Transport coefficients of nucleon neutron star cores for various nuclear interactions within the Brueckner-Hartree-Fock approach
arXiv:2004.14909 · doi:10.1103/PhysRevD.102.063010
Abstract
We consider the thermal conductivity, shear viscosity, and momentum relaxation rates in the nucleon cores of the neutron stars. We study how the choice of the nuclear interaction and the model for three-body forces may affect these transport coefficients calculated within the Brueckner-Hartree-Fock many-body nuclear theory. We find that at relatively large densities the model dependence of the results is substantial. In addition we provide the analytical approximations which allow to incorporate our results in practical simulations.
18 pages; 17 figures; minor edits to match the accepted version
References in corpus (6)
- Shear viscosity in neutron star cores
- Nucleon effective masses within the Brueckner-Hartree-Fock theory: Impact on stellar neutrino emission
- Shear viscosity of neutron matter from realistic nucleon-nucleon interactions
- Electron-muon heat conduction in neutron star cores via the exchange of transverse plasmons
- Viscosity of neutron star matter and -modes in rotating pulsars
- Dissipative relativistic magnetohydrodynamics of a multicomponent mixture and its application to neutron stars
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- Fermi-liquid view of viscosity in cold and dense nucleon matter