Speaker
Description
Next-generation gravitational-wave detectors are expected to constrain the unknown neutron star equation-of-state from static and dynamical tides in binary inspirals. The impact of dissipation on the tides is generally considered negligible, but recent work suggests that the bulk viscosity of exotic phases (e.g. hyperons and deconfined quark matter) can be significant enough to be detectable using the future instruments. As a step towards developing realistic waveform models, we incorporate dissipation from both gravitational radiation reaction and fluid viscosity in the tidal response of a neutron star expressed as a sum of contributions associated with the star’s free oscillation modes. We compute the effective Love number incorporating dissipation along with the expected ‘tidal lag’ between the induced quadrupole and the external tidal field. We also determine the expected energy loss to heat from fluid dissipation and quantify its impact on the orbital evolution. Finally, based on scaling relations of fluid viscosity with orbital frequency we discuss whether fluid dissipation can dominate over gravitational radiation reaction and thus have detectable impact on the gravitational waveform.
