{"total":10,"items":[{"citing_arxiv_id":"2605.13890","ref_index":20,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Analytic thin disks and rings in a class of nonasymptotically flat static spacetimes","primary_cat":"gr-qc","submitted_at":"2026-05-12T06:01:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"External quadrupolar distortion imprints on orbital dynamics and accretion structure in thin disks around deformed compact objects, with the radiating region's outer edge tied to the radiation-to-gas pressure transition.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"seed q-metric is asymptotically flat, the distorted geometry obtained in this way is, in general, only locally valid. In pro- late spheroidal coordinates 1 the corresponding line element takes the form ds2 =− x−1 x+1 !1+α e2 ˆψ dt2 (1) +M 2(x2 −1) x+1 x−1 !1+α e−2 ˆψ \" x2 −1 x2 −y 2 !α(2+α) e2ˆγ dx2 x2 −1 + dy2 1−y 2 ! +(1−y 2)dϕ 2 # . wheret∈(−∞,+∞),x∈(1,+∞),y∈[−1,1], andϕ∈ [0,2π) andα∈(−1,∞) is the deformation parameter in the q-metric. HereMis the Schwarzschild mass parameter ap- pearing in the metric and equals the physical mass when α=0. For generalα,M ADM =(1+α)M. Since the seed q-metric contribution has already been written explicitly in Equation 1, the functions ˆψand ˆγencode only the external distortion field (Faraji 2022). They are given by ˆψ= ∞X n=1 βnRnPn \u0012 xy R \u0013 ,(2) and ˆγ= ∞X n=1 βn(1+α) n−1X l=0 h (−1) n−l+1(x+y)−x+y i RlPl + ∞X n,k=1 nkβ nβk n+k Rn+k (PnPk −P n−1Pk−1) ,(3) whereβ n ∈Rare constants characterizing the external multi- polar distortion,P n denotes the Legendre polynomial of de- green, and Pn ≡P n \u0012 xy R \u0013 ,R= q x2 +y 2 −1.(4) By construction, setting ˆψ=0 and ˆγ=0 recov- ers the q-metric, whereas the additional limitα=0 yields the Schwarzschild solution. The transformation to Schwarzschild-like coordinates is x= r M −1,y=cosθ,(5) 1 Prolate spheroidal coordinates are obtained by rotating the two- dimensional elliptic coordinates about the focal axis of the ellipse. Analytic thin disks and rings3 so that the domainx>1 corresponds to the exterior region r>2M. This metric has a central curvature singularity at x=−1 (orr=0), as well as an additional singularity ap- pears atx=1 (orr=2M), and the norm of the time-like Killing vector at this latter vanishes. However, outside this hypersurface, there exists no additional horizon. Neverthe- less, considering a relatively small quadrupole moment, a physically interior solution can cover this hypersurface, since it is closely place to the central singularity (Quevedo 2011a). Besides, o"},{"citing_arxiv_id":"2605.02000","ref_index":38,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Ergosphere Geometry and Thermodynamic Properties of Boosted Kerr-Taub-NUT Solutions in Kaluza-Klein Theory","primary_cat":"gr-qc","submitted_at":"2026-05-03T18:08:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A Kaluza-Klein boost on Kerr-Taub-NUT enlarges the physical ergoregion volume without altering horizon radius, entropy, or temperature, while adding dyonic work terms to the first law.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.25560","ref_index":16,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Massive black holes and their galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-04-28T12:31:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":0.0,"formal_verification":"none","one_line_summary":"A review summarizing detection methods, population statistics, and coevolution of supermassive black holes with host galaxies from early universe observations and simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.24961","ref_index":1,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Pair-Rich Corona of an Accreting Kerr Black Hole","primary_cat":"astro-ph.HE","submitted_at":"2026-04-27T19:57:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A Monte Carlo model of a Kerr black hole corona shows that photon collisions create a dense electron-positron pair cloud concentrated near the black hole, yielding X-ray temperatures, Compton parameters, and 4-10% polarization consistent with binary black hole observations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"in Boyer-Lindquist (BL) coordinates. Here, ω(r, θ) =− gtϕ gϕϕ = 2M ar A (4) is the angular frequency of a ZAMO, and ˜gtt =g tt −ω 2gϕϕ; Σ(r, θ) =r 2 +a 2 cos2 θ; ∆(r) =r 2 −2M r+a 2; A(r, θ) = (r2 +a 2)2 −a 2∆ sin2 θ.(5) CentrifugalsupportneartheBHequatoristhenstable outside the standard ISCO for material test particles (Bardeen et al. 1972), rISCO M = 3 +Z2 −[(3−Z 1)(3 +Z 1 + 2Z2)]1/2; Z1 ≡1 + (1−a 2)1/3[(1 +a) 1/3 + (1−a) 1/3]; Z2 ≡(3a 2 +Z 2 1)1/2.(6) The ion density profile atr > rISCO is chosen to approx- imate an isothermal distribution in hydrostatic balance in theθ-direction, nd(θ, r) =n d,0(r) exp \u0012 − cos2 θ 2 sin2 θd \u0013 .(7) This angular profile is independent of radius within each segment of the disk, corresponding to a disk aspect ra-"},{"citing_arxiv_id":"2601.18422","ref_index":22,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Time-reversed Shannon entropy as a chaos indicator for non-integrable systems","primary_cat":"gr-qc","submitted_at":"2026-01-26T12:32:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Time-reversed Shannon entropy distinguishes chaotic from regular orbits in Kerr and Schwarzschild-Melvin spacetimes by quantifying forward-backward asymmetry in probability distributions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.19077","ref_index":36,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The First Model-Independent Upper Bound on Micro-lensing Signature of the Highest Mass Binary Black Hole Event GW231123","primary_cat":"gr-qc","submitted_at":"2025-12-22T06:37:44+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"No definitive lensing is detected in GW231123, though a potential microlensing feature with modulation amplitude up to 0.8 at 95% confidence is noted, limited by large waveform systematics in short signals.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2503.21203","ref_index":24,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Massive particle surfaces and black hole shadows from intrinsic curvature","primary_cat":"gr-qc","submitted_at":"2025-03-27T06:45:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Extends intrinsic curvature criteria for massive particle surfaces to stationary spacetimes and demonstrates application to black hole shadows in Kerr-family and Einstein-Maxwell-dilaton solutions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2411.19491","ref_index":29,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Magnetic reconnection under centrifugal and gravitational electromotive forces","primary_cat":"astro-ph.HE","submitted_at":"2024-11-29T06:15:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Centrifugal and gravitational forces both raise magnetic reconnection rates near Kerr black holes, with gravity separating charges and centrifugal force shortening the current sheet via curved geometry seen by a comoving observer.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2303.11713","ref_index":22,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The physics of gravitational waves","primary_cat":"gr-qc","submitted_at":"2023-03-21T10:04:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":0.0,"formal_verification":"none","one_line_summary":"Lecture notes deriving gravitational wave physics from first principles in general relativity for PhD and advanced MSc students.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1906.08310","ref_index":3,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A public relativistic transfer function model for X-ray reverberation mapping of accreting black holes","primary_cat":"astro-ph.HE","submitted_at":"2019-06-19T19:07:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A new public relativistic transfer-function model reltrans for X-ray reverberation mapping that fits both spectra and lags to measure black-hole masses.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"The grey dashed lines are the Newtonian equivalent for h = 1.8 (to be compared with the solid magenta line) and h = 100 (to be compared with the solid orange line). As expected, this is a better approximation for larger source heights. d: Emissivity profile for Γ = 2, a = 0.99 and h as labelled in panel c. Again, the grey dashed lines are the Newtonian equivalent [ϵ(r)∝( h2 + r 2)−3/2] for h = 100 and h = 1.8. for three different values of Γ, illustrating that a steeper spectrum leads to a steeper emissivity profile. Panels (c) and (d) show respectively the radial derivative of the cosine of the angle δ and the overall emissivity profile for various parameter combinations. The grey dashed lines represent the Newtonian approximations [|d cosδ/dr|= hr(h2 +r2)−3/2 and"}],"limit":50,"offset":0}