Abstract

The first detection of a gravitational-wave (GW) signal from a binary neutron star coalescence, known as GW170817 , by the LIGO and Virgo observatories, signified the beginning of a new era in astrophysics. By analysing GW signals from neutron star binaries, using adequate modelling of matter effects, we have constrained the barotropic equation of state (EoS) of cold matter at supranuclear densities found in the neutron-star interior. Recently, a second such event was detected, GW190425 . In this talk I will describe how the analysis on GW data put constraints on the stars’ tidal parameters, radii and EoS and will focus on how we can infer the nature of the final remnants based on GW data alone. I will briefly discuss the prospects of extracting additional information by using observations of EM counterparts and by modelling and analysing the post-merger part of the gravitational waveform.