Transport coefficients of dense matter in the liquid metal regime

Nandkumar, Radha; Pethick, C. J.

doi:10.1093/mnras/209.3.511

Cited by 93 publications

(78 citation statements)

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“…Calculations of the shear viscosity for the liquid phase were done by Flowers & Itoh [146, 147] and Nandkumar & Pethick [300]. Recently, calculations of the shear viscosity of the neutron star crust were done for both the liquid and the crystal phases, by Chugunov & Yakovlev [101]; their results are displayed in Figure 56.…”

Section: Conductivity and Viscositymentioning

confidence: 99%

Physics of Neutron Star Crusts

Chamel

Haensel

2008

Living Rev. Relativ.

661

789

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The physics of neutron star crusts is vast, involving many different research fields, from nuclear and condensed matter physics to general relativity. This review summarizes the progress, which has been achieved over the last few years, in modeling neutron star crusts, both at the microscopic and macroscopic levels. The confrontation of these theoretical models with observations is also briefly discussed.

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Section: Conductivity and Viscositymentioning

confidence: 99%

Physics of Neutron Star Crusts

Chamel

Haensel

2008

Living Rev. Relativ.

661

789

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“…The dominant form of shear viscosity in hot white dwarf stars is expected to be electron scattering with the ion liquid. Nandkumar and Pethick [20] …”

Section: Viscous Dissipationmentioning

confidence: 99%

Stability of ther-modes in white dwarf stars

Lindblom

1999

Phys. Rev. D

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Stability of the r-modes in rapidly rotating white dwarf stars is investigated. Improved estimates of the growth times of the gravitational-radiation driven instability in the r-modes of the observed DQ Her objects are found to be longer (probably considerably longer) than 6 × 10 9 y. This rules out the possibility that the r-modes in these objects are emitting gravitational radiation at levels that could be detectable by LISA. More generally it is shown that the r-mode instability can only be excited in a very small subset of very hot (T 10 6 K), rather massive (M 0.9M⊙) and very rapidly rotating (Pmin ≤ P 1.2Pmin) white dwarf stars. Further, the growth times of this instability are so long that these conditions must persist for a very long time (t 10 9 y) to allow the amplitude to grow to a dynamically significant level. This makes it extremely unlikely that the r-mode instability plays a significant role in any real white dwarf stars.

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“…A critical analysis of the numerical values for the transport coefficients found by different authors was given by Yakovlev and Urpin [5], who also provided useful and simple approximations for the transport coefficients in the degenerate electron regime in terms of the Coulomb logarithm. Nandkumar and Pethick [6] studied the temperature regime above the melting temperature, i.e., where ions form a liquid, showing that the screening of electron-ion interactions can lead to substantial corrections in this case. These calculations agree with those of Itoh et al [7] who also provide useful fitting formulae for the transport coefficient.…”

Section: Pos(mpcs2015)011mentioning

confidence: 99%

“…We next specify the form of the function Φ in the case of conduction as Φ = p p p · Ξ Ξ Ξ(ε), which after substitution in the linearized Boltzmann equation gives 6) where the relaxation time, which depends on electron energy ε, is defined by…”

Section: )mentioning

confidence: 99%

Electrical conductivity tensor of dense plasma in magnetic fields

Harutyunyan¹,

Sedrakian²

2016

Proceedings of the Modern Physics of Compact Stars 2015 — PoS(MPCS2015)

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Electrical conductivity of finite-temperature plasma in neutron star crusts is studied for applications in magneto-hydrodynamical description of compact stars. We solve the Boltzmann kinetic equation in relaxation time approximation taking into account the anisotropy of transport due to the magnetic field, the effects of dynamical screening in the scattering matrix element and correlations among the nuclei. We show that conductivity has a minimum at a non-zero temperature, a low-temperature decrease and a power-law increase with increasing temperature. Selected numerical results are shown for matter composed of carbon, iron, and heavier nuclei present in the outer crusts of neutron star.

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Transport coefficients of dense matter in the liquid metal regime

Cited by 93 publications

References 0 publications

Physics of Neutron Star Crusts

Physics of Neutron Star Crusts

Stability of ther-modes in white dwarf stars

Electrical conductivity tensor of dense plasma in magnetic fields

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