{"total":13,"items":[{"citing_arxiv_id":"2606.28499","ref_index":26,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Stochastic Variability of Binary Accretion","primary_cat":"astro-ph.HE","submitted_at":"2026-06-26T18:00:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Simulations show the accretion rate PSD in a q=0.2 SMBH binary is a broken power-law with white noise to -4 slope transition at ~5 times orbital frequency due to damped random walk gas delivery and minidisk filtering.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.22559","ref_index":46,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Migration Traps as Variability Attractors: Optical/UV Signatures of Embedded Stellar-Mass Black Holes in Active Galactic Nucleus Disks","primary_cat":"astro-ph.GA","submitted_at":"2026-06-21T15:33:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Migration traps concentrate stellar-mass black holes in AGN disks, generating self-regulated magnetic reconnection heating that yields excess short-timescale optical/UV variability, flattened structure functions, and deviations from the τ∝λ^{4/3} lag relation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20317","ref_index":160,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Simulation-Based Prediction of Black Hole Fe K$\\alpha$ Line Profiles","primary_cat":"astro-ph.HE","submitted_at":"2026-05-19T18:00:00+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Fe Kα lines from accreting black holes are produced mostly outside 10 gravitational radii due to radial ionization gradients, allowing broad profiles without high spin.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15867","ref_index":179,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Spectral-Regime Overlap and Transition-like Behavior in the Blazar Population from Multi-Instrument X-ray and TeV Observations","primary_cat":"astro-ph.HE","submitted_at":"2026-05-15T11:34:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Multi-instrument observations reveal broad overlap in X-ray photon indices across blazar subclasses with intra-source spectral evolution supporting transition-like behavior.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.07965","ref_index":96,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Changing-Look Seyfert Discovered by eROSITA Reveals a Two-Component Broad-Line Region","primary_cat":"astro-ph.GA","submitted_at":"2026-05-08T16:28:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"HE 1237-2252 exhibits a changing-look event driven by intrinsic accretion-rate variations, revealing a two-component broad-line region consisting of virialized gas at ~27 light-days and disk emission at larger radii.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05303","ref_index":97,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Multi-wavelength outburst activity from EP J174942.2-384834: a very faint X-ray transient discovered by Einstein Probe","primary_cat":"astro-ph.HE","submitted_at":"2026-05-06T18:00:02+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"EP J174942.2-384834 is classified as a very faint X-ray transient black hole candidate based on its hard X-ray spectra, optical/UV brightening correlated with X-rays, and lack of radio emission.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"well fitted with a number of zero-centered Lorentzians (C. Done et al. 2007). However, the dominant Poisson noise in theNuSTARdata of EP J1749 limits the de- tectable fraction of the intrinsic variability. Here we as- sume that the zero-centered Lorentzian fit presented in Section 3.3.1 corresponds toν b (C. Done et al. 2007). Ac- cording to the propagating accretion-rate fluctuations model (Y. E. Lyubarskii 1997; P. Ar' evalo & P. Utt- ley 2006), broad-band variability in accreting systems is produced by fluctuations in the viscosity that orig- inate at large radii and propagate inward through the accretion flow. In this framework,ν b traces the viscous frequency at the inner edge of the accretion flow, which evolves during state transitions (C. Done et al."},{"citing_arxiv_id":"2605.02662","ref_index":55,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Is XRISM/Resolve probing a \"raining\" absorber in Mrk 509?","primary_cat":"astro-ph.HE","submitted_at":"2026-05-04T14:41:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"XRISM/Resolve data on Mrk 509 show a tentative 3.6-sigma infalling absorber at 11000 km/s located within thousands of gravitational radii, interpreted as raining clumps from a failed wind.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"plenishing the fuel supply. The collision of such massive, dense clumps with the accretion disk may induce local instabilities and density perturbations within the flow. These stochastic inhomo- geneities can then propagate inward through the disk on vis- cous timescales, effectively acting as the physical \"seeds\" for the propagating fluctuations model (e.g., Lyubarskii 1997; Arévalo & Uttley 2006). In this scenario, the raining material may con- tribute to the intrinsic variability of the accretion flow, providing a mechanism to explain the observed broadband timing proper- ties, including the characteristic time lags detected between dif- ferent X-ray energy bands (De Marco et al. 2013). It is finally worth mentioning here that the possible detection"},{"citing_arxiv_id":"2604.21390","ref_index":6,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Synchronized Spin Model for Black-Hole Accretion Systems","primary_cat":"astro-ph.HE","submitted_at":"2026-04-23T07:58:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A model of accretion-disk dynamos as synchronized macro-spins unifies broadband variability, coronal heating, jets, and hard/soft cycles via collective spin dynamics.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"in changing-look AGN [1, 2, 3, 4, 5]. The main theoretical cha llenge is therefore not to explain any one component in isolation, but to identify a compact phy sical language that links timing, topology, and outflow morphology. Existing approaches address important subsets of the probl em. Propagating-fluctuation models reproduce red-noise continua and multiplicative variability [6, 7, 8]. Ordered-flux models explain how jets and winds are launched once a suitable magnetic geom etry exists [9, 10]. Reconnection and plasmoid pictures explain impulsive dissipation, flare s, and intermittent ejections [11, 12, 13]. What remains less clear is why these observables reorga nize together. We address this problem with a Synchronized Spin Model (SSM)."},{"citing_arxiv_id":"2604.16688","ref_index":48,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Persistence of the Millihertz X-ray Quasi-Periodic Oscillation in the Active Galactic Nucleus 1ES 1927+654","primary_cat":"astro-ph.HE","submitted_at":"2026-04-17T20:46:17+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"The mHz QPO in 1ES 1927+654 has persisted and stabilized at ~2.5 mHz with stable soft lags, no strong harmonic, and repeatable large-amplitude flux patterns, also seen in NuSTAR.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"to the short observations of 1ES 1927+654. To the first point, at low frequencies (f≲10 −4 Hz), nearly all AGN show hard lags and a log-linear increase in the LES to high energies (E. Kara et al. 2016). These low-frequency hard lags were first discovered in BHXRBs and have long been associated with propagating fluctuations in the accretion flow (e.g., Y. E. Lyubarskii 1997; O. Ko- tov et al. 2001; P. Ar' evalo & P. Uttley 2006). While we defer a detailed analysis of the RMS-flux relationship and the lack of propagating fluctuations to subsequent work, it is interesting to note that 1ES 1927+654 also clearly breaks the canonical RMS-flux relation of accret- ing sources that also is thought to arise from propagat- ing fluctuations (P."},{"citing_arxiv_id":"2604.12109","ref_index":77,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Identifying Changing-Look AGN Transitions in Light Curve Data with the Zwicky Transient Facility","primary_cat":"astro-ph.GA","submitted_at":"2026-04-13T22:32:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A criterion of |Δg| > 0.4 mag and |Δ(g-r)| > 0.2 mag detects photometric CL-AGN transitions in 9.6% of known hosts with 1.6% false positive rate from simulations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"close to the black hole which form the Broad Line Region (BLR) (R. Antonucci 1993; C. M. Urry & P. Padovani 1995). Meanwhile, face-on Type 1 AGN allow for ob- servations of the central accretion disk, which exhibits variable emission at all wavelengths (for a recent review, see M. Paolillo & I. Papadakis 2025). AGN variability in the UV/optical may come from accretion rate changes (e.g. Y. E. Lyubarskii 1997), changes in accretion disk properties (e.g. B. C. Kelly arXiv:2604.12109v1 [astro-ph.GA] 13 Apr 2026 2 et al. 2009; C. J. Burke et al. 2021), reprocessing of high- energy photons (e.g. D. Kazanas & S. Nayakshin 2001; E. M. Cackett et al. 2007; E. S. Kammoun et al. 2021), microlensing (e.g. G. Vernardos et al. 2024), or some combination of all of these (M."},{"citing_arxiv_id":"2604.07540","ref_index":18,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Stochastic Optical Variability and an rms-flux Relation in the Intermediate Polar EP240309a","primary_cat":"astro-ph.SR","submitted_at":"2026-04-08T19:32:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"New timing and spectral analysis of EP240309a yields conservative upper limits on the white-dwarf magnetospheric radius of a few times 10^10 cm and detects an rms-flux relation in some TESS sectors.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"therefore use the bootstrapped slope as the primary effect size and treat the Pearson statistics listed in Section 4.4 as descriptive diagnostics. The rapid optical variability and PSD constraints further indicate broadband red-noise behavior typical of cataclysmic variables: the fitted single-power-law indices spanα≃1.16±0.23to1.78±0.11across nights (Section 4.3), consistent with stochastic accretion-driven flickering (e.g., Y . E. Lyubarskii 1997; P. Uttley et al. 2005; A. Bruch 2021). However, we do not detect a robust PSD bend in the sampled frequency range, so the timing analysis provides only one-sided lower limits on any putative bend frequency. Under standard dynamical identifications, these translate into conservative upper bounds on a characteristic inner scale and do not constitute evidence for a measured magnetospheric truncation radius or for disc-fed accretion in EP240309a."},{"citing_arxiv_id":"2507.20232","ref_index":55,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Systematic Search for Active Galactic Nucleus Flares in ZTF Data Release 23","primary_cat":"astro-ph.HE","submitted_at":"2025-07-27T11:30:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Systematic search of ZTF DR23 data yields catalogs of 28,504 coarse and 1,984 refined AGN flares with public release.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1906.08266","ref_index":35,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"An X-ray reverberation mass measurement of Cygnus X-1","primary_cat":"astro-ph.HE","submitted_at":"2019-06-19T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"X-ray reverberation lags are used to measure the mass of the stellar-mass black hole Cygnus X-1 for the first time.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}