Speaker
Description
The transport properties of the high-density matter found in neutron stars affect the gravitational wave signals observed from colliding neutron stars. In particular, the effects of bulk viscosity differ from quark and nuclear matter. I will discuss the general hydrodynamic evolution of relativistic and dense matter near equilibrium. Focussing on the case of unpaired quark matter, I address how recent advances have made it possible to compute the equation of state with sufficient generality---at finite densities, temperatures, and with finite quark mass(es)---within perturbation theory. Lastly, I will display recent results showing how bulk viscous quark matter can be modelled as a two-component viscoelastic fluid, with one of the components dominating the dynamics depending on the temperature regime.