Exploring the dependence of the dissipative tidal deformability on the equation of state of a neutron star

Tidal interactions in binary neutron star systems allow us to extract information about the equation of state inside a neutron star from gravitational wave observations. We have recently argued that dissipative tidal interactions can be used to probe the viscous properties of the neutron star fluid. In this talk, I will first discuss how dissipative tidal deformability depends on the equation of the state of a neutron star and the source of dissipation inside a neutron star. In particular, I will show how different nuclear processes, such as Urca reactions, the presence of hyperons, and the scattering of electrons, affect the value of the dissipative tidal deformability, and discuss the scaling of the dissipative tidal deformability with the temperature of the neutron star. I will conclude by assessing the potential of future detectors to constrain the temperature and the presence of hyperons inside a neutron star.