Transport parameters in neutron stars from in-medium NN cross sections

TL;DR

This paper calculates shear viscosity and thermal conductivity of nuclear matter using Brueckner theory, providing insights into neutron star damping timescales based on in-medium nucleon interactions.

Contribution

It offers a comprehensive numerical analysis of transport coefficients in various nuclear matter states with consistent in-medium cross sections and effective masses.

Findings

Transport coefficients vary with baryon density.

Results inform neutron star oscillation damping times.

Consistent in-medium interactions improve accuracy.

Abstract

We present a numerical study of shear viscosity and thermal conductivity of symmetric nuclear matter, pure neutron matter and $\beta$-stable nuclear matter, in the framework of the Brueckner theory. The calculation of in-medium cross sections and nucleon effective masses is performed with a consistent two and three body interaction. The investigation covers a wide baryon density range as requested in the applications to neutron stars. The results for the transport coefficients in $\beta$-stable nuclear matter are used to make preliminary predictions on the damping time scales of non radial modes in neutron stars.