{"total":12,"items":[{"citing_arxiv_id":"2606.27429","ref_index":92,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Massive scalar fields in eccentric regime: Detectability and constraints from LISA observations of extreme mass-ratio inspirals","primary_cat":"gr-qc","submitted_at":"2026-06-25T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Computes scalar and tensor fluxes for eccentric EMRIs with massive scalars, quantifies dephasing, and shows via Fisher matrix that LISA can constrain scalar charge and mass.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02146","ref_index":40,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Spectral suppression of black hole ringdown tails","primary_cat":"gr-qc","submitted_at":"2026-06-01T12:12:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Spectral properties of oscillatory sources suppress the branch-cut contribution to black hole ringdown tails, explaining their absence in quasi-circular mergers.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15265","ref_index":8,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Eccentric Stellar-mass Binary Black Holes: Population, Detectability, and Waveform Analysis in the LISA and LIGO Era","primary_cat":"astro-ph.HE","submitted_at":"2026-05-14T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations of dynamical channels predict ~36 eccentric stellar-mass BBHs detectable by LISA in the Milky Way at SNR>1 over 10 years, a local merger rate of ~9 Gpc^{-3} yr^{-1}, and hundreds of faint extragalactic mHz sources.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.07187","ref_index":104,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing Gravitational Wave Signatures from Periodic Orbits of Regular Black Holes in Asymptotically Safe Gravity","primary_cat":"gr-qc","submitted_at":"2026-05-08T03:32:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The quantum parameter ξ in an asymptotically safe regular black hole shifts the innermost stable orbit, enhances whirl behavior in periodic geodesics, and produces amplitude-modulated millihertz gravitational-wave strains whose peak amplitude grows with ξ, placing them inside the sensitivity bands预计","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the large mass hierarchy and prolonged inspiral phase, such systems emit GWs within the millihertz frequency band, which lies well within the sensitivity windows of these detectors. The emitted gravitational radiation en- codes detailed information about the strong-field orbital dynamics and the underlying spacetime geometry of the central black hole [104, 105]. Consequently, EMRIs offer a unique opportunity to test GR in the strong-gravity regime and to probe possible deviations arising from quantum-gravity-motivated corrections. In particular, within the framework of ASG, the RBHASG solution (5) characterized by the scale parameterξmodifies the geodesic structure and orbital frequencies. These modifi-"},{"citing_arxiv_id":"2605.05362","ref_index":57,"ref_count":3,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraining Lorentz symmetry breaking in bumblebee gravity with extreme mass-ratio inspirals","primary_cat":"gr-qc","submitted_at":"2026-05-06T18:40:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"LISA can constrain the Lorentz symmetry breaking parameter ell in bumblebee gravity to O(10^{-4}) uncertainty via EMRI waveform analysis in the AAK framework.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"induced by bumblebee gravity. Below, we quantitatively discuss their detectability. B. Parameter Estimation To connect with observations, it is necessary to convert the plus and cross polarizations of the GW into the LISA detector response. The response of LISA to the incident GW is modeled by two independent Michelson-type channelsα=I, II, with time-domain strain [57] hα(t) = √ 3 2 \u0002 F + α (t)h+(t) +F × α (t)h×(t) \u0003 ,(29) whereF +,× α (t) are the antenna pattern functions. 7 10 7 10 6 10 5 10 4 10 6 10 5 10 4 10 3 10 2 10 1 Mismatch p = 12, e = 0.1 p = 12, e = 0.2 p = 14, e = 0.1 FIG. 2. Mismatch as a function ofℓbetween the reference waveform (ℓ= 0) and the modified waveform (ℓ̸= 0), shown for three representative initial orbital configurations (p, e) as labeled in the legend."},{"citing_arxiv_id":"2604.26011","ref_index":5,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Parameter-estimation bias induced by transient orbital resonances in extreme-mass-ratio inspirals","primary_cat":"gr-qc","submitted_at":"2026-04-28T18:00:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Neglecting transient orbital resonances in EMRIs causes significant SNR losses and biases in recovered parameters, with the sign and amplitude of resonance-induced changes to integrals of motion being critical.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"in LISA's sensitivity band for its entire mission dura- tion. Estimates indicate that LISA could detect up to 103 EMRI events over its nominal4.5-year mission life- time [1, 6, 7]. The GW signal produced by the slow inspiral encodes detailed information about the space- time geometry of the central object, enabling extremely precise measurements of BH masses and spins [5, 8, 9], as well as tests of consistency with the predictions of general relativity [10-12]. Moreover, EMRIs can act as high-precision standard sirens, providing independent constraints on cosmological parameters [13-15]. Observ- ing several EMRI events will also probe the population of massive BHs and stellar-mass compact objects in the galactic nuclei [16, 17]."},{"citing_arxiv_id":"2604.24413","ref_index":17,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational waves of extreme-mass-ratio inspirals in a rotating black hole with Dehnen dark matter halo","primary_cat":"gr-qc","submitted_at":"2026-04-27T12:40:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"EMRI waveforms in a rotating black hole with Dehnen DM halo show amplitude and phase shifts from Kerr, with mismatch rising as DM mass parameter and black hole spin increase.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"0005 0.0010 t/s h+D/μ Figure 1: Gravitational waveforms of EMRIs in Kerr (blue) and DMBH (orange). . 4 Analysis of the Waveforms 4.1 Detector Response The strain of space-based GW detectors caused by GWs is given by h= √ 3 2 \u0002 F +h+ +F ×h× \u0003 ,(63) 11 whereF + andF × in (63) are the response functions. For LISA, the response functions are given by [17,86-88] F + = 1 2(1 + cos2 Θ) cos(2Φ) cos(2Ψ) −cos(Θ) sin(2Φ) sin(2Ψ), F × = 1 2(1 + cos2 Θ) cos(2Φ) sin(2Ψ) + cos(Θ) sin(2Φ) cos(2Ψ). (64) The direction of polarization + is along ˆN× ˆL, where ˆNis the unit vector pointing from the detector to the GW source, ˆLdenotes the normal direction of the plane of the secondary's orbit. The axis of polarization state×is"},{"citing_arxiv_id":"2604.06053","ref_index":84,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing Kerr Symmetry Breaking with LISA Extreme-Mass-Ratio Inspirals","primary_cat":"gr-qc","submitted_at":"2026-04-07T16:41:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LISA EMRIs can constrain deviations from Kerr equatorial symmetry to 10^{-2} and axial symmetry to 10^{-3} using Analytic Kludge waveforms and Fisher analysis.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"pole moments of the primary (or a subset of them). The simplest description is the Peters and Matthews approximation [82, 83], in which the orbital dynamics is Newtonian and the GW emission mechanism is de- scribed by the quadrupole formula. A widely used ex- tension of the Peters and Matthews approximation is theAnalytic Kludge(AK) model introduced by Barack and Cutler [84], which incorporates all the remaining ingredients in EMRI dynamics not present in the Pe- ters and Matthews approximation using (low order) post- Newtonianapproximations: pericenterprecession, Lense- Thirring precession, and inspiral driven by radiation re- action. The AK model enables fast waveform generation and has been extensively used in data-analysis and pa-"},{"citing_arxiv_id":"2604.06009","ref_index":59,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Are Black Holes Fuzzballs? Probing Horizon-Scale Structure with LISA","primary_cat":"hep-th","submitted_at":"2026-04-07T16:05:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LISA can constrain non-axisymmetric mass quadrupole deformations at the 10^{-3} level and axisymmetric mass octupole deformations at the 10^{-2} level in EMRI signals to test fuzzball proposals.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"tions from the Kerr multipolar structure. This program was initiated by Ryan [51-55], who demonstrated its fea- sibility and showed that theclassicLISA design [56-58] could allow for the measurement of three to five multi- polemoments, correspondingtoonetothreeindependent tests of the Kerr hypothesis [54]. Later, Barack and Cutler, using theirAnalytic Kludge (AK) EMRI model [59], which contains all the main in- gredients of the EMRI dynamics in a Newtonian and post-Newtonian fashion, were able to introduce the mass quadrupole,M 2 (=−M a 2 =−S 2/Mfor a Kerr BH), as an additional independent parameter [60]. Recent stud- ies have shown [32] that LISA can constraint fractional deviations away from the Kerr mass quadrupoleQat the"},{"citing_arxiv_id":"2601.00550","ref_index":19,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Taxonomy of periodic orbits and gravitational waves in a non-rotating Destounis-Suvorov-Kokkotas black hole spacetime","primary_cat":"gr-qc","submitted_at":"2026-01-02T03:46:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Periodic orbits around a non-rotating Destounis-Suvorov-Kokkotas black hole are taxonomized with integer triplets and their gravitational waveforms are calculated, showing that large deformations eliminate circular orbits and modify wave signals.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.03788","ref_index":28,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Boson Stars Hosting Black Holes","primary_cat":"gr-qc","submitted_at":"2025-11-05T19:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Numerical and analytic modeling of boson star-black hole systems in the nonrelativistic limit, with Fisher analysis indicating LISA sensitivity to ultralight dark matter mass and self-coupling via gravitational wave dephasing.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.16399","ref_index":8,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on the extreme mass-ratio inspiral population from LISA data","primary_cat":"gr-qc","submitted_at":"2025-08-22T14:00:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A neural-network-accelerated hierarchical Bayesian pipeline is developed and validated on a phenomenological model to constrain EMRI population parameters from LISA data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}