Determining Dark Matter Properties from Gravitational Wave Observations of Dark Matter Induced Implosions of Neutron Stars and Their Tidal Deformability.

In this work, we explore the capability of future gravitational-wave detectors like the proposed US Cosmic Explorer and the European Einstein Telescope to distinguish between populations of sub-solar mass black-holes formed through dark-matter induced implosions of neutron stars and neutron stars using tidal deformability measurements. If progenitor binaries survive long enough such that dark matter particles, with some interaction cross-section and mass, get accumulated in the core of neutron stars to form a significant mass that can accrete more particles, such neutron stars are expected to collapse and form black-holes in the mass range 1-3 solar masses. In this scenario, we expect to see three kinds of compact binary populations in this mass range - binary neutron stars, binary black-holes, or neutron star - black hole binary systems. We study the tidal deformability distributions and relative rates of these populations to constrain the properties of dark matter particles.