What Can We Learn about the Unstable Equation-of-state Branch from Neutron Star Mergers?

Abstract

The equation of state (EOS) of dense strongly interacting matter can be probed by astrophysical observations of neutron stars (NS), such as X-ray detections of pulsars or the measurement of the tidal deformability of NSs during the inspiral stage of NS mergers. These observations constrain the EOS at most up to the density of the maximum-mass configuration, n _TOV , which is the highest density that can be explored by stable NSs for a given EOS. However, under the right circumstances, binary neutron star (BNS) mergers can create a postmerger remnant that explores densities above n _TOV . In this work, we explore whether the EOS above n _TOV can be measured from gravitational-wave or electromagnetic observations of the postmerger remnant. We perform a total of 25 numerical-relativity simulations of BNS mergers for a range of EOSs and find no case in which different descriptions of the matter above n _TOV have a detectable impact on postmerger observables. Hence, we conclude that the EOS above n _TOV can likely not be probed through BNS merger observations for the current and next generation of detectors.

Keywords

• Binary stars
• High energy astrophysics