Develops modified Teukolsky formalism for EMRIs in higher-derivative gravity and computes horizon and infinity fluxes for cubic gravity example.
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Leading-order deviations from general relativity in scalar quasinormal modes of rotating black holes are computed numerically up to dimensionless spins of 0.99 in quadratic-curvature scalar-tensor theories.
Leading-order cubic-curvature corrections to scalar quasinormal modes of black holes with spins up to 0.99M are computed numerically for modes up to l=5 with relative errors below 10^{-4}.
Effective field theory yields model-independent corrections to Kerr black hole quasinormal modes that oscillate logarithmically near extremality, indicating discrete scale invariance.
Higher-curvature terms deform the near-horizon potential of spherically symmetric black holes, producing progressively larger shifts in overtone quasinormal frequencies that remain detectable in ringdown waveforms when the fundamental mode stays close to its GR value.
Massive scalar quasinormal modes in quasi-topological black holes become long-lived as scalar mass grows, while photon-sphere radius, shadow size, and ISCO exhibit moderate deviations from Schwarzschild.
Higher dimensional regular black holes in quasi-topological gravity have suppressed grey-body factors and Hawking radiation compared to singular black holes in general relativity.
Numerical solutions show that leading effective-field-theory corrections to the Kerr metric grow with spin and are largest near extremality.
Theoretical investigation of black hole fragmentation possibilities beyond standard GR constraints, with relevance to primordial black holes and mergers.
A pedagogical review of Love numbers and tidal responses for black holes and compact objects in general relativity and extensions.
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Ringing of rapidly rotating black holes in effective field theory
Leading-order cubic-curvature corrections to scalar quasinormal modes of black holes with spins up to 0.99M are computed numerically for modes up to l=5 with relative errors below 10^{-4}.