Transport properties of dense matter. III - Analytic formulae for thermal conductivity

Flowers, E. G.; Itoh, Naoki

doi:10.1086/159423

Cited by 61 publications

(48 citation statements)

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“…In the limit of m * n = m * p = m n we obtain the viscosity η n which is a factor of ≈ 40 smaller than CL. Using the results of BHY01 for the thermal conductivity of neutrons κ n , derived in the same approximations as our results for η n , we obtain the values of κ n a factor of 2-4 smaller than those given by Flowers and Itoh [6,32]. The nature of this systematic disagreement of our results with the results of Flowers and Itoh is unclear.…”

Section: A Equations Of Statesupporting

confidence: 56%

Shear viscosity in neutron star cores

Shternin¹,

Yakovlev²

2008

Phys. Rev. D

120

264

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We calculate the shear viscosity η ≈ ηeµ +ηn in a neutron star core composed of nucleons, electrons and muons (ηeµ being the electron-muon viscosity, mediated by collisions of electrons and muons with charged particles, and ηn the neutron viscosity, mediated by neutron-neutron and neutronproton collisions). Deriving ηeµ, we take into account the Landau damping in collisions of electrons and muons with charged particles via the exchange of transverse plasmons. It lowers ηeµ and leads to the non-standard temperature behavior ηeµ ∝ T −5/3 . The viscosity ηn is calculated taking into account that in-medium effects modify nucleon effective masses in dense matter. Both viscosities, ηeµ and ηn, can be important, and both are calculated including the effects of proton superfluidity. They are presented in the form valid for any equation of state of nucleon dense matter. We analyze the density and temperature dependence of η for different equations of state in neutron star cores, and compare η with the bulk viscosity in the core and with the shear viscosity in the crust.

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Section: A Equations Of Statesupporting

confidence: 56%

Shear viscosity in neutron star cores

Shternin¹,

Yakovlev²

2008

Phys. Rev. D

120

264

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“…Finally for the thermal conductivity of the hadronic matter, we follow the calculations of [42], and for the quark matter we use the results of [43]. In order to investigate how the difference in the quark cores manifests itself in the thermal evolution, we investigate the cooling of hybrid stars of same mass, but different quark cores.…”

Section: Resultsmentioning

confidence: 99%

Quark core impact on hybrid star cooling

2012

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In this paper we investigate the thermal evolution of hybrid stars, objects composed of a quark matter core, enveloped by ordinary hadronic matter. Our purpose is to investigate how important are the microscopic properties of the quark core to the thermal evolution of the star. In order to do that we use a simple MIT bag model for the quark core, and a relativistic mean field model for the hadronic envelope. By choosing different values for the microscopic parameters (bag constant, strange quark mass, strong coupling constant) we obtain hybrid stars with different quark core properties. We also consider the possibility of color superconductivity in the quark core. With this simple approach, we have found a set of microscopic parameters that lead to a good agreement with observed cooling neutron stars. Our results can be used to obtain clues regarding the properties of the quark core in hybrid stars, and can be used to refine more sophisticated models for the equation of state of quark matter.

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“…Also shown are the limit of the degenerate region (broken line) and the melting curve for neutron star crustal material (e.g. Flowers andItoh 1981, Slattery et a1 1980). The densities correspond to the lowest energy ionic lattice.…”

Section: Strong Field (Pt < Ptf S B)mentioning

confidence: 99%

Magnetic susceptibility of a neutron star crust

Blandford

Hernquist

1982

J. Phys. C: Solid State Phys.

108

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Abstract. The magnetic susceptibility of the degenerate free electrons in the crust of a neutron star is computed for a range of densities, temperatures, and field strengths. It is shown that when the temperature is low enough (typically less than 10' K for densities of about 1O'g and 10" G fields), the susceptibility undergoes large de Haas-van Alphen oscillations. The crust is then unstable to the formation of layers of domains of alternating magnetisation. Associated with these domains are magnetic field fluctuations of a few per cent amplitude and anisotropic magnetostrictive stresses which may be large enough to crumble the crust. It is argued that these domains are unlikely to directly influence the surface properties of the neutron star but may possibly be coupled indirectly to observable effects.

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Transport properties of dense matter. III - Analytic formulae for thermal conductivity

Cited by 61 publications

References 0 publications

Shear viscosity in neutron star cores

Shear viscosity in neutron star cores

Quark core impact on hybrid star cooling

Magnetic susceptibility of a neutron star crust

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