The accumulation of dark matter particles in neutron star(NS) cores over long timescales could lead to the formation of a mini black hole causing the neutron star causing the NS to destabilize, and eventually implode to form a similarly massive black hole. In this talk, I will discuss the capability of different generations of GW detector networks to differentiate between populations of binary black hole and binary neutron star systems with component masses 1-2 solar masses through the measurement of the effective tidal deformability parameter, and in turn set limits on dark matter properties using the relative abundance of BNS and BBH mergers.
Zoom link: https://icts-res-in.zoom.us/j/89179610280?pwd=RDZ6VlJybUxrdmpsbEp5dzRtM2dpZz09
Meeting ID: 891 7961 0280
Passcode: 212123