Speaker
Description
The post-merger phase of binary neutron star (BNS) mergers provides a unique opportunity to probe the equation of state (EOS) of dense matter at finite temperatures and out-of-equilibrium conditions. While current EOS constraints are dominated by cold inspiral signals, the hot and turbulent post-merger remnant encodes additional microphysics that remains unexplored. In this talk, I will present results from full general-relativistic smoothed particle hydrodynamics simulations with SPHINCS_BSSN, implementing parametric models of the thermal EOS. I will show how variations in the thermal sector subtly but detectably alter the post-merger gravitational-wave spectrum and late-time thermal profiles. These effects, potentially observable with third-generation detectors such as Cosmic Explorer and Einstein Telescope, open a new window into constraining dense matter physics beyond the cold EOS.
