does not penetrate into the interior of the nuclear cluster. This suggests that the coupling between the superfluid phonon and the lattice phonon could be weak, and it may affect the thermal conductivity of inner crust.

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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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Erratum: Dynamics of the inner crust of neutron stars: Hydrodynamics, elasticity, and collective modes [Phys. Rev. C 87 , 055803 (2013)]

Cited by 32 publications

References 1 publication

Dispersion and decay of collective modes in neutron star cores

Dispersion and decay of collective modes in neutron star cores

Density Functional Approach to Superfluid Phonon in Inner Crust of Neutron Stars

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

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