Speaker
Description
Extreme mass-ratio inspirals (EMRIs), consisting of a stellar-mass compact object spiraling into a massive black hole, are key targets for space observatories like the recently adopted LISA, TianQin, and Taiji. Together with self-force effects, the smaller companion spin is one of the crucial post-adiabatic terms needed for accurate waveform templates. This work presents the adiabatic, quasi-spherical inspiral of a spinning test body in a Kerr spacetime for the first time. We leverage recent solutions for the motion of spinning test particles to efficiently compute the gravitational fluxes. Next, we implement a numerical scheme to derive the quasi-spherical inspiral trajectories and generate frequency-domain waveforms. Finally, we assess the impact of the secondary spin on the gravitational wave signal. Our results indicate that neglecting the secondary spin induces detectable mismatches in the waveform across much of the parameter space.
Based on https://arxiv.org/abs/2506.20726
