Modeling and detecting resonant tides of exotic compact objects

Quasinormal Modes from Penrose Limits

“…In both cases, it would be valuable to connect more closely and in more generality to the large literature on solutions to the wave equation on a rotating black hole background [89,96,97,115]. This could include using higher-spin fields and making contact to the Teukolsky equation [116], as opposed to the scalar wave equations used here, considering other modifications to the wave equations, as for example in modified theories of gravity or black holes [68,[117][118][119][120][121][122][123][124], the introduction of sources [125,126], investigating how to describe caustics as well as the propagator and scattering on the black hole background more generally [127][128][129][130][131].…”

Resonances, black hole mimickers, and the greenhouse effect: Consequences for gravitational-wave physics

“…Refs. [34,37] studied extreme-mass-ratio inspirals (q < 10 −4 ) around spinning horizonless compact objects (see also [33,35] for non-spinning analysis and [36,53] for hierarchical triple systems). As in our toy-model, the lowfrequency QNMs of the spinning exotic compact object can be resonantly excited during the inspiral, which leads to nonnegligible effects in the waveform that need to be considered for the detection and parameter estimation of these sources.…”

“…It has been pointed out that horizonless compact objects would have low-frequency oscillation modes, which could be excited by orbiting bodies [33][34][35][36][37]. This is in contrast with BHs, whose modes of oscillation are localized close to the photonsphere, where matter on stable orbits cannot exist [38].…”

“…Previous analysis of detectability of resonance-crossing in BH mimickers were done in the frequency domain [33][34][35][36][37]. By definition, the analysis assumes that the field is stationary, and then superposes an adiabatic evolution to evolve the particle in its motion, driven by GW emission.…”

Fuzzballs and observations

“…Next steps Beyond those discussed in this review, there are many other observables accessible within the microstate geometry program that would be interesting for future analysis. For example, resonance effects in the inspiral phase (see section 1.1) are closely related to tidal effects (see sections 4.3 and 5.2) and may lead to effects such as high frequency "glitches" in or a phase shift of the gravitational wave signal [206,207]. Also related is the "tidal heating" effect [208,209,210,211], which affects the energy loss in the inspiral phase and is especially relevant for EMRIs [208,209].…”