{"total":12,"items":[{"citing_arxiv_id":"2605.25625","ref_index":42,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Periodic orbits and gravitational waveforms around a Schwarzschild black hole with a cloud of strings embedded in perfect fluid dark matter","primary_cat":"gr-qc","submitted_at":"2026-05-25T09:28:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Analysis of how string cloud parameter a and dark matter parameter α alter MBO, ISCO, periodic orbits indexed by q, and the gravitational waveforms generated by those orbits in a modified Schwarzschild spacetime.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.07187","ref_index":18,"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":"method","top_context_polarity":"use_method","context_text":"broadens asξincreases, indicating that quantum cor- rections enlarge the parameter space for bound orbital motion. III. PERIODIC ORBITS In this section, we investigate the periodic orbits around the RBHASG. To construct the particle trajec- tories, one may in principle integrate Eqs. (8) and (9), which determinet(τ),ϕ(τ), andr(τ) in terms of the affine parameterτ[18, 98]. However, the radial equa- tion (9) contains a square root, thereby requiring an ex- plicit choice of sign corresponding to inward ( ˙r <0) and outward ( ˙r >0) motion. To avoid this ambiguity, we ob- tained a convenient equation of motion by differentiating Eq. (9), which reads ¨r= L2f(r) r3 − f ′(r)Veff(r) 2f(r) .(12) This radial equation is convenient for numerical integra-"},{"citing_arxiv_id":"2604.13564","ref_index":29,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Topologically equivalent yet radiatively distinct orbits in EMRI system","primary_cat":"gr-qc","submitted_at":"2026-04-15T07:21:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"In dyonic black holes, periodic orbits with identical rotation numbers but spanning different curvature regions generate radiatively distinct gravitational waveforms in EMRIs.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"ing rise to two distinct bound branches with energiesE 1 andE 2, as well as an additional extended branch with higher energyE 3 that spans both wells. On the equatorial plane, bound motion is characterized by two fundamental frequencies: the radial frequencyω r and the azimuthal frequencyω ϕ. Periodic orbits arise when their ratio is rational. Following the standard def- inition [29], we introduce the parameterq q≡ ωϕ ωr −1 = ∆ϕr 2π −1,(8) where ∆ϕ r is the total azimuthal advance accumulated during one complete radial oscillation. Whenqis rational, the orbit closes afterzradial os- cillations andwwhirls, with an additional vertex shiftv, allowing a discrete topological classification (z, w, v) [29]. The total number of azimuthal revolutions in one full pe-"},{"citing_arxiv_id":"2604.11866","ref_index":35,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Equatorial periodic orbits and gravitational wave signatures in Euler-Heisenberg black holes surrounded by perfect fluid dark matter","primary_cat":"gr-qc","submitted_at":"2026-04-13T17:07:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Periodic orbits in Euler-Heisenberg black holes surrounded by perfect fluid dark matter produce burst-like gravitational wave signals whose amplitude and frequency content are modified by both dark matter density and QED parameters.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the ratio of angular and radial frequencies is rational. The rational parameterqis defined as q= ωϕ ωr −1 = ∆ϕ 2π −1,(24) where∆ϕis the total azimuthal angle accumulated during one complete radial oscillation between the periapsisr p and apoapsisr a, ∆ϕ= 2 Z ra rp L r2 q E2 −g(r) 1 + L2 r2 \u0001 dr.(25) The rational numberqcan be written in terms of three inte- gers(z, w, v)[35], q=w+ v z ,(26) wherezis the zoom number,wis the number of whirls, and vis the vertex number. This zoom-whirl structure character- 6 FIG. 2: Dependence of the ISCO radiusr ISCO, ISCO angular momentumL ISCO, and ISCO energyE ISCO on the model parameterα. izes the topology of strong-field orbits around the EH-PFDM black hole. For bound motion, the angular momentum is restricted to"},{"citing_arxiv_id":"2603.25084","ref_index":95,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Particle motions and gravitational waveforms in rotating black hole spacetimes of loop quantum gravity","primary_cat":"gr-qc","submitted_at":"2026-03-26T06:38:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The LQG parameter ξ enlarges equatorial bound orbit energy ranges, confines off-equatorial trajectories, and produces larger deviations from Kerr waveforms in EMRI models for two rotating LQG black holes, though signals fall below detector sensitivities.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"95 0.0 0.5 1.0 1.5 2.0 9.5 10.0 10.5 11.0 11.5 12.0 12.5 ξ  L=2.2, E=0.868 L=2.5, E=0.93 0.0 0.1 0.2 0.3 0.4 0.5 6 7 8 9 ξ  FIG. 7. The allowed region ofCas the function ofξwith selectedLandEfor the prograde cases in the type BH-I. From left to right,a= 0.1,0.5,0.9. pointing to the radial direction associated to the motion of the secondary object [95]. Now, to describe the orbital motion, we can define an orbital eccentricityeand semi-latus rectumpusing the conventional Keplerian definitions rp = p 1 +e, r a = p 1−e,(39) thentheorbitscanbedescribedintermsofanewangular 10 0 2 4 6 8 10 12 14 -4 -2 0 2 4 r sin θ r cos θ FIG. 8. The projections of prograde orbits on the meridian plan fora= 0.5,L= 3."},{"citing_arxiv_id":"2601.14979","ref_index":71,"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":"[68] J. Hor' ak, M. A. Abramowicz, W. Klu' zniak, P. Rebusco, and G. T¨ or¨ ok, Astronomy and Astrophysics499, 535 (2009), arXiv:0901.3076 [astro-ph.CO]. [69] P. Rebusco, Publ. Astron. Soc. 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Buxton, C."},{"citing_arxiv_id":"2601.02904","ref_index":30,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing the nature of Einstein nonlinear Maxwell Yukawa black hole through gravitational wave forms from periodic orbits and quasiperiodic oscillations","primary_cat":"gr-qc","submitted_at":"2026-01-06T10:41:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Gravitational waveforms from periodic orbits and QPOs around ENLMY black holes are derived and used with MCMC to constrain the Yukawa parameter and charge for microquasars and the galactic center.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.00550","ref_index":17,"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":"2512.11911","ref_index":22,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational radiations from periodic orbits around a black hole in the effective field theory extension of general relativity","primary_cat":"gr-qc","submitted_at":"2025-12-11T01:04:43+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.14080","ref_index":47,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Periodic orbits and their gravitational wave radiations in $\\gamma$-metric","primary_cat":"gr-qc","submitted_at":"2025-11-18T03:10:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Deviations from γ=1 in the Zipoy-Voorhees metric shift the (z,w,v) classification of periodic orbits and induce phase shifts plus amplitude modulations in their gravitational-wave signals.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.23318","ref_index":25,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational waveforms from periodic orbits around a novel regular black hole","primary_cat":"gr-qc","submitted_at":"2025-09-27T14:06:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Numerical study finds that a deviation parameter in a regular black hole with Minkowski core produces phase shifts and amplitude changes in kludge waveforms from periodic orbits, making them distinguishable from Schwarzschild for larger deviations and certain orbit types.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.04261","ref_index":22,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Topological charge and black hole photon spheres in massive gravity","primary_cat":"gr-qc","submitted_at":"2025-09-04T14:38:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"In dRGT massive gravity, static spherically symmetric black holes exhibit zero, one, or two photon spheres whose topological charges and stability patterns differ from Einstein gravity and from horizonless compact objects.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"03404 [gr-qc] . 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