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AT2021aeuk: A Repeating Partial Tidal Disruption Event Candidate in a Narrow-line Seyfert 1 galaxy

T0 review · 3 major / 5 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read The paper argues that AT2021aeuk, a transient in a narrow-line Seyfert 1 galaxy that flared twice in three years, is a repeating partial tidal disruption event candidate whose second flare comes from the debris stream colliding with the…

desk verdict A well-observed repeating transient in an NLS1 with a striking X-ray/optical anti-correlation; the repetition statistics are weaker than claimed, but the data merit a serious referee. read the letter →

arxiv 2501.01824 v2 pith:YX5WFDUN submitted 2025-01-03 astro-ph.HE astro-ph.GA

Jingbo Sun , Hengxiao Guo , Minfeng Gu , Ya-Ping Li , Yongjun Chen , D. González-Buitrago , Jian-Guo Wang , Sha-Sha Li
show 8 more authors
Hai-Cheng Feng Dingrong Xiong Yanan Wang Qi Yuan Jun-Jie Jin Wenda Zhang Hongping Deng Minghao Zhang
This is my paper · ORCID
classification astro-ph.HEastro-ph.GA
keywords tidaldisruptioneventrepeatingpartialTDEnarrow-lineSeyfert1galaxyaccretiondiskX-raycoronareverberationmappingopticaltransientAGN
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

The paper reports AT2021aeuk, a transient in a narrow-line Seyfert 1 galaxy that produced two similar optical flares about three years apart, plus a smaller precursor. The authors argue these are repeating partial tidal disruption events (rpTDEs): a star that is only partly destroyed each pass, with the second flare caused by the debris stream crashing into the inner accretion disk. That collision, the paper claims, triggers the optical flare while depleting the inner disk and destroying the X-ray corona, producing the observed V-shaped X-ray light curve that lags the optical by about 40 days. If the interpretation is right, AT2021aeuk joins a small set of rpTDEs in active galaxies and gives a physical explanation for X-ray/optical anti-correlation in such events. The paper also notes that a stellar-mass black hole merger in the disk could mimic these flares, and it predicts a third flare around September 2026.

What carries the argument

The load-bearing mechanism is the stream-disk collision in a repeating partial tidal disruption. In this picture, the star's orbital pericenter is near the tidal radius (about 12 $R_g$ for a $10^{6.9} M_\odot$ black hole), the debris stream follows a highly eccentric orbit with $1 - e_{\min} \approx 0.01$, and the stream hits the inner accretion disk at a distance given by $R_c = (a^2 - f^2)/(a \pm f \sin\theta)$. With an assumed inclination of 60 degrees, the two collision points lie at roughly 1 and 14 tidal radii, or 12 and 160 $R_g$. The shock from the collision dissipates kinetic energy into the UV/optical flare, drains the inner disk, and cuts off the corona's fuel supply, producing the V-shaped X-ray dip and its lag; the late-time UV dip below the pre-outburst level is the depleted disk region. The measured $\sim$40-day optical-to-X-ray lag and the $\sim$25-day Balmer lag are quantitative constraints that the mechanism must reproduce.

What would settle it

Monitor AT2021aeuk through the predicted third flare in September 2026 in optical and X-ray: if the third optical flare does not occur, or if it occurs without the V-shaped X-ray dip lagged by roughly 40 days, the repeating partial TDE picture is falsified. A decisive secondary check is to measure X-ray absorption during the dip: if an absorbing column appears while the X-ray spectrum hardens, the dip could be obscuration rather than coronal destruction.

Watch

Extended reading notes

Core claim

AT2021aeuk, coincident with the center of the narrow-line Seyfert 1 galaxy SDSS J161259.83+421940.3 at $z=0.2336$, brightened in 2019 and again in 2023 with similar g-band light curve shapes, colors, and blackbody temperatures, after being stable within about 0.1 magnitude for 15 years. During the second flare, Swift monitoring revealed an X-ray light curve shaped like a V: the X-ray luminosity dropped as the optical rose, reached its faintest state, and recovered to the pre-outburst level within roughly 150 days, while the optical flare led the X-ray dip by $39.9^{+15.2}_{-15.0}$ days with an ICCF coefficient near $-0.8$. New broad components in H$\alpha$ and H$\beta$ appeared during the second flare with a reverberation lag of about 25 days, consistent with the pre-existing broad-line region. The authors interpret the dual flares as a repeating partial TDE: the fallback stream from a partially disrupted solar-type star collides with the inner accretion disk at roughly 12 to 160 gravitational radii, producing the optical flare and partially destroying the X-ray corona, while the late-time UV dip below the pre-outburst level is the depleted disk interior to the collision point.

Load-bearing premise

The two bright flares and the precursor are causally connected episodes from a single repeating object rather than independent nuclear transients; the paper's argument for this depends on an assumed TDE rate of about $3\times10^{-5}$ per galaxy per year, a number with large systematic uncertainties.

Editorial extensions

If this is right

  • If the interpretation is right, a third flare should arrive around September 2026 with a similar optical shape and a matching X-ray dip trailed by roughly 40 days.
  • Stream-disk collisions become a plausible observable mechanism for X-ray/optical anti-correlation in AGN, and the $\sim$40-day lag provides a direct constraint on the collision radius and disk properties.
  • The new broad Balmer components with a $\sim$25-day reverberation lag imply that rpTDEs in AGNs can still map the pre-existing broad-line region and black hole mass, even during a flare.
  • The weaker second flare (about 0.65 times the first) fits the picture of a star that gains orbital energy after each partial disruption, giving a way to measure the mass stripped per encounter.
  • The late-time UV dip below the pre-outburst level, if it repeats, becomes a signature of inner-disk depletion and a measure of how long the disk takes to refill.

Reading between the lines

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

  • If the third flare repeats the same pattern, the V-shaped X-ray dip would be the cleanest coronal-disruption signature found so far, because the X-ray spectra show a power law with no absorption column; high-resolution X-ray spectroscopy during the dip could confirm whether the corona is truly removed or merely obscured.
  • The degeneracy between the rpTDE and stellar-mass black hole merger scenarios can be broken by timing and amplitude: rpTDEs should show gradually decreasing flare energy and drifting periods as the star loses mass, while a disk-embedded merger would produce very regular periods and stable amplitudes.
  • The statistical argument that independent flares are unlikely (probability $\sim$1e-8 within the same database) depends on the adopted TDE rate; if AGN environments boost TDE rates by an order of magnitude, the case for a causal connection weakens substantially, so the rates are worth refining with larger AGN samples.
  • Monitoring AT2021aeuk's UVW1 light curve through the 2026 flare will test whether the $>$200-day refilling time of the inner disk is a constant delay in every cycle, which would constrain the viscosity of the inner AGN disk.
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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 / 5 minor

Summary. AT2021aeuk is a transient in the NLS1 galaxy SDSS J161259.83+421940.3 at z=0.2336 that shows two optical flares separated by about three years plus a precursor flare. The paper presents multi-wavelength monitoring during the second flare: Swift UV/X-ray, ZTF and LJT optical photometry, GTC/LJT/XLT spectroscopy, VLA radio, and WISE mid-infrared data. The key observational claims are: an X-ray light curve with a V-shaped dip that anti-correlates with the optical flare, with an ICCF lag of 39.9 (+15.2/-15.0) days; a new broad component in the Balmer lines appearing during the second flare, with a reverberation lag of about 25 days; and positive UV/optical/MIR continuum lags. The authors propose that the dual flares are a repeating partial tidal disruption event (rpTDE) in an AGN, in which the fallback stream collides with the inner accretion disk, producing the optical flare and partially destroying the X-ray corona. They also discuss a stellar-mass black-hole merger in the disk as an alternative explanation and predict a third flare around September 2026 assuming a constant period.

Significance. If the rpTDE interpretation holds, AT2021aeuk would be one of very few repeating TDE candidates in an AGN, and the anti-correlated X-ray/optical evolution would provide a rare probe of stream-disk interactions and coronal destruction. The paper's strengths are its rapid and broad multi-wavelength follow-up, the careful spectral decomposition of the Balmer lines, a quantitative (though simplified) collision-geometry estimate, comparison with known TDE and ambiguous-nuclear-transient samples, and an explicit and falsifiable prediction of a third flare. The authors also honestly discuss an alternative sBH-merger scenario. The central observational dataset is valuable, and the paper does not overclaim certainty. However, the statistical case for repetition and the robustness of the X-ray/optical anti-correlation need to be substantially strengthened before the 'repeating' classification is secure.

major comments (3)
  1. [Section 4.2]
  2. [Section 2.3 and Section 3.2]
  3. [Section 4.1]
minor comments (5)
  1. [Table 2]
  2. [Section 3.3 and Appendix B]
  3. [Figure 10 and Section 3.2]
  4. [Section 4.1, Equations (1)-(2)]
  5. [Section 3.1.1]

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the interpretation rests on direct measurements, external comparisons, and explicitly labeled assumptions rather than on fitted quantities or self-citations.

full rationale

AT2021aeuk's central interpretive claims do not reduce to their inputs. The rpTDE interpretation is offered as a candidate explanation ('We propose that the dual-flare may be linked to a repeating partial TDE'), explicitly contrasted with an sBH-merger alternative that the authors say they cannot rule out. The X-ray/optical anti-correlation and ~40-day lag are measured directly via ICCF, not generated by a fitted model. The collision-point estimate in Section 4.1 adopts stated external assumptions (solar-type star, 60-degree median inclination, Rp=Rt, and the Bonnerot & Stone 2021 eccentricity relation) and yields a range of 12-160 Rg that is only compared for consistency with the observed lag; no parameter is fitted to the lag and then re-presented as a prediction. The third-flare prediction in Section 4.2.1 and Table 2 is explicitly labeled 'assuming a similar period' or 'assuming the same period'; it is an extrapolation of the observed inter-flare interval, not a quantity statistically forced by a fit disguised as a forecast. The repetition probability argument in Section 4.2 uses the external TDE rate of Yao et al. (2023) and external flare-rate studies (Graham et al. 2017; Ren et al. 2022); whether the chosen null hypothesis (two independent TDEs) is the right one is a statistical-correctness question, not a circularity. Self-citations (Guo et al. 2022, 2025; Guo et al. 2018 software) appear only as comparative references for RM lags or as fitting software, and the central claims do not rest on those citations. The paper is therefore self-contained against external benchmarks and exhibits no definitional or fitted-input reduction.

Assumptions & free parameters 9 free parameters · 5 assumptions · 0 invented entities

The paper introduces no new physical entities. It relies on established TDE fallback theory, the stream-disk collision simulations of Chan et al. (2019, 2020), and empirical scaling relations for AGN broad-line regions. The main free choices are the assumed stellar, orbital, and black hole parameters used to estimate the collision radius, plus the many fitted parameters in the empirical light curve and blackbody models.

free parameters (9)
  • First flare decay slope (p1) = -2.2 +/- 0.16
    Fitted to the g-band light curve decline (Table 1, Figure 4); used to support consistency with the t^-9/4 partial TDE fallback rate.
  • Second flare decay slope (p2) = -3.4 +/- 0.2
    Fitted to the second flare decline; the paper notes it may be biased by incomplete tail data.
  • Blackbody temperature (T_BB) = ~10^4.0 K (log T_BB)
    From single blackbody fits to UV/optical SEDs in Figure 7; used to claim constant temperature evolution.
  • Blackbody radius (R_BB) = ~10^15.5 cm
    From the same blackbody fits; used to estimate photosphere size.
  • Assumed stellar mass (M_*) = 1 solar mass
    Chosen in Section 4.1 to compute the tidal radius and pericenter; not fitted to AT2021aeuk data.
  • Assumed stellar radius (R_*) = 1 solar radius
    Same as above.
  • Assumed stream inclination (theta) = 60 degrees
    Median for random orientations; sets the collision radius range in Equation (2).
  • Black hole mass (M_BH) = 10^6.9 solar masses
    Taken from Foschini et al. (2015); an input to the collision-point estimate.
  • Empirical light curve model parameters (precursor, bumps, plateau) = Multiple values (Table 1)
    These describe the observed light curve shape; they are fits, not predictions. The peak luminosities, Gaussian widths, plateau length, and bump parameters are all fitted to the data.
assumptions (5)
  • domain assumption Partial TDE fallback follows a power-law decay with index ~ -9/4 (Coughlin & Nixon 2019).
    Invoked in Section 3.1.1 to interpret the first flare's decay slope.
  • domain assumption Stream-disk collisions in a pre-existing AGN disk can produce precursor flares and deplete the inner disk (Chan et al. 2019; Chan et al. 2020).
    Used in Section 4.1 and Figure 15 to explain the precursor, the second flare, the UV dip, and the X-ray corona destruction.
  • domain assumption The X-ray corona is powered by the inner accretion disk and can be suppressed by disk depletion or strong outflows (Uttley et al. 2014; Cao et al. 2023).
    Basis for the corona destruction mechanism in Section 4.1.
  • ad hoc to paper The recurrence period between the first and second flares is constant, so a third flare is predicted in September 2026.
    A linear extrapolation used for the prediction in Section 4.2.1 and Table 2; no physical model for period stability is provided.
  • domain assumption The a priori rate of TDEs in this galaxy is ~3.2e-5 per year and flaring AGN rates are under 0.1%, making two independent flares highly unlikely (Yao et al. 2023; Graham et al. 2017; Ren et al. 2022).
    Used in Section 4.2 to argue the two flares are physically related.

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Cite this review

Pith. "Pith review of AT2021aeuk: A Repeating Partial Tidal Disruption Event Candidate in a Narrow-line Seyfert 1 galaxy." pith.science (2026). https://pith.science/paper/YX5WFDUN

@misc{pith2026250101824,
  author       = {Pith},
  title        = {Pith review of: AT2021aeuk: A Repeating Partial Tidal Disruption Event Candidate in a Narrow-line Seyfert 1 galaxy},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/YX5WFDUN}},
  note         = {Machine review of arXiv:2501.01824}
}
abstract

A black hole (BH) can tear apart a star that ventures within its tidal radius, producing a luminous flare as the stellar debris falls back, known as a tidal disruption event (TDE). While TDEs in quiescent galaxies are relatively well understood, identifying TDEs in active galactic nuclei (AGN) still remains a significant challenge. We present the discovery of AT2021aeuk, a transient exhibiting dual flares within around three years in a narrow-line Seyfert 1 galaxy. Multi-wavelength observations triggered during the second flare in 2023 revealed an extraordinary X-ray V-shaped light curve, strongly anti-correlated with the optical light curve and accompanied by a lag of $\sim$40 days. This behavior is inconsistent with both supernova and pure AGN origins. In addition, a new broad component emerges in the Balmer lines during the second flare, showing a clear reverberation signal to the continuum variation. We propose that the dual-flare may be linked to a repeating partial TDE (rpTDE), where the second flare results from a collision between the TDE stream and the inner accretion disk, triggering an optical flare while simultaneously partially destroying the X-ray corona. However, other mechanisms, such as a stellar-mass BH (sBH) merger within an accretion disk, could produce similar phenomena, which we cannot entirely rule out. The Vera C. Rubin Observatory will be a powerful tool for further investigating the nature of such events in the future.

Figures

Figures reproduced from arXiv: 2501.01824 by the authors.

Figure 1
Figure 1. The HSC optical, VLA radio, and Swift X-ray images for AT2021aeuk. Left panel: HSC gri composite image with a 15′′× 15′′ field of view (FOV) observed before the flares of AT2021aeuk. Middle panel: VLA 6 − 8 GHz image with a 4′′× 4 ′′ FOV using A-configuration during the second flare. The gray ellipse and green cross indicate the beam size and GAIA optical center, respectively. Diffuse components are discovered on bo… view at source ↗
Figure 2
Figure 2. Long-term light curves of AT2021aeuk. CRTS data are seasonally binned for clarity. No dramatic variability was detected during the 15-year baseline prior to the outburst. subsequent analyses due to its larger telescope aperture and superior photometric accuracy. These optical flares from AT2021aeuk have also been noticed by Bao et al. (2023). 2.2. Optical Photometric Observations We triggered photometric observation… view at source ↗
Figure 3
Figure 3. Top panel: The MIR light curves, exhibiting significant echos to the optical flares. Middle panel: The X-ray light curve, with a nearly inverse evolution pattern to the optical light curve of the second flare. Bottom panel: ZTF (circles) and LJT (stars) light curves of the flares. The blue shadow indicates the period of the g−band plateau phase. The spectroscopic and radio observations are indicated by the black and… view at source ↗
Figures from the paper (16 more)
Figure 4
Figure 4. Figure 4 [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 6
Figure 6. Figure 6: SEDs for the pre-outburst state (black) and the second flare (orange). The first flare’s SED is decom￾posed into accretion disk and dust torus components, while the SED of the second flare peak incorporates an additional blackbody component into the pre-outburst SED. P…
Figure 5
Figure 5. Figure 5: Top panel: pre-outburst subtracted g-band light curves of the two flares of AT2021aeuk in AGN and other identified TDEs in quiescent galaxies (Yao et al. 2023). Bot￾tom panel: the ∆g − r color evolution during the flares. reaching about 20% of the luminosity of the fir…
Figure 7
Figure 7. Figure 7: Evolution of the blackbody luminosity, tempera￾ture, and radius during the second flare of AT2021aeuk, us￾ing non-parametric fitting methods. Each epoch’s fitting is based on UV W2, UV W1, and interpolated g- and r-band lu￾minosities derived from the fitted light curve…
Figure 8
Figure 8. Figure 8: The UV W1 light curve for the second flare is pre￾sented without host subtraction. The pre-outburst bright￾ness, estimated through SED fitting, is denoted by the hori￾zontal line, which aligns with the observed UV W1 luminosity at both the end of the first flare and th…
Figure 10
Figure 10. Figure 10: Top panel: Evolution of the X-ray light curve during the second flare, with different bins color-coded. The inset panel displays the measured time lag demonstrating the anti-correlation between the optical and X-ray light curves. Bottom panel: Evolution of the X-ray p…
Figure 11
Figure 11. Figure 11: Spectroscopic follow-up observations of AT2021aeuk during its second flare. All spectra have been corrected for Galactic extinction. For comparison, the SDSS archival spectrum from 2003 is included as a reference. The positions of the fluorescence lines O IIIλ3133 and…
Figure 12
Figure 12. Figure 12: The luminosity and FWHM evolution of the Hα and Hβ lines. Both parameters display a delay of 25 days to the second flare. Note that the XLT epoch is discarded due to significant influence from moonlight, poor seeing conditions, and high airmass. 4200 4400 4600 4800 50…
Figure 13
Figure 13. Figure 13: The continuum-subtracted spectra from archival SDSS (gray line) and GTC observations (blue/green/purple lines). The short red lines indicate Fe II emission lines. The variability of N III and He II lines is not discernible after subtracting the Fe II pseudo continuum.…
Figure 15
Figure 15. Figure 15: A brief scheme about the stream-disk evolution to explain the anti-correlation between the optical and X-ray light curves in the second flare. Top panel: The trajectory of the disrupted star intersects with the inner disk. Middle panel: Following an elliptical orbit, …
Figure 16
Figure 16. Figure 16: The four rpTDEs within the ZTF footprint. The AT2020vdq and AT2022dbl are rpTDEs in quiescent galaxies, while the AT2019aalc and AT2021aeuk are rpTDE candidates in AGN. The y-axis is set as the ratio between evolving luminosity and the peak luminosity of the first fla…
Figure 17
Figure 17. Figure 17: Naturally weighted CLEAN maps of VLA observations at 5−18 GHz in B-configuration and A-configuration. The green cross indicates the optical centroid from GAIA DR3. The grey ellipses in the bottom left corner of each panel represent the FWHM of the restoring beam. 1 3 …
Figure 18
Figure 18. Figure 18: Radio spectrum of AT2021aeuk. The integrated flux is shown in solid circles, while the core flux is shown as open circles. The black and red symbols represent the flux in B-configuration and A-configuration, respectively. The black line indicates the best-fit power-la…
Figure 19
Figure 19. Figure 19: Spectral decomposition of the Hα complex. A narrow plus an intermediate component are used to fit each narrow line, and one additional broad component is used for Hα. 0 100 SDSS (archive) 2 = 2.2 0 100 LJT (-8) 2 = 1.3 0 100 LJT (+11) 2 = 0.8 0 100 GTC (+22) 2 = 1.9 0…
Figure 20
Figure 20. Figure 20: The same as [PITH_FULL_IMAGE:figures/full_fig_p024_20.png]
Figure 21
Figure 21. Figure 21: Comparison of AT2021aeuk with TDEs (gray), as well as ANTs and TDE in AGN candidates (cyan). Solid markers denote reliable BH mass while hollow markers, are considered less robust. For most light curve properties, the uncertainty from the fitting is negligible. For th…

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Forward citations

Cited by 2 Pith papers

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

  1. IGR J12580+0134: A Possible Repeated Partial Tidal Disruption Event Inferred from Late-Time Radio Re-brightenin

    astro-ph.HE 2026-02 conditional novelty 6.0 of 10

    IGR J12580+0134 is proposed as a repeating partial tidal disruption event candidate, with two radio flares separated by ~1513 days and a possible third rebrightening.

  2. The Double Tidal Disruption Event AT 2022dbl Implies That at Least Some "Standard" Optical TDEs are Partial Disruptions

    astro-ph.HE 2025-05 accept novelty 6.0 of 10

    The repeating optical-UV tidal disruption event AT 2022dbl is the first robust case of a 'normal' TDE being a partial disruption of the same star.

Reference graph

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