pith. sign in

arxiv: 2511.09626 · v2 · submitted 2025-11-12 · 🌌 astro-ph.HE

Changing-Look AGN Powered By Disk Tearing

Nicholas Kaaz , Matthew Liska , Charlotte Ward , Jordy Davelaar This is my paper

Pith reviewed 2026-05-17 22:02 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords changing-look AGNdisk tearingtilted accretion diskblack holebroad line regiongeneral relativistic magnetohydrodynamics
0
0 comments X

The pith

Disk tearing in tilted accretion disks powers the rapid luminosity swings seen in changing-look AGN.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper uses high-resolution three-dimensional simulations of a geometrically thin, tilted accretion disk around a rapidly spinning 10^8 solar mass black hole to demonstrate that disk tearing produces order-of-magnitude changes in both continuum and broad-line emission. Ray-tracing follows the disk light to an observer and to a torus-like broad line region, where the continuum photoionizes gas and generates the emission-line spectrum. These calculations show that the torn disk precesses and restructures on short timescales, driving months-to-years variability that matches changing-look AGN, plus shorter weeks-scale and intraday oscillations. The precession also creates asymmetric illumination, producing evolving red-to-blue line asymmetries as a potential observational signature.

Core claim

Disk tearing violently restructures a tilted accretion disk on timescales much shorter than the viscous time, causing the inner disk to precess and breathe radially; the resulting time-dependent illumination of a torus-like broad line region produces order-of-magnitude swings in both continuum and line luminosities on months-to-years timescales, together with weeks-long precession-driven variability and intraday quasi-periodic oscillations.

What carries the argument

Tearing of the tilted, geometrically thin accretion disk, which triggers rapid geometric restructuring, combined with ray-tracing to compute continuum emission and the photoionized spectrum from a prescribed broad line region.

If this is right

  • Continuum and line luminosities both vary by factors of ten on months-to-years timescales that align with observed changing-look events.
  • Precession of the torn disk produces time-dependent red-to-blue asymmetries in the broad emission lines.
  • Geometric precession of the inner disk drives additional weeks-scale variability while radial breathing produces intraday quasi-periodic oscillations.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The same tearing process may operate across a broader range of black hole spins and inclinations than the specific parameters simulated here.
  • Asymmetric line profiles evolving on similar timescales could serve as a distinctive observational test for disk tearing in other variable AGN.
  • Future wide-field surveys may catch the onset of these events and allow direct comparison with the simulated light-curve shapes.

Load-bearing premise

The chosen black hole mass, rapid spin, disk tilt, and torus-like broad line region model produce illumination patterns and line responses that match those in real changing-look AGN.

What would settle it

Detection or absence of time-evolving red-to-blue asymmetries in the broad emission lines during a changing-look event, or the predicted variability patterns in ULTRASAT and Vera Rubin Observatory light curves.

Figures

Figures reproduced from arXiv: 2511.09626 by Charlotte Ward, Jordy Davelaar, Matthew Liska, Nicholas Kaaz.

Figure 1
Figure 1. Figure 1: Three-dimensional gas density rendering of a torn disk with a cartoon depiction of the broad line region (BLR). Light col￾ors are high density, dark colors are low density. The majority of the emission emanates from the inner disk (yellow squiggles). This emission photoionizes the BLR, which is idealized as a rotating torus of optically thin gas located ∼ 45◦ above the outer disk (white region). Each segme… view at source ↗
Figure 2
Figure 2. Figure 2: Simulated light curves. Each curve exhibits roughly order-of-magnitude variability on months-to-years timescales. Panel a. Bolo￾metric isotropic-equivalent luminosity at 15◦ inclination and 0◦ azimuth (black). We also show M˙ rescaled to a luminosity assuming 10% radiative efficiency. Liso mostly tracks M˙ , but features some weeks-long periodicity due to the geometric precession of the inner disk. One exa… view at source ↗
Figure 3
Figure 3. Figure 3: Spacetime diagram of disk midplane density and tilt, which reveals repeated tearing cycles and, sometimes, transient alignment of the inner disk. Panel a. Midplane density, ρmidplane. Low-density (purple) regions indicate gaps between sub-disks or a recently-consumed inner disk. We have highlighted two tears with white lines; the outer disk will refill the inner region at a rate vr ≳ 10−2 vk (white dashed … view at source ↗
Figure 4
Figure 4. Figure 4: Effective temperature and luminosity per unit radius at time t − t0 = 40days. Panel a. The effective temperature of the disk as a function of radius. We also have labeled the radius of the tear, rtear. Panel b. The luminosity per unit radius, dL dr (Eq. 7), as a function of radius. We show curves both for the band-dependent luminosity and (0.1% of) the bolometric luminosity, where we have assumed that each… view at source ↗
Figure 5
Figure 5. Figure 5: Ray-traced images of the precessing inner disk (corre￾sponds to vertical green lines in Fig. 2a and Fig. 3b). We can see a ∼ 180◦ geometric precession from panel (a) to (d), which super￾imposes weeks-long periodicity in the light curve on top of the months-to-years long variability. The oscillations of the inner disk are presumably forced by time-dependent interactions with the outer disk. However, it rema… view at source ↗
Figure 7
Figure 7. Figure 7: Time series of synthetic optical spectra. We clearly see a temporary (near) disappearance of the broad Hα, Hβ and He I (λ = 5876Å) lines within a year, which defines this system as a CLAGN. The panels correspond to the green curves in Figs. 2 and [PITH_FULL_IMAGE:figures/full_fig_p008_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Evolving asymmetries in the Hα broad line. Panel a. We depict the profile of the Hα broad line as a function of time (see Fig. 2c for the integrated profile as a function of time). Panel b. We show the residuals of the profile shown in panel a, revealing a rich evolution of the broad line asymmetries that trace the evolution of the inner disk (see Sec. 3.4 for how we calculate the residuals). Panel c. We s… view at source ↗
Figure 9
Figure 9. Figure 9: Thermodynamic properties of disk at r = 25rg in φ− θ plane, tilted such that the local disk midplane coincides with θ = π/2 (see App. A for details). Panel a. We show the cooling function used in the simulation (Eq. A1). Panel b. We show our prescribed radiation temperature (Eq. A6). Panel c. We show the radiation temperature without prescribed warp-dependent non-axisymmetries (Eq. A6 with fψ = 1 [PITH_FU… view at source ↗
read the original abstract

Changing-look active galactic nuclei (CLAGN) feature order-of-magnitude variability in both the continuum and broad line luminosities on months-to-years long timescales, and are currently unexplained. Simulations have demonstrated that rotating black holes sometimes tear apart tilted accretion disks. These tearing events violently restructure the disk on timescales much shorter than a viscous timescale, hinting at a connection to CLAGN. Here, we show that disk tearing can power changing-look events. We report synthetic observations of an extremely high resolution three-dimensional general-relativistic magnetohydrodynamic simulation of a geometrically thin, tilted accretion disk around a rapidly rotating, $10^8\,M_\odot$ black hole. We perform ray-tracing calculations that follow the disk light to both a line of sight camera and to a distribution of cameras in a prescribed torus-like broad line region. The continuum photoionizes the broad line region and we calculate the resulting spectrum. Both the continuum and line luminosities undergo order of magnitude swings on months-to-years long timescales. We find shorter, weeks long variability driven by the geometric precession of the inner disk and an intraday quasi-periodic oscillation driven by radial breathing of the inner disk. When the torn disk precesses, it causes asymmetric illumination of the broad line region, driving time-evolving red-to-blue asymmetries of the broad emission lines that may be a smoking gun for disk tearing. We also make predictions for future photometric observations from ULTRASAT and Vera Rubin Observatory, both of which may play an important role in detecting future changing-look events.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript claims that disk tearing in a tilted, geometrically thin accretion disk around a rapidly spinning 10^8 M_⊙ black hole can power changing-look AGN events. An extremely high-resolution 3D GRMHD simulation is post-processed with ray-tracing to a distant observer and to a prescribed torus-like broad-line region; the resulting continuum and line luminosities exhibit order-of-magnitude swings on months-to-years timescales, with additional shorter-term variability from inner-disk precession and radial breathing, plus evolving red/blue line asymmetries.

Significance. If the central result holds, the work supplies a concrete, simulation-based mechanism that links GRMHD disk dynamics directly to the rapid continuum and emission-line changes observed in CLAGN, bypassing the usual viscous timescale. The production of synthetic light curves, line profiles, and explicit predictions for ULTRASAT and Vera Rubin Observatory observations adds immediate observational utility.

major comments (2)
  1. [Simulation setup (methods/results)] The simulation is performed at a single set of parameters (M = 10^8 M_⊙, high spin, chosen tilt). Because the reported order-of-magnitude luminosity swings and BLR illumination patterns depend on these choices, the claim that disk tearing can power CLAGN across the observed population would be substantially stronger if the authors showed that comparable variability persists under modest variations in mass, spin, or tilt (or provided a clear argument for why the chosen values are representative).
  2. [Results on synthetic observations and light curves] No quantitative comparison is presented between the simulated continuum and line light curves (amplitudes, timescales, or red/blue asymmetries) and existing CLAGN monitoring data. Without such a comparison, it remains unclear whether the reported variability amplitudes and line-profile evolution are consistent with observations or are specific to the adopted torus BLR geometry and photoionization treatment.
minor comments (2)
  1. [Methods] The abstract and main text refer to an 'extremely high resolution' run; explicit grid dimensions, cell aspect ratios, and any convergence tests performed on the tearing dynamics should be stated clearly in the methods section.
  2. [Post-processing and ray-tracing description] Notation for the broad-line region (torus-like distribution, camera placement) and the precise definition of 'order of magnitude' swings should be made explicit when first introduced to avoid ambiguity for readers unfamiliar with the post-processing pipeline.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful and constructive comments, which have helped us improve the manuscript. We respond to each major comment below and indicate the revisions made.

read point-by-point responses

  1. Referee: [Simulation setup (methods/results)] The simulation is performed at a single set of parameters (M = 10^8 M_⊙, high spin, chosen tilt). Because the reported order-of-magnitude luminosity swings and BLR illumination patterns depend on these choices, the claim that disk tearing can power CLAGN across the observed population would be substantially stronger if the authors showed that comparable variability persists under modest variations in mass, spin, or tilt (or provided a clear argument for why the chosen values are representative).

    Authors: We agree that demonstrating robustness across a wider parameter range would strengthen the generality of the conclusions. The extreme computational cost of the high-resolution GRMHD simulation limits us to the present high-fidelity case in this work. In the revised manuscript we have added a paragraph in the discussion that justifies the representativeness of the chosen mass, spin, and tilt based on observational constraints for CLAGN host black holes, and we explain how the relevant timescales scale with black-hole mass so that the results can be rescaled to other systems. revision: partial

  2. Referee: [Results on synthetic observations and light curves] No quantitative comparison is presented between the simulated continuum and line light curves (amplitudes, timescales, or red/blue asymmetries) and existing CLAGN monitoring data. Without such a comparison, it remains unclear whether the reported variability amplitudes and line-profile evolution are consistent with observations or are specific to the adopted torus BLR geometry and photoionization treatment.

    Authors: We have added a new subsection that directly compares the simulated continuum and line variability amplitudes and timescales with published monitoring data for several CLAGN. The time-evolving red/blue line asymmetries are placed in the context of observed profile variations. We have also clarified that the adopted BLR geometry is a standard torus prescription and that the main qualitative features remain robust under reasonable changes to the BLR model and photoionization treatment. revision: yes

Circularity Check

0 steps flagged

No significant circularity; variability emerges from forward simulation dynamics

full rationale

The paper's central result is obtained by evolving a GRMHD simulation of a tilted thin disk around a 10^8 M⊙ rapidly spinning black hole and then performing ray-tracing to a line-of-sight camera plus a prescribed torus-like BLR. Continuum and line luminosities, including order-of-magnitude swings and red/blue asymmetries, are computed outputs of the time-dependent tearing, precession, and radial breathing. No equation or claim reduces by construction to its own inputs, no parameter is fitted to CLAGN data and then relabeled a prediction, and no load-bearing uniqueness theorem or ansatz is imported via self-citation. The demonstration is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard GRMHD assumptions for disk evolution, a simplified torus model for the broad line region, and chosen values for black hole mass and spin that enable tearing; no new entities are postulated.

free parameters (2)
  • Black hole mass = 10^8 M_sun
    Set to 10^8 solar masses as a representative AGN value
  • Black hole spin = high
    Chosen to be rapid to permit disk tearing
axioms (2)
  • domain assumption General-relativistic magnetohydrodynamics accurately captures the dynamics of a tilted thin accretion disk
    Invoked as the foundation of the simulation method
  • domain assumption The broad line region can be represented as a static torus-like distribution of clouds photoionized by the disk continuum
    Used to compute the emission-line response

pith-pipeline@v0.9.0 · 5580 in / 1564 out tokens · 72923 ms · 2026-05-17T22:02:09.604207+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Forward citations

Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. SDSSJ110546.07+145202.4: The first long-duration radio changing-look NLS1 galaxy

    astro-ph.HE 2026-04 unverdicted novelty 7.0

    SDSSJ110546.07+145202.4 is the first known long-duration radio changing-look NLS1 galaxy whose outburst is explained by an accretion-rate change that triggered a powerful radio jet.

  2. Reshaping the inner shadow of a Kerr black hole by a torn accretion disk

    gr-qc 2026-04 conditional novelty 6.0

    Torn accretion disks around Kerr black holes erode the inner shadow and create bifurcated, crescent, and multi-ring shadow features driven by sub-disk discontinuities and outer tilt angle.

  3. Identifying Changing-Look AGN Transitions in Light Curve Data with the Zwicky Transient Facility

    astro-ph.GA 2026-04 unverdicted novelty 6.0

    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.

Reference graph

Works this paper leans on

49 extracted references · 49 canonical work pages · cited by 3 Pith papers

  1. [1]

    - [1] #1 = = ^ ^ ^ .\!\!^ d .\!\!^ h .\!\!^ m .\!\!^ s .\!\!^ @mss

    thebibliography [1] 20pt to REFERENCES 6pt =0pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command Each re...

    work page 2016

  2. [2]

    F 0j7 7-qERu P)JI(> ? q 0 K5>kx_0s 7KVO7R zU W9 93 9

    thebibliography [1] 20pt to REFERENCES 6pt =0pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command Each re...

    work page doi:10.5281/zenodo.831784 2017

  3. [3]

    1993, ARA&A, 31, 473, doi: 10.1146/annurev.aa.31.090193.002353

    Antonucci , R. 1993, , 31, 473, 10.1146/annurev.aa.31.090193.002353

    work page doi:10.1146/annurev.aa.31.090193.002353 1993

  4. [4]

    M., Petterson J

    Bardeen , J. M., & Petterson , J. A. 1975, , 195, L65, 10.1086/181711

    work page doi:10.1086/181711 1975

  5. [5]

    2018, , 613, A2, 10.1051/0004-6361/201732149

    Bronzwaer , T., Davelaar , J., Younsi , Z., et al. 2018, , 613, A2, 10.1051/0004-6361/201732149

    work page doi:10.1051/0004-6361/201732149 2018

  6. [6]

    M., Bentz , M

    Cackett , E. M., Bentz , M. C., & Kara , E. 2021, iScience, 24, 102557, 10.1016/j.isci.2021.102557

    work page doi:10.1016/j.isci.2021.102557 2021

  7. [7]

    Chatterjee , K., Liska , M., Tchekhovskoy , A., & Markoff , S. B. 2019, , 490, 2200, 10.1093/mnras/stz2626

    work page doi:10.1093/mnras/stz2626 2019

  8. [8]

    D., De Rosa , G., Croxall , K., et al

    Denney , K. D., De Rosa , G., Croxall , K., et al. 2014, , 796, 134, 10.1088/0004-637X/796/2/134

    work page doi:10.1088/0004-637x/796/2/134 2014

  9. [9]

    A., Huang , X., Davis , S

    Dodd , S. A., Huang , X., Davis , S. W., & Ramirez-Ruiz , E. 2025, arXiv e-prints, arXiv:2506.19900, 10.48550/arXiv.2506.19900

    work page doi:10.48550/arxiv.2506.19900 2025

  10. [10]

    W., & Ogilvie , G

    Fairbairn , C. W., & Ogilvie , G. I. 2021, , 508, 2426, 10.1093/mnras/stab2717

    work page doi:10.1093/mnras/stab2717 2021

  11. [11]

    2021, , 916, 61, 10.3847/1538-4357/ac07a6

    Feng , J., Cao , X., Li , J.-w., & Gu , W.-M. 2021, , 916, 61, 10.3847/1538-4357/ac07a6

    work page doi:10.3847/1538-4357/ac07a6 2021

  12. [12]

    2018, , 563, 657, 10.1038/s41586-018-0731-9

    Gravity Collaboration , Sturm , E., Dexter , J., et al. 2018, , 563, 657, 10.1038/s41586-018-0731-9

    work page doi:10.1038/s41586-018-0731-9 2018

  13. [13]

    M., Van Hoof P

    Gunasekera , C. M., van Hoof , P. A. M., Chatzikos , M., & Ferland , G. J. 2023, Research Notes of the American Astronomical Society, 7, 246, 10.3847/2515-5172/ad0e75

    work page doi:10.3847/2515-5172/ad0e75 2023

  14. [14]

    M., et al

    Horne , K., De Rosa , G., Peterson , B. M., et al. 2021, , 907, 76, 10.3847/1538-4357/abce60

    work page doi:10.3847/1538-4357/abce60 2021

  15. [15]

    LSST: From Science Drivers to Reference Design and Anticipated Data Products , journal =

    Ivezi \'c , Z ., Kahn , S. M., Tyson , J. A., et al. 2019, , 873, 111, 10.3847/1538-4357/ab042c

    work page doi:10.3847/1538-4357/ab042c 2019

  16. [16]

    Kaaz , N., Liska , M. T. P., Jacquemin-Ide , J., et al. 2023, , 955, 72, 10.3847/1538-4357/ace051

    work page doi:10.3847/1538-4357/ace051 2023

  17. [17]

    2025, , 979, 192, 10.3847/1538-4357/ad9a85

    Kaaz , N., Lithwick , Y., Liska , M., & Tchekhovskoy , A. 2025, , 979, 192, 10.3847/1538-4357/ad9a85

    work page doi:10.3847/1538-4357/ad9a85 2025

  18. [18]

    M., Cales , S., Moran , E

    LaMassa , S. M., Cales , S., Moran , E. C., et al. 2015, , 800, 144, 10.1088/0004-637X/800/2/144

    work page doi:10.1088/0004-637x/800/2/144 2015

  19. [19]

    , keywords =

    Lawrence , A. 2012, , 423, 451, 10.1111/j.1365-2966.2012.20889.x

    work page doi:10.1111/j.1365-2966.2012.20889.x 2012

  20. [20]

    2018, Nature Astronomy, 2, 102, 10.1038/s41550-017-0372-1

    ---. 2018, Nature Astronomy, 2, 102, 10.1038/s41550-017-0372-1

    work page doi:10.1038/s41550-017-0372-1 2018

  21. [21]

    B., Van Moer M., 2021, @doi [ ] 10.1093/mnras/staa099 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.507..983L 507, 983 ( @eprint arXiv 1904.08428 )

    Liska , M., Hesp , C., Tchekhovskoy , A., et al. 2021, , 507, 983, 10.1093/mnras/staa099

    work page doi:10.1093/mnras/staa099 2021

  22. [22]

    Liska , M. T. P., Chatterjee , K., Issa , D., et al. 2022, , 263, 26, 10.3847/1538-4365/ac9966

    work page doi:10.3847/1538-4365/ac9966 2022

  23. [23]

    L., Ross, N

    MacLeod , C. L., Ross , N. P., Lawrence , A., et al. 2016, , 457, 389, 10.1093/mnras/stv2997

    work page doi:10.1093/mnras/stv2997 2016

  24. [24]

    McKernan , B., Ford , K. E. S., Cantiello , M., et al. 2022, , 514, 4102, 10.1093/mnras/stac1310

    work page doi:10.1093/mnras/stac1310 2022

  25. [25]

    D., Giustini , M., et al

    Miniutti , G., Saxton , R. D., Giustini , M., et al. 2019, , 573, 381, 10.1038/s41586-019-1556-x

    work page doi:10.1038/s41586-019-1556-x 2019

  26. [26]

    A., & Voit , G

    Murray , N., Chiang , J., Grossman , S. A., & Voit , G. M. 1995, , 451, 498, 10.1086/176238

    work page doi:10.1086/176238 1995

  27. [27]

    2023, , 518, 1656, 10.1093/mnras/stac2754

    Musoke , G., Liska , M., Porth , O., van der Klis , M., & Ingram , A. 2023, , 518, 1656, 10.1093/mnras/stac2754

    work page doi:10.1093/mnras/stac2754 2023

  28. [28]

    1985, , 289, 451, 10.1086/162906

    Netzer , H. 1985, , 289, 451, 10.1086/162906

    work page doi:10.1086/162906 1985

  29. [29]

    2015, ARA&A, 53, 365, doi: 10.1146/annurev-astro-082214-122302

    ---. 2015, , 53, 365, 10.1146/annurev-astro-082214-122302

    work page Pith review doi:10.1146/annurev-astro-082214-122302 2015

  30. [30]

    2012, , 757, L24, 10.1088/2041-8205/757/2/L24

    Nixon , C., King , A., Price , D., & Frank , J. 2012, , 757, L24, 10.1088/2041-8205/757/2/L24

    work page doi:10.1088/2041-8205/757/2/l24 2012

  31. [31]

    C., Krolik , J

    Noble , S. C., Krolik , J. H., & Hawley , J. F. 2009, , 692, 411, 10.1088/0004-637X/692/1/411

    work page doi:10.1088/0004-637x/692/1/411 2009

  32. [32]

    Ogilvie , G. I. 1999, , 304, 557, 10.1046/j.1365-8711.1999.02340.x

    work page doi:10.1046/j.1365-8711.1999.02340.x 1999

  33. [33]

    Papaloizou , J. C. B., & Pringle , J. E. 1983, , 202, 1181, 10.1093/mnras/202.4.1181

    work page doi:10.1093/mnras/202.4.1181 1983

  34. [34]

    , keywords =

    Perego , A., Dotti , M., Colpi , M., & Volonteri , M. 2009, , 399, 2249, 10.1111/j.1365-2966.2009.15427.x

    work page doi:10.1111/j.1365-2966.2009.15427.x 2009

  35. [35]

    Peterson , B. M. 2006, in Physics of Active Galactic Nuclei at all Scales, ed. D. Alloin , Vol. 693 (Springer, Berlin and Heidelberg), 77, 10.1007/3-540-34621-X_3

    work page doi:10.1007/3-540-34621-x_3 2006

  36. [36]

    Pringle , J. E. 1981, , 19, 137, 10.1146/annurev.aa.19.090181.001033

    work page doi:10.1146/annurev.aa.19.090181.001033 1981

  37. [37]

    , keywords =

    ---. 1992, , 258, 811, 10.1093/mnras/258.4.811

    work page doi:10.1093/mnras/258.4.811 1992

  38. [38]

    Raj , A., & Nixon , C. J. 2021, , 909, 82, 10.3847/1538-4357/abdc25

    work page doi:10.3847/1538-4357/abdc25 2021

  39. [39]

    2023, Changing-look active galactic nuclei, Nature Astronomy, 7, 1282, doi: 10.1038/s41550-023-02108-4

    Ricci , C., & Trakhtenbrot , B. 2023, Nature Astronomy, 7, 1282, 10.1038/s41550-023-02108-4

    work page doi:10.1038/s41550-023-02108-4 2023

  40. [40]

    The Astrophysical Journal Letters , author =

    Ricci , C., Kara , E., Loewenstein , M., et al. 2020, , 898, L1, 10.3847/2041-8213/ab91a1

    work page doi:10.3847/2041-8213/ab91a1 2020

  41. [41]

    C., & Dexter , J

    Scepi , N., Begelman , M. C., & Dexter , J. 2021, , 502, L50, 10.1093/mnrasl/slab002

    work page doi:10.1093/mnrasl/slab002 2021

  42. [42]

    I., & Sunyaev , R

    Shakura , N. I., & Sunyaev , R. A. 1973, , 24, 337

    work page 1973

  43. [43]

    J., Prieto , J

    Shappee , B. J., Prieto , J. L., Grupe , D., et al. 2014, , 788, 48, 10.1088/0004-637X/788/1/48

    work page Pith review doi:10.1088/0004-637x/788/1/48 2014

  44. [44]

    2024, , 964, 74, 10.3847/1538-4357/ad2704

    Shvartzvald , Y., Waxman , E., Gal-Yam , A., et al. 2024, , 964, 74, 10.3847/1538-4357/ad2704

    work page doi:10.3847/1538-4357/ad2704 2024

  45. [45]

    2020, , 641, A167, 10.1051/0004-6361/202038575

    Sniegowska , M., Czerny , B., Bon , E., & Bon , N. 2020, , 641, A167, 10.1051/0004-6361/202038575

    work page doi:10.1051/0004-6361/202038575 2020

  46. [46]

    L., et al

    Trakhtenbrot , B., Arcavi , I., MacLeod , C. L., et al. 2019, , 883, 94, 10.3847/1538-4357/ab39e4

    work page doi:10.3847/1538-4357/ab39e4 2019

  47. [47]

    Ulrich , M.-H., Maraschi , L., & Urry , C. M. 1997, , 35, 445, 10.1146/annurev.astro.35.1.445

    work page doi:10.1146/annurev.astro.35.1.445 1997

  48. [48]

    E., Wilhite , B

    Vanden Berk , D. E., Wilhite , B. C., Kron , R. G., et al. 2004, , 601, 692, 10.1086/380563

    work page doi:10.1086/380563 2004

  49. [49]

    A., Telfer , R

    Zheng , W., Kriss , G. A., Telfer , R. C., Grimes , J. P., & Davidsen , A. F. 1997, , 475, 469, 10.1086/303560

    work page doi:10.1086/303560 1997