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. In this talk, we discuss how one could potentially probe out-of-equilibrium effects inside a neutron star by modeling the effects of tidal dissipation during the inspiral of a binary neutron star system. To account for dissipative effects such as viscosity, we introduce a new dissipative tidal deformability parameter and show that this term contributes to the gravitational wave phase at the 4th post-Newtonian (PN) order for quasi-circular binaries. This contribution receives a large finite-size enhancement by the stellar compactness, analogous to the case of the tidal deformability, which makes the parameter potentially measurable with ground-based gravitational wave detectors. In this talk, we will discuss our derivation of this result, present the constraints on the dissipative tidal deformability from analyzing the GW170817 data, and discuss how these results can be used to constrain out-of-equilibrium properties of neutron stars.
Zoom link: https://icts-res-in.zoom.us/j/97073757266?pwd=MHlVN3drN0FMbi9OK3ZkeWUwSjJFZz09
Meeting ID: 970 7375 7266
Passcode: 097216