Speaker
Description
Recently, there have been significant advances in the development of eccentric gravitational-wave models, so that multiple eccentric models are now available. Real-event reanalysis with these models revealed evidence of nonzero eccentricity in the black hole-neutron star (BHNS) merger GW200105. Such evidence for eccentricity points to a dynamical formation channel in dense environments, rather than isolated evolution.
In this talk, I am going to present recent simulations of low-mass black hole-neutron star (BHNS) mergers with moderate eccentricities (about 0.1) in the late inspiral. I will directly compare these systems with those from our previous study of quasicircular BHNS in the equal- and near-equal-mass regimes and with current waveform models, laying a foundation for model calibration, especially the tidal-phase contributions. Moreover, I will show how strong magnetic fields affect the behavior of trapped g-mode oscillations in accretion disks, the modulation of the accretion rate, and their observational implications.