Transport coefficients of hyperonic neutron star cores

Peter Shternin; Isaac Vidaña

doi:10.3390/universe7060203

paper

Transport coefficients of hyperonic neutron star cores

arXiv:2106.08474 · doi:10.3390/universe7060203

Abstract

We consider transport properties of the hypernuclear matter in neutron star cores. In particular, we calculate the thermal conductivity, the shear viscosity, and the momentum transfer rates for np $Σ^{-} Λ e μ$ composition of dense matter in $β$ --equilibrium for baryon number densities in the range $0.1 - 1$ ~fm $^{- 3}$ . The calculations are based on baryon interactions treated within the framework of the non-relativistic Brueckner-Hartree-Fock theory. Bare nucleon-nucleon (NN) interactions are described by the Argonne v18 phenomenological potential supplemented with the Urbana IX three-nucleon force. Nucleon-hyperon (NY) and hyperon-hyperon (YY) interactions are based on the \new{NSC97e and NSC97a models} of the Nijmegen group. We find that the baryon contribution to transport coefficients is dominated by the neutron one as in the case of neutron star cores containing only nucleons. In particular, we find that neutrons dominate the total thermal conductivity over the whole range of densities explored and that, due to the onset of $Σ^{-}$ which leads to the deleptonization of the neutron star core, they dominate also the shear viscosity in the high density region, in contrast with the pure nucleonic case where the lepton contribution is always the dominant one.

arXiv comment22 pages, 10 figures, accepted in the Universe, the special issue "Fundamental Processes in Neutron Stars and Supernovae"

Transport coefficients of hyperonic neutron star cores

Abstract

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