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 neutron star inspirals. Although, the impact of dissipation on the tides are generally considered negligible while modeling the inspiral of binary neutron stars, recent studies shows that fluid dissipation from bulk viscosity of exotic phases(e.g. hyperons and deconfined quark matter) can be significant enough to be detectable using the next generation gravitational wave detectors. 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 as a sum of contributions associated with the star’s free oscillation modes. We compute the effective love number incorporating dissipation and 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 its impact on the orbital evolution. Finally, based on scaling relations of fluid viscosity with orbital frequency we argue whether fluid dissipation can dominate over gravitational radiation reaction and have detectable impact on the gravitational waveform.
