Speaker
Description
The nuclear equation of state (EoS) of hot and dense matter plays a crucial role in understanding extreme astrophysical phenomena such as proto-neutron stars and binary neutron star (BNS) mergers. In BNS mergers that do not undergo prompt collapse, the post-merger remnant emits gravitational waves (GWs) with characteristic frequencies that encode valuable information about the underlying nuclear EoS at finite temperature and high density. However, modeling the hot EoS remains challenging due to significant uncertainties in nuclear matter properties.
Recent progress through microscopic calculations, heavy-ion experiments, and astrophysical observations from electromagnetic and gravitational waves provide new insights to constrain the nuclear EoS. In this work, we generate a posterior set of finite temperature EoS employing Non-Linear Relativistic Mean Field Theory consistent with multi-messenger constraints. Using these EoS posteriors, we estimate the dominant post-merger GW peak frequency associated with the quadrupolar oscillations of the hot and rapidly rotating BNS merger remnant. Finally, we discuss the implications of our results for the optimal high-frequency configuration of future high frequency GW detectors.
