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REVIEW 3 major objections 6 minor 245 references

The physical mechanism for two rapid changing-look AGNs: SDSS J0225+0030 and SDSS J1723+5504

T0 review · 3 major / 6 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read The revised model attributes the rapid turn-ons of SDSS J0225+0030 and SDSS J1723+5504 to the collapse of an inner hot accretion flow, with cooling times comparable to the observed 254-day and 142-day transitions.

desk verdict A transparent, incremental revision of the authors' own ADAF-cooling model that turns two outlier CL AGNs into borderline successes, but the exact match relies on an unmeasured accretion-rate ratio and a clean flux decomposition that is not robustly tested. read the letter →

arxiv 2608.01249 v1 pith:BBKM2XVF submitted 2026-08-02 astro-ph.GA

Shuang-Liang Li , Xinwu Cao , Wei-Min Gu This is my paper · ORCID
classification astro-ph.GA
keywords changing-lookAGNaccretiondiskadvection-dominatedflowtransitionradiuscoolingtimescalesupermassiveblackholeviscousSDSSJ0225+0030
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper addresses two changing-look active galactic nuclei that switched on in less than a year, faster than standard disk models can easily produce. It argues that the earlier ADAF-collapse explanation failed for these two only because the transition radius was overestimated, and that using the observed 5100 Å flux change to locate that radius makes the predicted ADAF cooling times comparable to the observed 254-day and 142-day transitions. Because these black holes are massive (about $10^9$ solar masses) and accrete at only about one percent of Eddington, the disk is cool enough that a modest inward move of the hot inner flow can halve the optical flux. If right, the result removes the two outlier objects from the sample and strengthens the case that rapid changing-look events are accretion-mode transitions rather than obscuration or tidal disruptions.

What carries the argument

The load-bearing object is the transition radius $R_{\rm tr}$ between the inner ADAF and the outer thin disk, because the ADAF cooling time scales as $t_{\rm cool}\propto \Omega_K^{-1}\propto R_{\rm tr}^{3/2}$. The paper replaces the earlier temperature-based estimate with a flux-based one: equations (1)--(3) compute the 5100 Å flux from a multicolor thin disk with an inner edge at $R_{\rm tr}$, and the observed ratio $L'_{5100}/L_{5100}$ fixes $R_{\rm tr}$ under the assumption that the inner ADAF contributes no 5100 Å light. A second curve relates the flux ratio to the accretion-rate ratio $\dot m'/\dot m$, showing the degeneracy between a smaller $R_{\rm tr}$ and a lower dim-state accretion rate.

What would settle it

A high-cadence spectroscopic campaign that caught either object completing its transition in well under 254 or 142 days rest frame, or a spectral decomposition showing that the dim-state 5100 Å continuum contains a substantial component from the inner hot flow or host stars rather than only the outer thin disk, would settle the claim against the model.

Watch

Extended reading notes

Core claim

The paper claims that the sub-year turn-on times of SDSS J0225+0030 and SDSS J1723+5504 can be explained by the collapse of an inner advection-dominated accretion flow (ADAF) into a thin disk, provided the transition radius $R_{\rm tr}$ is inferred from the observed 5100 Å flux ratio between the dim and bright states rather than from a rough temperature criterion. With the flux ratio alone and a constant mass accretion rate, the inferred transition radii drop from $78.1\,R_s$ to $14.89\,R_s$ and from $158.4\,R_s$ to $30.48\,R_s$ for the two objects, shortening the ADAF cooling times from thousands of days to $342$ and $197$ days. Allowing the accretion rate to drop in the dim state pushes the required $R_{\rm tr}$ even smaller, so the cooling time can be made shorter than the observed upper limits of $254$ and $142$ days. The paper also shows that a large-scale poloidal magnetic field, though it shortens thin-disk viscous timescales by about three orders of magnitude, still leaves them far longer than one year for these objects.

Load-bearing premise

The argument assumes that the only thing changing between the dim and bright states is where the hot inner disk begins, with no other source of 5100 Å light and no change in how much gas falls in; if starlight, the inner hot flow, or a changing accretion rate shifts the balance, the predicted timescales change substantially.

Editorial extensions

If this is right

  • The two fastest turn-on changing-look AGNs no longer require exotic mechanisms; the same ADAF-collapse process that explains the broader sample can account for them once $R_{\rm tr}$ is measured from the flux change.
  • High-cadence spectroscopic monitoring of these objects should find transitions that are consistent with the predicted cooling times, and any further shortening of the observed upper limits would tighten the allowed $\dot m'/\dot m$ parameter space.
  • Large black hole mass and low Eddington ratio make an AGN a good candidate for rapid changing-look behavior, because the low disk temperature lets a small inward move of the inner flow produce a large optical flux change.
  • In the constant-accretion-rate case, the model predicts that the thin disk in the dim state is truncated at about $15\,R_s$ and $30\,R_s$ for the two objects, a geometry that could be tested with detailed continuum fitting or reverberation mapping.
  • A large-scale poloidal magnetic field acting on a thin disk is insufficient to explain sub-year transitions in these two objects, so the ADAF-collapse channel is the preferred explanation.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The same flux-ratio method could be applied to other changing-look AGNs with multi-epoch spectra, converting each measured 5100 Å flux change into a predicted transition timescale and giving a ready-made test of the ADAF-collapse scenario across a larger sample.
  • Because the observed transition timescales are upper limits and the constant-accretion-rate predictions already exceed them, the model's success leans on allowing the accretion rate to drop in the dim state; a decisive check would be independent dim-state accretion-rate indicators, such as X-ray or UV luminosity, falling in the inferred $\dot m'/\dot m$ ranges.
  • If the inner ADAF or host starlight contributes a measurable fraction of the dim-state 5100 Å continuum, the inferred $R_{\rm tr}$ would move outward and the predicted cooling time would grow, so high-quality spectral decomposition of the dim-state continuum directly tests the paper's central mapping.
  • The reverse process, a turn-off where the thin disk recedes and an ADAF reforms, should obey the same flux-ratio relation with a heating timescale, suggesting that turn-off changing-look AGNs with well-sampled light curves could be used as independent checks of the model.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 6 minor

Summary. The paper revisits two rapidly changing-look AGNs, SDSS J0225+0030 and SDSS J1723+5504, whose observed transition timescales are shorter than one year and which were outliers in the ADAF-collapse model of Li & Cao (2025, LC2025). The authors first show that a thin disk with a large-scale poloidal magnetic field cannot reproduce the observed timescales, then revise the LC2025 model by estimating the ADAF/outer-disk transition radius R_tr from the observed ratio of dim-state to bright-state 5100 Å flux using standard thin-disk flux integrals. With a constant mass accretion rate, the inferred R_tr values give cooling timescales of 342 days and 197 days for the two objects, compared with observed upper limits of 254 days and 142 days. Allowing the dim-state accretion rate to be lower than the bright-state value gives mdot'/mdot ranges of about 74%--91% and yields R_tr values that make the cooling timescale equal to the observed transition timescale. The revised model is then applied to the full LC2025 sample.

Significance. If the result holds, the paper would offer a plausible explanation for the short transition timescales in two previously problematic CL AGNs and would strengthen the LC2025 cooling-collapse scenario. The approach is transparent: the flux-integral calculation is simple and reproducible, the magnetic-field appendix provides a concrete negative result, and the application to the full sample is a useful consistency check. The main novelty is using the observed 5100 Å flux variation to locate the transition radius rather than relying on a temperature criterion. However, the quantitative match is not yet a free prediction: it is completed by allowing the unconstrained ratio mdot'/mdot to vary, and the dominant systematic in the flux decomposition is not estimated. The central claim is therefore plausible but currently under-supported.

major comments (3)
  1. [§3, Figures 1–2 and Table 1] The central claim that the cooling timescale is 'comparable to' the observed transition timescale is not established as a prediction. In the constant-mdot case, the model gives t_cool = 342 days and 197 days, which exceed the observed upper limits of 254 days and 142 days listed in Table 1. Agreement is achieved only by allowing mdot'/mdot to vary, and the quoted ranges are obtained by first setting t_cool = t_tran, which selects R_tr = 12.21 R_s and 24.5 R_s from the degeneracy curve in Figure 2, and then reading off mdot'/mdot. Because mdot'/mdot is not independently measured, the reported agreement is a consistency condition rather than a test of the model. The paper should either be reframed as an allowed parameter-space consistency check, with clear language, or provide an independent observational constraint on mdot'/mdot.
  2. [§2, Eqs. (1)–(2), Table 1 note] The inferred R_tr rests entirely on the assumption that the dim-state 5100 Å flux is produced by the outer thin disk, with no contribution from the inner ADAF and no host-galaxy starlight. Since t_cool ∝ R_tr^{3/2}, any contamination in the observed L'_5100/L_5100 ratio propagates nonlinearly into the predicted timescale. The note to Table 1 correctly states that the quoted uncertainties are only formal spectral-fitting errors, but the dominant systematic is the flux decomposition and it is not estimated. If even roughly ten percent of the dim-state flux is host starlight or ADAF emission, the intrinsic disk-flux ratio is lower than 74.1% and 69.2%, R_tr becomes larger, and the already marginal constant-mdot agreement worsens. The authors should quantify this systematic using the available spectra or justify its neglect with a specific argument.
  3. [§1 and Table 1, col. (7)] The observed transition timescales for both objects are upper limits, as the text itself notes: SDSS J1723+5504 has only two epochs and SDSS J0225+0030 has an intermediate observation that still gives an upper limit. The analysis nevertheless treats t_tran as exact when setting t_cool = t_tran and deriving the allowed mdot'/mdot ranges. If the true transition timescale is shorter than the quoted upper limit, the required R_tr is smaller and the inferred mdot'/mdot range shifts. The comparison should be formulated as inequalities, t_cool ≤ t_tran,upper, and the allowed parameter space should be presented as such rather than as a single curve crossing.
minor comments (6)
  1. [Title and Abstract] The title contains 'SD SS J0225+0030' with a spurious space; it should read 'SDSS J0225+0030' consistently throughout.
  2. [§3, after Eq. (4)] The text uses 'Angstrom' instead of the proper symbol 'Å', and Eq. (4) should state the dimensions of the numerical constant explicitly, since the constant is dimensional.
  3. [Table 2 and Figure 3] It is not clear whether the full-sample comparison in Figure 3 uses the constant-mdot or variable-mdot variant, and whether the two target objects are plotted with the tuned mdot'/mdot values or with the constant-mdot values. Please clarify which model variant produced the points in Figure 3.
  4. [Figure 4 note] The Figure 4 note mentions revised-model R_tr values of 10.83 R_s and 21.52 R_s, but these do not appear in Table 1; please define them and explain how they are obtained.
  5. [Abstract and §1] The statement that the magnetic-field model timescale 'remains significantly longer than one year' is vague; the appendix gives values of order 10^6 days for strong magnetic fields, which is many orders of magnitude longer than one year and should be stated precisely.
  6. [§3, parameter range] The inequality '74.13% < mdot'/mdot < 90.99%' uses 74.13%, the observed flux ratio, as the lower bound; since the lower limit is set by R_tr = 3 R_s, this should be stated as equal to the observed ratio, 74.1%, or the provenance should be clarified.

Circularity Check

1 steps flagged · score 6.0 of 10

Variable-ṁ branch sets R_tr from the observed t_tran, then reports that t_cool can satisfy t_cool < t_tran; the agreement is partly constructed.

  1. fitted input called prediction [Section 3, paragraph introducing Figure 2 (parameter space satisfying t_cool < t_tran)]
    "For the observed transition times of 254 (SDSS J0225+0030) and 142 (SDSS J1723+5504) days , the corresponding Rtr are 12.21 Rs and 24.5 Rs, respectively. Therefore, the parameter space defined by 3 Rs < R tr < 12.21Rs (implying 74.13% < ˙m′/ ˙m < 90.99%) can satisfy the condition tcool < t tran for SDSS J0225+0030."

    The two R_tr values are obtained by inverting t_cool(R_tr) = t_tran, because the paper states in §2 that t_cool ∝ R_tr^{3/2}, and the Figure 2 caption labels these R_tr values as the points where t_cool = t_tran. The subsequent claim that a parameter space can satisfy t_cool < t_tran is therefore a restatement of having chosen R_tr below the equality threshold, not a tested prediction. The unmeasured ratio ṁ′/ṁ is the fitted knob: the observed t_tran selects the boundary of the allowed range, and any value of ṁ′/ṁ below the boundary gives agreement by construction. The independent constant-ṁ branch gives t_cool = 342 d and 197 d, which the paper itself notes are longer than the observed upper limits of 254 d and 142 d.

full rationale

The core derivation is not circular up to the constant-ṁ calculation: Eqs. (1)–(3) convert an observed flux ratio L′_5100/L_5100 into R_tr, and the LC2025 cooling-time scaling then yields t_cool. That is a genuine model prediction, and it is cleanly falsifiable — for these two objects it fails, as the paper admits (342 > 254 d and 197 > 142 d). The circularity enters only in the variable-ṁ route: the observed t_tran is fed back through t_cool ∝ R_tr^{3/2} to choose R_tr = 12.21 R_s and 24.5 R_s, and the quoted ṁ′/ṁ ranges are then read off as the parameter space that satisfies t_cool < t_tran. This makes the headline claim that the cooling timescales are comparable to the observed transition timescales at least partly constructed rather than independently predicted. Because the constant-ṁ branch is an independent calculation and the paper is explicit that the variable-ṁ branch defines a parameter space, the circularity is partial rather than total. The systematic concern that host-galaxy or ADAF contamination could shift the inferred R_tr is a correctness/robustness issue, not an additional circularity.

Assumptions & free parameters 2 free parameters · 5 assumptions · 0 invented entities

The central timescale comparison rests on two adjustable inputs: the unmeasured dim-state accretion-rate ratio mdot'/mdot (used to tune R_tr so t_cool matches t_tran) and the LC2025 cooling-timescale normalization, which encodes ADAF physics (alpha, f_adv, spin) and is adopted from the authors' prior paper without re-derivation. The flux-to-R_tr mapping also assumes the standard thin disk blackbody model and neglects ADAF and host-galaxy contributions. No new entities are introduced.

free parameters (2)
  • mdot'/mdot (dim-state to bright-state mass accretion rate ratio) = not fixed; allowed ranges 0.741-0.910 (J0225) and 0.692-0.897 (J1723), chosen so t_cool <= t_tran
    The flux ratio L'_5100/L_5100 provides one constraint for two unknowns (R_tr and mdot'/mdot). The paper plots the degeneracy and uses the observed transition timescale to select the R_tr (12.21 R_s and 24.5 R_s) that makes t_cool = t_tran, then quotes the allowed mdot'/mdot range. This is an effectively fitted parameter, not an independent measurement.
  • Cooling timescale normalization C in t_cool = C Omega_K^{-1} = inherited from LC2025, not re-derived here
    The absolute value of t_cool depends on the ADAF model parameters (alpha, f_adv, spin) from Li and Cao (2025). The paper adopts t_cool ~ R^{3/2} with LC2025's normalization; uncertainties in these model parameters are explicitly excluded from the error budget (Table 1 footnote).
assumptions (5)
  • domain assumption Shakura-Sunyaev thin disk emits locally as a blackbody with effective temperature T_eff given by Eq. (3); the optical flux is the integral (1)-(2).
    Used to convert the observed 5100 Angstrom flux ratio into R_tr. Standard but assumes no Comptonization or color correction.
  • domain assumption In the dim state the accretion flow is an inner ADAF plus an outer thin disk, and the inner ADAF contributes negligibly to the 5100 Angstrom flux, so the dim-state flux is the thin-disk integral from R_tr to R_out.
    Taken from Ruan et al. (2019), Lyu et al. (2022), and LC2025. If the ADAF or a hot corona contributes at 5100 Angstroms, the inferred R_tr is wrong.
  • domain assumption The cooling timescale of the ADAF at R_tr is t_cool = C Omega_K^{-1}(R_tr) with C from LC2025; this is the timescale for the inner ADAF to collapse into a thin disk when the accretion rate rises.
    The central timescale comparison rests entirely on this formula, which is cited from the authors' own LC2025 paper and is not re-derived or numerically verified here.
  • domain assumption Schwarzschild black hole (a* = 0) and R_in = 3 R_s for the bright-state thin disk; the authors argue Kerr effects are minor at 5100 Angstroms.
    Used in Eqs. (1)-(3). The paper asserts qualitatively the same results for Kerr without a calculation; spin uncertainty is excluded from the error bars.
  • domain assumption The two observed transition timescales (254 days and 142 days in the rest frame) are treated as proxies for the physical transition times; both are upper limits because of sparse sampling.
    Stated in the introduction. If higher-cadence observations give much shorter timescales, the agreement worsens.

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Cite this review

Pith. "Pith review of The physical mechanism for two rapid changing-look AGNs: SDSS J0225+0030 and SDSS J1723+5504." pith.science (2026). https://pith.science/paper/BBKM2XVF

@misc{pith2026260801249,
  author       = {Pith},
  title        = {Pith review of: The physical mechanism for two rapid changing-look AGNs: SDSS J0225+0030 and SDSS J1723+5504},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/BBKM2XVF}},
  note         = {Machine review of arXiv:2608.01249}
}
abstract

SDSS J0225+0030 and SDSS J1723+5504 are two turn-on changing-look active galactic nuclei (CL AGNs) with transition timescales shorter than one year. Such short timescales pose a challenge for the current physical models of CL AGNs. We investigate this issue by exploring two possible mechanisms in this work. First, we consider the effect of a large-scale magnetic field on the viscous timescale, which can increase the radial velocity of the accretion disk. However, it is found that the timescale given by this model remains significantly longer than one year. Second, we improve the model of \citet{2025ApJ...988..207L}, which proposed that the inner thin disk in the bright state may form through the collapse of an advection-dominated accretion flow (ADAF) in the dim state, rather than being replaced by the advection of the outer thin disk. We re-estimate the transition radius $R_{\rm tr}$ between the inner ADAF and the outer thin disk through the observed variation of optical flux between the bright state and dim state. It is found that $R_{\rm tr}$ can be significantly reduced in these two objects owing to the lower gas temperature in the inner disk region (of the order of $10^4$ K), resulting from their large black hole masses ($\sim 10^9 M_{\odot}$) and small Eddington-scaled mass accretion rates ($\sim 0.01$). The cooling timescales given by the revised model in these two objects are found to be comparable to the observed transition timescales.

Figures

Figures reproduced from arXiv: 2608.01249 by the authors.

Figure 1
Figure 1. Upper panel: variation of the ratio between the optical flux (5100 ˚A) of the dim state and the bright state with the transition radius of a thin accretion disk for SDSS J0225+0030 (the red solid line), where the blue dashed line represents f ′ ν,5100/fν,5100 = 74.13%. Lower panel: same as upper panel, but for the object SDSS J1723+5504, where the blue dashed line represents f ′ ν,5100/fν,5100 = 69.2%. respectively.… view at source ↗
Figure 2
Figure 2. Upper panel: variation of the mass accretion rate ratio between the dim state and bright state as a function of the transition radius Rtr for SDSS J0225+0030 (the red solid line), where the blue dashed line represents Rtr = 12.21Rs (tcool = ttran). Lower panel: same as upper panel, but for the object SDSS J1723+5504, where the blue dashed line represents Rtr = 24.5Rs (tcool = ttran) [PITH_FULL_IMAGE:figures/full_fi… view at source ↗
Figure 3
Figure 3. Comparison of the observed transition timescales ttran of CL AGNs with the cooling timescales tcool given by our new model, where the solid red line represents ttran = tcool. The two red dots with error bars represent SDSS J0225+0030 and SDSS J1723+5504, respectively. the inner disk region. The maximum temperatures in SDSS J0225+0030 and SDSS J1723+5504 are only 3.3 × 104K and 5.5 × 104K, respectively. Therefore, th… view at source ↗
Figures from the paper (1 more)
Figure 4
Figure 4. Figure 4: Upper panel: viscous timescale as functions of radius for SDSS J0225+0030, where the black hole mass Mbh = 1.86 × 109M⊙, viscosity parameter α = 0.1 and mass accretion rate log ˙m = −2.15 ( ˙m = M /˙ M˙ Edd, where M˙ and M˙ Edd are the Eddington scaled mass accretion r…

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