{"total":72,"items":[{"citing_arxiv_id":"2605.20320","ref_index":21,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The third wheel: ringdown and lensing of triple systems","primary_cat":"gr-qc","submitted_at":"2026-05-19T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Numerical relativity simulations of triple black hole systems reveal redshift effects and gravitational lensing in ringdown signals from head-on mergers, with no additional black hole formation from amplified waves.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Disks of Active Galactic Nuclei,\" Astrophys. J.964, 61 (2024), arXiv:2310.03832 [astro-ph.HE]. [20] Shu-Cheng Yang, Wen-Biao Han, Hiromichi Tagawa, Song Li, Ye Jiang, Ping Shen, Qianyun Yun, Chen Zhang, and Xing-Yu Zhong, \"Indication for a Com- pact Object Next to a LIGO-Virgo Binary Black Hole Merger,\" Astrophys. J. Lett.988, L41 (2025), arXiv:2401.01743 [astro-ph.HE]. [21] A. G. Abacet al.(LIGO Scientific, Virgo, KAGRA), \"GW241011 and GW241110: Exploring Binary Forma- tion and Fundamental Physics with Asymmetric, High- spin Black Hole Coalescences,\" Astrophys. J. Lett.993, L21 (2025), arXiv:2510.26931 [astro-ph.HE]. [22] Khun Sang Phukon, Patricia Schmidt, Gonzalo Mor- ras, andGeraintPratten,\"DetectionofGW200105with"},{"citing_arxiv_id":"2605.19829","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Hamiltonian formalism, master functions and Darboux transformations for perturbed (interiors and exteriors of) nonrotating black holes","primary_cat":"gr-qc","submitted_at":"2026-05-19T13:24:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The work reviews a Hamiltonian formalism for perturbations of nonrotating black holes, interprets Darboux transformations as canonical transformations, extends the axial-polar correspondence to polar cases, and demonstrates mixing transformations between axial and polar master functions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19121","ref_index":14,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Ringdown Signatures of Dehnen Dark Matter Halos: Fluid Modes and Detectability with Space-Based Detectors","primary_cat":"gr-qc","submitted_at":"2026-05-18T21:15:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Numerical ringdown waveforms for black holes in Dehnen dark matter profiles are generated and analyzed for detectability and parameter inference using second-generation TDI in space-based detectors such as LISA, Taiji, and TianQin.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18595","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Impact of sky localization uncertainty on ringdown inference","primary_cat":"gr-qc","submitted_at":"2026-05-18T16:07:29+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Properly accounting for sky localization uncertainty in ringdown inference widens mode-amplitude posteriors, avoids bias from fixed point estimates, and leaves amplitude ratios robust for Kerr spectroscopy.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.17840","ref_index":4,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Pole Skipping, Avoided Crossing, and Resonant Excitation in Kerr Quasinormal Modes near Algebraically Special Frequencies","primary_cat":"gr-qc","submitted_at":"2026-05-18T04:21:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Kerr QNM anomalies near algebraically special frequencies arise from avoided crossings with resonant excitation and pole skipping due to quasinormal-Matsubara pole-zero cancellations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16492","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dynamical quasinormal mode excitation II: propagation and convergence in Schwarzschild","primary_cat":"gr-qc","submitted_at":"2026-05-15T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Refined propagation prescription for quasinormal modes excited by plunging particles confirms a bounce radius at r_*=0 and yields accurate reproduction of the post-bounce oscillatory waveform component from first principles.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16489","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Bouncing singularities in Schwarzschild: a geometric origin of the QNM convergence region","primary_cat":"gr-qc","submitted_at":"2026-05-15T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Bouncing singularities from null geodesics off the black hole singularity set the convergence region of the QNM expansion for the Schwarzschild retarded Green's function.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16199","ref_index":14,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Detectability of avoided crossings in black hole ringdowns","primary_cat":"gr-qc","submitted_at":"2026-05-15T17:13:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Bayesian analysis finds individual QNM frequencies near avoided crossings hard to resolve even under optimistic conditions, though collective AC waveform signatures may remain detectable if those modes dominate and slower-mode contamination is minimal.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16132","ref_index":254,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Nucleosynthesis in the fast ejecta of a neutron star merger","primary_cat":"astro-ph.HE","submitted_at":"2026-05-15T16:15:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Free neutrons survive r-process freeze-out in fast ejecta of neutron star mergers and their beta-decay heating produces a visible early kilonova precursor for mass fractions above ~0.05.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15429","ref_index":16,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Ringdown and echoes from compact objects: Debye series and Debye quasinormal modes","primary_cat":"gr-qc","submitted_at":"2026-05-14T21:23:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Introduces Debye series and Debye-QNMs to decompose waveforms from Schwarzschild-star models, achieving early-time convergence and organizing ringdown plus echo packets into individual propagation channels.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15271","ref_index":8,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Polarization Analysis of Ringdown Signals","primary_cat":"gr-qc","submitted_at":"2026-05-14T18:00:02+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Constrained polarization model for Kerr ringdown modes enables inclination inference from two-detector data for non-precessing mergers but introduces biases when applied to precessing systems.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.14078","ref_index":21,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Properties of natural polynomials for Schwarzschild and Kerr black holes","primary_cat":"gr-qc","submitted_at":"2026-05-13T20:01:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Natural polynomials for Schwarzschild and Kerr quasinormal modes are Pollaczek-Jacobi polynomials with complex parameters, with recurrence peaking at the physical overtone index for Schwarzschild.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13901","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"On the impossibility of observational confirmation of black holes","primary_cat":"gr-qc","submitted_at":"2026-05-12T18:41:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"No observational data can confirm the existence of black holes because general relativity imposes fundamental limits on what can be established about them.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11890","ref_index":13,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A cosmology-to-ringdown EFT consistency map for scalar-tensor gravity","primary_cat":"gr-qc","submitted_at":"2026-05-12T10:05:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"An EFT consistency map transports cosmology-conditioned posteriors from scalar-tensor FLRW backgrounds to black-hole quasinormal-mode kernels, showing tensor-speed effects fall below ringdown detectability while other operators remain potentially active near black holes.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"post-merger waveform modeling and with next-generation detectors such as Einstein Telescope and LISA [13-17]. At the same time, recent reviews make clear that precision spectroscopy must contend with real theoretical and data-analysis issues - including mode resolvability, nonlinear mode content, and spectral stability - before it can become a precision test of gravity [13, 18]. On the theory side, a large literature has computed QNMs in specific beyond-GR models, and recent work has begun to organize those calculations through perturbative spectral expansions and EFT descriptions of rotating black-hole ringdown [19, 20]. These developments are important, but they mostly answer a forward question: once a strong-field theory is"},{"citing_arxiv_id":"2605.10874","ref_index":76,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cusp Formation in Merging Black Hole Horizons","primary_cat":"gr-qc","submitted_at":"2026-05-11T17:26:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Numerical study of cusp formation on horizons in head-on non-spinning black hole mergers, with analysis of mass and multipole behavior at the cusp and a proposed phenomenological model.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05352","ref_index":19,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Perturbations in the parametrized wormhole spacetime and their related quasinormal modes","primary_cat":"gr-qc","submitted_at":"2026-05-06T18:23:56+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Observationally constrained galactic wormhole models show quasinormal mode damping rates more sensitive to galactic compactness than deformation parameters, while oscillation frequencies remain comparatively stable.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"For wormholes, they offer a similarly powerful diagnostic because they are sensitive to the underlying geometry and can help distinguish WHs from BHs and other ECOs [6]. However, while the QNM spectra of Schwarzschild, Kerr, and Reissner-Nordstr ¨om BHs, as well as many BH solutions in modified gravity, are now known in considerable detail, analogous results for parametrized wormholes remain much more limited [19, 20]. In particular, a systematic description of how the parametrization coefficients affect mode frequencies, damping timescales, and spectral structure is still lacking. This question has become more timely in view of recent observational developments. The Event Horizon Telescope (EHT) observations of M87∗ and SgrA ∗ have opened a new avenue for constraining compact-object geometries through direct imaging"},{"citing_arxiv_id":"2605.04147","ref_index":3,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Unifying the Regge-Wheeler-Zerilli and Bardeen-Press-Teukolsky formalisms on spherical backgrounds","primary_cat":"gr-qc","submitted_at":"2026-05-05T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A self-dual curvature formulation unifies the Regge-Wheeler-Zerilli and Bardeen-Press-Teukolsky equations on spherical backgrounds as components of one tensorial curvature equation.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Affairs and International Cooperation Grant No. PGR01167. References [1] E. Berti, V. Cardoso and A.O. Starinets,Quasinormal modes of black holes and black branes, Class. Quant. Grav.26(2009) 163001 [0905.2975]. [2] L. Barack et al.,Black holes, gravitational waves and fundamental physics: a roadmap,Class. Quant. Grav.36(2019) 143001 [1806.05195]. [3]LISA Consortium W a veform Working Groupcollaboration,Waveform modelling for the Laser Interferometer Space Antenna,Living Rev. Rel.28(2025) 9 [2311.01300]. [4] J. Abedi et al.,Black hole spectroscopy: from theory to experiment,2505.23895. [5] T. Regge and J.A. Wheeler,Stability of a schwarzschild singularity,Phys. Rev.108(1957) 1063. [6] F.J. Zerilli,Effective potential for even-parity regge-wheeler gravitational perturbation"},{"citing_arxiv_id":"2605.03730","ref_index":3,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Total transmission modes in draining bathtub model with vorticity","primary_cat":"gr-qc","submitted_at":"2026-05-05T13:20:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Numerical spectra of total transmission modes in the draining bathtub model with vorticity can have positive or negative imaginary parts depending on parameters, with higher overtones exhibiting pronounced spectral mobility.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"8(σ−2)(σ−1) 4 +m 2(36 +σ(−103 +σ(124 +σ(−76−3σ(σ−8))))) \u0003\u0011 +c 6D4r6 0(σ−1) 4 \u0010 c2r2 0(σ−2) \u0002 4 + 4m2 + 5σ(σ−2) \u0003\u0002 15 +σ(σ−2)(10 +σ(σ−2)) \u0003 −4B 2\u0002 −8(σ−2)(σ−1) 2 +m 2(−16 +σ(39 +σ(−44 +σ(26 +σ(σ−8))))) \u0003\u0011) . (B5) [1] H.-P. Nollert, Class. Quant. Grav.16, R159 (1999). [2] K. D. Kokkotas and B. G. Schmidt, Living Rev. Rel.2, 2 (1999), arXiv:gr-qc/9909058 . [3] E. Berti et al., (2025), arXiv:2505.23895 [gr-qc] . [4] E. Berti, V . Cardoso, and A. O. Starinets, Class. Quant. Grav.26, 163001 (2009), arXiv:0905.2975 [gr-qc] . [5] O. Trivedi, A. Gurrola, and R. J. Scherrer, (2026), arXiv:2603.04375 [gr-qc] . [6] B. P. Abbott et al. (LIGO Scientific, Virgo), Phys. Rev. Lett.116, 221101 (2016), [Erratum: Phys.Rev."},{"citing_arxiv_id":"2605.03576","ref_index":20,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Ringdown Analysis of GW250114 with Orthonormal Modes","primary_cat":"gr-qc","submitted_at":"2026-05-05T09:45:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Orthonormal QNM analysis of GW250114 raises the significance of the first overtone of the ℓ=m=2 mode from 82.5% to 99.9% and detects no significant deviation from Kerr predictions.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Will, \"On gravitational-wave spectroscopy of massive black holes with the space interferometer LISA,\" Phys. Rev. D73, 064030 (2006), arXiv:gr-qc/0512160. [19] Emanuele Berti, Jaime Cardoso, Vitor Cardoso, and Marco Cavaglia, \"Matched-filtering and parameter esti- mation of ringdown waveforms,\" Phys. Rev. D76, 104044 (2007), arXiv:0707.1202 [gr-qc]. [20] Jahed Abediet al., \"Black hole spectroscopy: from the- ory to experiment,\" (2025), arXiv:2505.23895 [gr-qc]. [21] Sizheng Ma and Huan Yang, \"Excitation of quadratic quasinormal modes for Kerr black holes,\" Phys. Rev. D 109, 104070 (2024), arXiv:2401.15516 [gr-qc]. [22] Lionel London, Deirdre Shoemaker, and James Healy, \"Modeling ringdown: Beyond the fundamental quasinor-"},{"citing_arxiv_id":"2605.03025","ref_index":1,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Can wormholes have vanishing Love numbers?","primary_cat":"gr-qc","submitted_at":"2026-05-04T18:00:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"For a specific R=0 wormhole, the magnetic Love number for ℓ=2 vanishes to linear order in the regularization parameter under static axial gravitational perturbations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Our approximate analytical calculations show that under a strictly static axial gravitational perturbation of this spacetime, the magnetic-type tidal Love number (forℓ= 2) vanishes if we keep the solution of the master equation up to linear order in the regularisation parameter of the geometry. I. INTRODUCTION Nowadays, GW astronomy of binary black hole merger[1, 2] has opened the window to test general rel- ativity in the previously unexplored strong and dynamic regime of gravity in an unprecedented manner[3-6]. Such observations can give us scope not only to test general rel- ativity but also to test the black hole nature of the com- pact objects[7]. One way to quantify the nature of the compact object is to measure it's tidal deformation dur-"},{"citing_arxiv_id":"2605.03018","ref_index":1,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Gravitational electric-magnetic duality at the light ring and quasinormal mode isospectrality in effective field theories","primary_cat":"gr-qc","submitted_at":"2026-05-04T18:00:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Gravitational electric-magnetic duality at the light ring organizes and preserves quasinormal mode isospectrality in GR and selects duality-invariant higher-derivative corrections in effective field theories.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"duality-invariant corrections to general relativity. Introduction.Gravitational-wave astronomy has opened an unprecedented window onto the strong-field dynamics of spacetime. The LIGO-Virgo-KAGRA Col- laboration runs have yielded an expanding catalog of compact-binary merger observations in which the short, clean ringdown stage is becoming increasingly amenable to precision measurements [1]. This stage is dominated by a discrete set of damped oscillations known as quasi- normal modes (QNMs) [2-7]. Because QNM frequencies are fixed entirely by the background spacetime and by the field equations that govern small perturbations, they provide a direct and model-independent probe of gravity in its most nonlinear regime [8-15]. A remarkable structural feature of QNM spectra in gen-"},{"citing_arxiv_id":"2605.02820","ref_index":57,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Gravitational-Bumblebee perturbations: Exact decoupling and isospectrality","primary_cat":"gr-qc","submitted_at":"2026-05-04T16:57:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Bumblebee gravity perturbations decouple exactly into gravitational and vector sectors, with gravitational modes dynamically immune to Lorentz violation and odd-even parities strictly isospectral.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Among these consequences, extracting observable signa- tures from LSB backgrounds is of particular importance, and gravitational waves provide perhaps the most promising ob- servational channel for this purpose [43-55]. Compared with test field perturbations [56], gravitational perturbations are more directly relevant in this context, since they are tied to the ringdown signal of gravitational waves [57]. In Einstein- Bumblebee theory, however, existing studies, even for the simplest spherically symmetric background, have often been restricted either to odd-parity perturbations [58] or to purely gravitational perturbations with the bumblebee field frozen [59, 60]. From the viewpoint of theoretical consistency, this is unsatisfactory. Since bumblebee black hole solutions are ob-"},{"citing_arxiv_id":"2605.01964","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Pole Structure of Kerr Green's Function","primary_cat":"gr-qc","submitted_at":"2026-05-03T16:51:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Homogeneous solutions and connection coefficients in the radial Teukolsky equation for Kerr black holes exhibit simple poles at Matsubara frequencies that cancel in the Green's function, along with canceling zero-frequency singularities scaling as ω^{-2l-1}.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"and quasinormal modes at large imaginary frequencies in schwarzschild space-time,\" Class. Quant. Grav.20, L159-L165 (2003), arXiv:gr-qc/0307024 [gr-qc]. [12] Marc Casals, Sam Dolan, Adrian C. Ottewill, and Barry Wardell, \"Self-force and green function in schwarzschild spacetime via quasinormal modes and branch cut,\" Phys. Rev. D88, 044022 (2013), arXiv:1306.0884 [gr-qc]. [13] Marc Casals and Adrian C. Ottewill, \"Analytic inves- tigation of the branch cut of the green function in schwarzschild space-time,\" Phys. Rev. D87, 064010 (2013), arXiv:1210.0519 [gr-qc]. [14] Marc Casals and Adrian C. Ottewill, \"High-order tail in schwarzschild spacetime,\" Phys. Rev. D92, 124055 (2015), arXiv:1509.04702 [gr-qc]. [15] David Q. Aruquipa and Marc Casals, \"Green func-"},{"citing_arxiv_id":"2604.27377","ref_index":6,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Bound-State Resonances of Schwarzschild-de Sitter Black Holes: Analytic Treatment","primary_cat":"gr-qc","submitted_at":"2026-04-30T03:40:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"SdS black holes support only a finite number of bound-state resonance levels with closed-form energies, while asymptotically flat Schwarzschild black holes have infinitely many that delocalize without bound.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.25223","ref_index":31,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Early-Time Nonlinear Growth in an Unstable Q-Ball Hairy Black Hole","primary_cat":"gr-qc","submitted_at":"2026-04-28T05:03:56+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"second-order quasi-normal modes for AdS black branes. JHEP, 09:147, 2025.arXiv:2412.20683,doi:10.1007/ JHEP09(2025)147. [30] Patrick Bourg, Rodrigo Panosso Macedo, Andrew Spiers, Benjamin Leather, Bonga B' eatrice, and Adam Pound. Quadratic quasinormal modes at null infinity on a Schwarzschild spacetime.Phys. Rev. D, 112(4):044049, 2025.arXiv:2503.07432,doi:10.1103/fbz4-qsvn. [31] Emanuele Berti et al. Black hole spectroscopy: from theory to experiment. 5 2025.arXiv:2505.23895. [32] Sizheng Ma, Keefe Mitman, Ling Sun, Nils Deppe, Fran¸ cois H' ebert, Lawrence E. Kidder, Jordan Moxon, William Throwe, Nils L. Vu, and Yanbei Chen. Quasinormal-mode filters: A new approach to analyze the gravitational-wave ringdown of binary black-hole"},{"citing_arxiv_id":"2604.24584","ref_index":6,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Pair-Dependent Drift of Kerr Neighboring-Overtone Gap Minima","primary_cat":"gr-qc","submitted_at":"2026-04-27T15:09:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Kerr overtone frequency gaps exhibit pair-dependent spin locations for their interior minima.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"for local organizing principles in the complex-frequency plane, beyond treating the spectrum as a set of isolated scalar gaps; see also Ref. [27]. What is still missing is a direct description of howneighboring overtonesapproach and separate as the Kerr spin varies, when each overtone is continuously tracked and its label is held fixed along the scan[6, 7, 10-12]. In this paper we therefore study a raw neighboring-overtone quantity: the complex-frequency separation between two adjacent overtones along a one-parameter scan ina. We find a robust and simple-to-state phenomenon. Different neighboring pairs develop clear interior minima at different spins, even within the same (s, ℓ,m) sector. The central problem is to identify what sets these minima and why their locations"},{"citing_arxiv_id":"2604.23625","ref_index":8,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Physics informed operator learning of parameter dependent spectra","primary_cat":"gr-qc","submitted_at":"2026-04-26T09:35:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DeepOPiraKAN learns parameter-to-spectrum mappings via operator learning and achieves relative errors of O(10^{-6}) to O(10^{-4}) for Kerr black hole quasinormal modes up to n=7 when benchmarked against Leaver's method.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"[6] E. Barausse, V. Cardoso, P. Pani, Can environmental effects spoil precision gravitational-wave astrophysics?, Phys. Rev. D 89 (10) (2014) 104059.arXiv:1404.7149, doi:10.1103/PhysRevD.89.104059. [7] N. Franchini, S. H. V¨ olkel, Testing General Relativity with Black Hole Quasi-normal Modes, 2024.arXiv: 2305.01696,doi:10.1007/978-981-97-2871-8_9. [8] J. Abedi, et al., Black hole spectroscopy: from theory to experiment (5 2025).arXiv:2505.23895. [9] B. P. Abbott, et al., Observation of Gravitational Waves from a Binary Black Hole Merger, Phys. Rev. Lett. 116 (6) (2016) 061102.arXiv:1602.03837,doi:10.1103/ PhysRevLett.116.061102. [10] P. Amaro-Seoane, et al., Laser Interferometer Space An- tenna, e-prints (2 2017)."},{"citing_arxiv_id":"2604.22734","ref_index":1,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Radiation outer boundary conditions and near-to-far field signal transformations for the Bardeen-Press equation","primary_cat":"gr-qc","submitted_at":"2026-04-24T17:29:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Exact transparent radiation boundary conditions and near-to-far field teleportation kernels are derived for the Bardeen-Press equation, approximated via exponential sums with error bounds, and shown to eliminate late-time artifacts in time-domain solvers.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"problematic high-order differential conditions associated with a Bayliss-Turkel-style hierarchy. Although the conditions involve formal infinite expansions, a closure condi- tion fixes the approximation order and defines incoming characteristic information. As before, this work goes well beyond the wave equation in addressing gauge issues. Moreover, the approach has been implemented within theSpEC infrastructure [1] and tested [18]. Their method also contends with issues that would arise in extending our convolution-based approach to the Einstein equations. Other strategies for outer boundary conditions and far-field signal recovery include the hyperboloidal-layer method [64, 65] pioneered by Zenginoglu and, more recently, Cauchy-characteristic matching (CCM) [45, 44]."},{"citing_arxiv_id":"2604.22684","ref_index":30,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Quasinormal Modes and Neutrino Energy Deposition for a Magnetically Charged Black Hole in a Hernquist Dark Matter Halo","primary_cat":"gr-qc","submitted_at":"2026-04-24T16:10:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Computations for a new black hole metric with magnetic charge and Hernquist halo show that charge raises QNM frequencies while the halo lowers them, with similar opposing effects on shadow size and neutrino annihilation efficiency.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"field, and the boundary conditions of purely ingoing waves at the horizon and purely outgoing waves at infinity [25-27]. They are therefore central to black-hole spectroscopy and to tests of the no-hair paradigm [28, 29]. In the eikonal regime, the real part of the QNM frequency and the damping rate are controlled by the angular frequency and Lyapunov exponent of the unstable photon orbit [30]. This correspondence gives a directbridgebetweenringdownobservablesandshadowmeasurements, andmotivatestreatingwavedynamics and null geodesics within a common framework. Most idealized studies assume an isolated vacuum black hole. Astrophysical black holes, however, are embedded in galactic environments whose dark-matter distribution can influence geodesics, redshift factors,"},{"citing_arxiv_id":"2604.22009","ref_index":108,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Black Hole Response Theory and its Exact Shockwave Limit","primary_cat":"hep-th","submitted_at":"2026-04-23T18:55:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Black hole response theory in WQFT exactly reproduces the Aichelburg-Sexl shockwave metric, geodesics, and the transfer matrix for gravitational-wave scattering off it via post-Minkowskian resummation.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Pound, B. Wardell, N. Warburton and J. Miller,Second-Order Self-Force Calculation of Gravitational Binding Energy in Compact Binaries,Phys. Rev. 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Le Tiec, Gravitational Waveforms for Compact Binaries from Second-Order Self-Force"},{"citing_arxiv_id":"2604.20914","ref_index":4,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Cracking Gravitational Wave Multiple Ringdown Modes in Space","primary_cat":"gr-qc","submitted_at":"2026-04-22T02:46:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"FIREFLY algorithm enables 200-fold faster multi-mode ringdown analysis for space-borne gravitational wave detectors while remaining compatible with time-delay interferometry.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.15758","ref_index":34,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Geometrically Regular Black Holes with Hedgehog Scalar Hair","primary_cat":"gr-qc","submitted_at":"2026-04-17T07:01:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A continuous family of asymptotically flat, geometrically regular black holes with hedgehog scalar hair exists in a minimally coupled GR-scalar-three-form theory.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"177(1969) 2239-2247. 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Suyama, \"Instability of hairy black holes in shift-symmetric horndeski theories,\"Phys."},{"citing_arxiv_id":"2604.15431","ref_index":25,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Highly eccentric non-spinning binary black hole mergers: quadrupolar post-merger waveforms","primary_cat":"gr-qc","submitted_at":"2026-04-16T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Polynomial models for the (2,2) post-merger waveform amplitudes of eccentric non-spinning binary black holes are constructed from numerical-relativity data as functions of symmetric mass ratio and two merger-time dynamical parameters.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"with (complex) frequencies completely described by the BH massM and angular momentumJ, due to the no-hair conjecture (for electromagnetically neutral BHs, consis- tent with LVK data [26, 27]). This simplicity has sparked interest in utilizing BHs not only as astrophysical tracers, but also as testing grounds for GR and the BH paradigm, a program known as Black Hole Spectroscopy [ 25, 28-37]. Current analyses carried out by the LVK collaboration ∗nishkal.rao@students.iiserpune.ac.in †gregorio.carullo@ligo.org mostly use waveform models that describe binary BH coalescences on quasi-circular orbits, the exception being Ref. [38]. This is motivated by the fact that GW radi- ation is very efficient in circularizing binaries during a"},{"citing_arxiv_id":"2604.14290","ref_index":4,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Emergent structure in the binary black hole mass distribution and implications for population-based cosmology","primary_cat":"gr-qc","submitted_at":"2026-04-15T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"B-spline agnostic reconstruction of binary black hole masses from GWTC-4.0 reveals multiple features and a logarithmic hierarchy that impacts Hubble constant measurements, with a low-mass subpopulation isolation method to mitigate systematics.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"116, 061102 (2016), arXiv:1602.03837 [gr-qc]. [2] T. A. 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[86] Nils Siemonsen, \"Ergoregion instability in bosonic stars:"},{"citing_arxiv_id":"2604.13182","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Bilinear products and the orthogonality of quasinormal modes on hyperboloidal foliations","primary_cat":"gr-qc","submitted_at":"2026-04-14T18:05:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Bilinear products for black hole quasinormal modes on hyperboloidal foliations are divergent due to CPT transformations but can be regularized to define orthogonal modes and excitation coefficients.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Rev. D34, 384 (1986). [9] R. H. Price, Phys. Rev. D5, 2419 (1972). [10] C. Gundlach, R. H. Price, and J. Pullin, Phys. Rev. D 49, 883 (1994), arXiv:gr-qc/9307009. [11] M. De Amicis, S. Albanesi, and G. Carullo, Phys. Rev. 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Ching, P."},{"citing_arxiv_id":"2604.12800","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Spectroscopy of analogue black holes using simulation-based inference","primary_cat":"gr-qc","submitted_at":"2026-04-14T14:29:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulation-based inference reliably extracts physical parameters from noisy spectra of analogue black holes.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"[12] K. D. Kokkotas and B. G. Schmidt, Living Rev. Rel.2, 2 (1999), arXiv:gr-qc/9909058. [13] H.-P. Nollert, Class. Quant. Grav.16, R159 (1999). [14] E. Berti, V. Cardoso, and A. O. Starinets, Class. Quant. Grav.26, 163001 (2009), arXiv:0905.2975 [gr-qc]. [15] R. A. Konoplya and A. Zhidenko, Rev. Mod. Phys.83, 793 (2011), arXiv:1102.4014 [gr-qc]. [16] E. Berti, V. Cardoso, G. Carullo, J. Abedi, N. Afshordi, S. Albanesi, V. Baibhav, S. Bhagwat, J. L. Bl' azquez- Salcedo, B. Bonga,et al., Black hole spectroscopy: from theory to experiment (2025), arXiv:2505.23895 [gr-qc]. [17] W. G. Unruh, Phys. Rev. Lett.46, 1351 (1981). [18] C. Barcel' o, S. Liberati, and M. Visser, Living Rev. Rel- ativ.14, 3 (2011)."},{"citing_arxiv_id":"2604.11895","ref_index":1,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Novel ringdown tests of general relativity with black hole greybody factors","primary_cat":"gr-qc","submitted_at":"2026-04-13T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"GreyRing model based on greybody factors reproduces numerical relativity ringdown signals with mismatches of order 10^{-6} and enables a new post-merger consistency test of general relativity applied to GW250114.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The final stage of a binary black hole (BH) merger, the so-calledringdown, provides one of the cleanest probes of strong-field gravity. During this phase the newly formed BH relaxes toward equilibrium through damped oscillations, and the gravitational wave- form is commonly described as a superposition of quasi- normal modes (QNMs) of the remnant spacetime [1]. In general relativity (GR), the remnant is a rotating (Kerr) BH and the entire QNM spectrum is uniquely determined by its massMand dimensionless spinχ=J/M 2 [2- 7] (we use geometrical units,G=c= 1). This prop- erty underlies the program of BH spectroscopy, in which multiple QNMs extracted from the data are checked for consistency with the Kerr prediction [8-10]."},{"citing_arxiv_id":"2604.11755","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Ringing of rapidly rotating black holes in effective field theory","primary_cat":"gr-qc","submitted_at":"2026-04-13T17:28:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"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}.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Cardoso, and C. M. Will, On gravitational- wave spectroscopy of massive black holes with the space interferometer LISA, Physical Review D73, 064030 (2006), arXiv:gr-qc/0512160. [15] E. Berti, V. Cardoso, and A. O. Starinets, Quasinormal modes of black holes and black branes, Classical and Quantum Gravity26, 163001 (2009), arXiv:0905.2975 [gr-qc]. [16] E. Berti, V. Cardoso, G. Carullo,et al., Black hole spectroscopy: from theory to experiment, Classical and Quantum Gravity (2026), arXiv:2505.23895 [gr-qc]. [17] C. Vishveshwara, Stability of the schwarzschild metric, Physical Review D1, 2870 (1970). [18] S. Teukolsky, Rotating black holes - separable wave equations for gravitational and electromagnetic pertur-"},{"citing_arxiv_id":"2604.08680","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Prompt Response from Plunging Sources in Schwarzschild Spacetime","primary_cat":"gr-qc","submitted_at":"2026-04-09T18:12:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The prompt response is ~1.2 times stronger than quasinormal mode excitation during inspiral and enables 99% accurate reconstruction of the full inspiral-merger-ringdown waveform when combined with other components.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"These results offer new insight into the transition from inspiral to merger and ringdown. I. INTRODUCTION Understanding the morphology of gravitational-wave (GW) waveforms emitted by merging binaries is essen- tial for deciphering spacetime dynamics in its most dy- namical and nonlinear regime. Over the past decades, post-Newtonian theory [1] and black hole (BH) perturba- tion theory [2] have been developed to describe the early inspiral [3-7] and late ringdown [4, 8-11] stage, thereby forming the theoretical foundation for waveform modeling and for parameterizing deviations from General Relativity [12-23]. Although quasinormal modes (QNMs), their nonlin- ear effects [24-41], and late-time tails [42, 43] have been widely used as the primary components to model the late-"},{"citing_arxiv_id":"2604.05988","ref_index":27,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Quasinormal modes of coupled metric-dilaton perturbations in two-dimensional stringy black holes","primary_cat":"gr-qc","submitted_at":"2026-04-07T15:15:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Coupled intrinsic perturbations of the MSW black hole yield complex quasinormal frequencies with negative imaginary parts confirming stability and non-zero real parts indicating oscillatory behavior, with damping rates decreasing as the central charge parameter increases.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.04568","ref_index":62,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Stationary Einstein-vector-Gauss-Bonnet black holes","primary_cat":"gr-qc","submitted_at":"2026-04-06T09:58:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"New stationary vectorized black holes exist in Einstein-vector-Gauss-Bonnet theory, including charged spherical, uncharged axial with magnetic moments, and rotating solutions bounded by Kerr and static cases.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.03985","ref_index":12,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Autoencoder-Based Parameter Estimation for Superposed Multi-Component Damped Sinusoidal Signals","primary_cat":"cs.LG","submitted_at":"2026-04-05T06:12:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Autoencoder uses latent space to estimate parameters of multi-component damped sinusoids in noise with high accuracy even for weak or opposing-phase components.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"including nuclear magnetic resonance [1], free-induction-decay optical magnetometry [2, 3], and cavity ring-down polarimetry/ellipsometry [4, 5], as well as structural health monitoring [6], vibration analysis [7], radar [8], sonar [9], communication channels [10], nuclear collective ex- citations [11], and black-hole ringdown in gravitational-wave astronomy [12]. Depending on the physical setting, such signals may decay rapidly, be contaminated by observational noise, or ∗Corresponding author †momoka.iida@g.kogakuin.jp ‡motohashi@tmu.ac.jp §hirotaka@tcu.ac.jp 1 arXiv:2604.03985v1 [cs.LG] 5 Apr 2026 consist of multiple superposed damped sinusoidal components. Their analysis therefore provides access to underlying physical properties across a wide variety of systems."},{"citing_arxiv_id":"2604.02214","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Quadratic gravity corrections to scalar QNMs of rapidly rotating black holes","primary_cat":"gr-qc","submitted_at":"2026-04-02T16:06:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"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.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"spectroscopy: from theory to experiment, Classical and Quantum Gravity (2026), arXiv:2505.23895 [gr-qc]. [16] O. Dreyer, B. J. Kelly, B. Krishnan, L. S. Finn, D. Gar- rison, and R. 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Tests of the Remnants","primary_cat":"gr-qc","submitted_at":"2026-03-19T15:22:28+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Gravitational wave remnants from GWTC-4.0 binary mergers are consistent with general relativity Kerr black hole predictions, with no evidence for post-merger echoes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2603.07469","ref_index":4,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Can Oscillatory and Persistent Nonlinearities Be Bridged in Black Hole Ringdown?","primary_cat":"gr-qc","submitted_at":"2026-03-08T05:11:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Quadratic quasinormal modes and the memory effect in black hole ringdown are related through bridge coefficients that depend primarily on remnant black hole parameters.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.18613","ref_index":30,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Correspondence between quasinormal modes and grey-body factors of Schwarzschild--Tangherlini black holes","primary_cat":"gr-qc","submitted_at":"2026-01-26T15:53:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Quasinormal modes correspond well to grey-body factors for vector and tensor perturbations of Schwarzschild-Tangherlini black holes in all dimensions, but fail for scalar l=2 modes in D≥7 because of multiple potential barriers.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.16016","ref_index":44,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Nonlinear tails of massive scalar fields around a black hole","primary_cat":"gr-qc","submitted_at":"2026-01-22T14:41:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Nonlinear tails of massive scalar fields around black holes decay at the same rate as linear tails during intermediate times, independent of sources or initial conditions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.14979","ref_index":18,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The relativistic restricted three-body problem: geometry and motion around tidally perturbed black holes","primary_cat":"gr-qc","submitted_at":"2026-01-21T13:27:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Increasing tidal deformation around a black hole drives bound geodesics through weak chaos, plunging, unbinding, and eventual depletion of all bound motion, with semi-analytic critical amplitudes for each transition.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"(GRAVITY), Astron. 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II: isospectrality loss in gravitational waveforms","primary_cat":"gr-qc","submitted_at":"2026-01-19T21:48:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"In a beyond-GR cubic-curvature model, loss of isospectrality makes it generally difficult to identify the two fundamental quasinormal modes from black hole ringdown time series, though evidence for a non-GR mode is sometimes possible.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}