Dynamics of the inner crust of neutron stars: Hydrodynamics, elasticity, and collective modes

Kobyakov, Dmitry; Pethick, C. J.

doi:10.1103/physrevc.87.055803

Cited by 53 publications

(34 citation statements)

References 26 publications

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“…The parameter R e , though, will have a strong impact on all calculated frequencies, and a possible reduction of R e , as suggested in Ref. [68], will move all bands up, as shown in the previous section.…”

Section: Frequencies Of the Fundamental Crustal Shear Modementioning

confidence: 68%

“…[20] themselves vary between 0.3 and 0.9 in the density range relevant for the neutron-star inner crust. Furthermore, Kobyakov and Pethick [68] suggested a sizable correction factor of ≈ 0.4 to these values.…”

Section: Shear Modulus and Shear Velocitiesmentioning

confidence: 96%

“…[20]) is only compatible with any observed QPO frequency for very light or very heavy neutron stars. Kobyakov and Pethick [68] suggested that lattice vibrations can reduce R e , and, in the relevant density regime, they found a correction factor of ≈ 0.4. Multiplying R e by a constant correction factor of this magnitude (which is a good approximation in the density range n = 0.01 − 0.06 fm −3 ) leads to a frequency band of 23.5 − 34.6 Hz, which is in very good agreement with the observed 28 − 29 Hz QPO frequencies for all neutron-star masses.…”

Section: Frequencies Of the Fundamental Crustal Shear Modementioning

confidence: 99%

“…The upper boundary of the crust is defined as Γ 0 = 173 [67]. Assuming T = 0 and including electron screening effects [68], µ is given by…”

Section: Shear Modulus and Shear Velocitiesmentioning

confidence: 99%

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Spectrum of shear modes in the neutron-star crust: Estimating the nuclear-physics uncertainties

Tews¹

2017

Phys. Rev. C

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I construct a model of the inner crust of neutron stars using interactions from chiral effective field theory (EFT) in order to calculate its equation of state (EOS), shear properties, and the spectrum of crustal shear modes. I systematically study uncertainties associated with the nuclear physics input, the crust composition, and neutron entrainment, and estimate their impact on crustal shear properties and the shear-mode spectrum. I find that the uncertainties originate mainly in two sources: The neutron-matter EOS and neutron entrainment. I compare the spectrum of crustal shear modes to observed frequencies of quasi-periodic oscillations in the afterglow of giant γ-ray bursts and find that all of these frequencies could be described within uncertainties, which are, however, at present too sizable to infer neutron-star properties from observations.

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Section: Frequencies Of the Fundamental Crustal Shear Modementioning

confidence: 68%

Section: Shear Modulus and Shear Velocitiesmentioning

confidence: 96%

Section: Frequencies Of the Fundamental Crustal Shear Modementioning

confidence: 99%

“…The upper boundary of the crust is defined as Γ 0 = 173 [67]. Assuming T = 0 and including electron screening effects [68], µ is given by…”

Section: Shear Modulus and Shear Velocitiesmentioning

confidence: 99%

See 2 more Smart Citations

Spectrum of shear modes in the neutron-star crust: Estimating the nuclear-physics uncertainties

Tews¹

2017

Phys. Rev. C

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“…Of particular interest for the phenomenology of neutron stars is the hydrodynamical limit, in which case a crustal layer can be considered as a two-fluid system consisting of the unbound neutron superfluid and plasma comprising crustal nuclei and electrons [411][412][413][414][415][416][417][418]. The normal fluid is locked into the motion of the star by the magnetic field.…”

Section: Collective Modes and Entrainmentmentioning

confidence: 99%

Superfluidity in nuclear systems and neutron stars

2019

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Nuclear matter and finite nuclei exhibit the property of superfluidity by forming Cooper pairs. We review the microscopic theories and methods that are being employed to understand the basic properties of superfluid nuclear systems, with emphasis on the spatially extended matter encountered in neutron stars, supernova envelopes, and nuclear collisions. Our survey of quantum many-body methods includes techniques that employ Green functions, correlated basis functions, and Monte Carlo sampling of quantum states. With respect to empirical realizations of nucleonic and hadronic superfluids, this review is focused on progress that has been made toward quantitative understanding of their properties at the level of microscopic theories of pairing, with emphasis on the condensates that exist under conditions prevailing in neutron-star interiors. These include singlet S-wave pairing of neutrons in the inner crust, and, in the quantum fluid interior, singlet-S proton pairing and triplet coupled P -F -wave neutron pairing. Additionally, calculations of weak-interaction rates in neutron-star superfluids within the Green function formalism are examined in detail. We close with a discussion of quantum vortex states in nuclear systems and their dynamics in neutron-star superfluid interiors. PACS. 97.60.Jd Neutron stars -21.65.+f Nuclear matter -47.37.+q Hydrodynamic aspects of superfluidity; quantum fluids -67.85.+d Ultracold gases, trapped gases -74.25.Dw Superconductivity phase diagrams Contents arXiv:1802.00017v4 [nucl-th] 26 Sep 2019 emerge in the interaction part of the Hamiltonian when evaluating Eq. (5) in terms of Bogolyubov operators vanish. Such terms would account for fluctuations in the system, but are beyond the scope of the present mean-field treatment. 4 Note that the variation δ(E − µN )/δn p,↑ , with up and vp held constant, yields the quantity Ep, confirming its interpretation. Armen Sedrakian, John W. Clark: Superfluidity in nuclear systems and neutron stars 5

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Misconceptions on Effective Field Theories and Spontaneous Symmetry Breaking: Response to Ellis’ Article

Luu

Meißner

2020

Found Phys

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In an earlier paper Luu and Meißner (arXiv:1910.13770 [physics.hist-ph]) we discussed emergence from the context of effective field theories, particularly as related to the fields of particle and nuclear physics. We argued on the side of reductionism and weak emergence. George Ellis has critiqued our exposition in Ellis (arXiv:2004.13591 [physics.hist-ph]), and here we provide our response to his critiques. Many of his critiques are based on incorrect assumptions related to the formalism of effective field theories and we attempt to correct these issues here. We also comment on other statements made in his paper. Important to note is that our response is to his critiques made in archive versions arXiv:2004.13591v1-5 [physics.hist-ph]. That is, versions 1–5 of this archive post. Version 6 has similar content as versions 1–5, but versions 7–9 are seemingly a different paper altogether (even with a different title).

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Dynamics of the inner crust of neutron stars: Hydrodynamics, elasticity, and collective modes

Cited by 53 publications

References 26 publications

Spectrum of shear modes in the neutron-star crust: Estimating the nuclear-physics uncertainties

Spectrum of shear modes in the neutron-star crust: Estimating the nuclear-physics uncertainties

Superfluidity in nuclear systems and neutron stars

Misconceptions on Effective Field Theories and Spontaneous Symmetry Breaking: Response to Ellis’ Article

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