Speaker
Description
Gravitational waves (GWs) from binary neutron star (BNS) mergers offer crucial insights into the Neutron Star (NS) interiors and nuclear physics. The inference of NS properties hinges on the GW waveform, and achieving an accurate description of BNS GWs is a key focus of current research. The leading tidal contribution arises from the f-mode oscillation of the NS, for which the mode frequency is typically much higher than the orbital frequency, and thus adiabatic tidal corrections are considered. However, recent studies indicate that dynamic f-mode corrections during the late inspiral phase can significantly influence the inferred NS properties. In our work, we examine the bias in nuclear physics due to the ignorance of dynamical f-mode tides in GW waveform models, using data from GW170817 and an ensemble of future detectable BNS events. We discuss precision measurements of the NS equation of state (EOS) and nuclear parameters, utilizing data from BNS events detectable by the upgraded LIGO-VIRGO detectors and next-generation detectors. Furthermore, we explore the viscous dissipation of the f-mode in binaries and the tidal heating involving strange matter in the NS interior. This heating in the presence of the strange matter could raise the temperature of the star higher than that of purely nucleonic NSs, potentially making it observable by future GW detectors. We also investigate the impact of compositional g-modes on the BNS signal.
