Speaker
Описание
Abstract
Extreme-mass-ratio inspirals (EMRIs) provide a unique opportunity to investigate gravitational dynamics in the strong-field regime of rotating black holes and to test general relativity through precision gravitational-wave measurements. Owing to their long-lived orbital evolution, even weak non-vacuum interactions or localized dissipative processes can accumulate into coherent gravitational-wave phase deviations. An important unresolved question is whether such effects can be distinguished from standard Kerr inspiral waveforms and how they influence the reliability of gravitational-wave parameter estimation. In this talk, we investigate the gravitational-wave signatures of localized dissipative transitions in circular, equatorial EMRIs around Kerr black holes. Using Teukolsky-based energy-flux data within an adiabatic relativistic inspiral framework, we introduce a finite-width localized correction to the dissipative evolution and quantify its influence on orbital phase accumulation and waveform morphology. The resulting signals are analyzed using detector-weighted inner products appropriate to the Laser Interferometer Space Antenna (LISA), with particular emphasis on waveform mismatches, coherent residuals, and degeneracies with the intrinsic Kerr parameters. For a representative system with a central black-hole mass of (2\times10^5 M_\odot), a secondary mass of (1.4M_\odot), and a dimensionless spin of (0.9), we find that a weak localized dissipative perturbation produces a non-negligible accumulated phase shift. At a reference signal-to-noise ratio of 30, the time-and-phase-optimized waveform mismatch reaches (4.83\times10^{-3}), while the detector-weighted residual signal-to-noise ratio is approximately 2.95. A subsequent intrinsic-parameter refit substantially reduces the mismatch but shifts the inferred masses and spin. A restricted zero-noise profile-likelihood analysis further demonstrates that waveform deformations can remain largely degenerate with nearby Kerr templates while producing nontrivial parameter-estimation systematics. These findings highlight an important distinction between waveform similarity and the reliability of precision gravitational-wave inference. They motivate more complete EMRI waveform models incorporating localized dissipative physics and provide a general framework for investigating potential signatures of compact-matter transitions, environmental interactions, and non-vacuum dynamics in future space-based gravitational-wave observations. Keywords: Extreme-mass-ratio inspirals; Kerr spacetime; Gravitational waves; Dissipative transitions; Black-hole perturbation theory; LISA; Parameter estimation.
Links
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