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arxiv: 2606.06578 · v1 · pith:UMMBGWHJnew · submitted 2026-06-04 · 🌌 astro-ph.HE

A Disappearing Act: Constraints From "Missing" Flares of Repeating Partial TDE Candidates

Jason T. Hinkle , Chang Liu , Adam A. Miller , Ping Chen , Katie Auchettl , Benjamin J. Shappee , Christopher S. Kochanek , K. Z. Stanek
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Todd A. Thompson
This is my paper

Pith reviewed 2026-06-28 00:05 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords repeating partial TDEstidal disruption eventsUV/optical flaresmain-sequence starsbound orbitssemi-analytical modelingTDE ratesnon-detections
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The pith

Non-detections of predicted third flares show two repeating TDE candidates are actually rpTDEs from a single bound star.

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

The paper investigates two sources that each produced two bright flares but none in the expected third window. Low statistical odds of two separate TDEs from one galaxy, plus inconsistency with binary-star disruption models, lead the authors to identify both as repeating partial TDEs. Semi-analytical calculations then show that only a main-sequence star placed promptly onto a bound orbit with a deep first pericenter passage reproduces the observed pair of similar-energy flares without a third detectable one. This interpretation implies that many observed rTDEs over short baselines are partial disruptions and that a sizable fraction of such systems yield only two visible flares.

Core claim

TDE 2022dbl and TDE 2020vdq are rpTDEs. To produce only two observable flares with similar energetics, semi-analytical modeling strongly favors a main-sequence star promptly placed on a bound orbit with a deep initial tidal encounter at pericenter.

What carries the argument

Semi-analytical modeling of rpTDE flare sequences that varies stellar type, orbital binding, and pericenter depth to match observed energetics and the absence of a third flare.

If this is right

  • Most rTDEs that show multiple flares on a few-year baseline are repeating partial disruptions rather than independent full TDEs.
  • A significant fraction of rpTDE systems may produce only two observable flares.
  • Use of r(p)TDEs to probe TDE physics and nuclear dynamics must account for this limited flare count.
  • Yield estimates for upcoming time-domain surveys should incorporate the possibility that many rpTDEs are visible for only two flares.

Where Pith is reading between the lines

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

  • Survey cadence and depth choices may need to prioritize catching the first two flares rather than waiting for a longer sequence.
  • The preference for prompt bound orbits after the first encounter could link to specific dynamical channels for placing stars near supermassive black holes.
  • If only two flares are common, the overall TDE rate inferred from flare counts may be underestimated unless rpTDE demographics are folded in.

Load-bearing premise

The two observed flares are strictly periodic, so a third flare must appear at the predicted time.

What would settle it

Continued non-detection or a clear detection of a third flare around early 2026 in either source would test whether the periodicity assumption holds and whether the rpTDE classification is required.

Figures

Figures reproduced from arXiv: 2606.06578 by Adam A. Miller, Benjamin J. Shappee, Chang Liu, Christopher S. Kochanek, Jason T. Hinkle, Katie Auchettl, K. Z. Stanek, Ping Chen, Todd A. Thompson.

Figure 1
Figure 1. Figure 1: Host-subtracted and Galactic foreground extinction-corrected UV/optical light curves of TDE 2022dbl (ASASSN-22ci; top) and TDE 2020vdq (ZTF20acaazkt; bottom). Data from Swift (UV+U; circles), ASAS-SN (g; squares), ATLAS (co; pentagons), ZTF (gr; pluses), and dedicated follow-up photometry of TDE 2022dbl from CDK24 + RC32 (gri) are shown. Survey photometry is stacked in 1-d bins during the two flares, excep… view at source ↗
Figure 2
Figure 2. Figure 2: Spectral energy distribution (SED) of the host-galaxy and near the (predicted) peaks for TDE 2022dbl (ASASSN-22ci; left) and TDE 2020vdq (ZTF20acaazkt; right). The host-galaxy photometry is shown in gray circles, and the black line is the best-fitting model. The blue diamonds, gold squares, and red pentagons are the observed SEDs near the time of peak for the first, second, and expected third flares. All p… view at source ↗
Figure 3
Figure 3. Figure 3: Outcomes of TDE-like encounters for several stellar models across a wide range of initial β0. The stellar models include a low-mass fully convective star, 1–3 M⊙ main-sequence stars at various evolutionary stages (ZAMS, solar-type, and TAMS), and a 1 M⊙ RGB star. The number of detectable flares, defined by a mass loss threshold of ∆M ≥ Max(10−3 M⊙, ∆Mmax/30), is indicated in each cell. The background color… view at source ↗
read the original abstract

Recurrent tidal disruption events (rTDEs) are sources that exhibit multiple TDE-like flares; many are likely powered by the recurring partial disruption of a bound star, in a repeating partial TDE (rpTDE). Two such sources, TDE 2022dbl (ASASSN-22ci) and TDE 2020vdq (ZTF20acaazkt), each exhibited two UV/optical flares and, under the assumption of periodicity, both were expected to exhibit a third flare in early 2026. Neither exhibited such a flare, to limits of $L_{\textrm{UV/optical}} \lesssim 10^{42}$ erg s$^{-1}$, $\sim$30$\times$ fainter than the previous flares. Here, we examine several possible explanations. Observing two independent TDEs from the same galaxy within $\sim$2 yr has a probability of $\lesssim$0.5% for measured average TDE rates and currently expected rate enhancements, unless there is extreme intrinsic dispersion in the rates. Theoretical predictions for a double TDE of both stars in a binary are inconsistent with the observed flares. We therefore conclude that TDE 2022dbl and TDE 2020vdq are rpTDEs. To produce only two observable flares with similar energetics, our semi-analytical modeling strongly favors a main-sequence star promptly placed on a bound orbit with a deep initial tidal encounter at pericenter. These results suggest that the majority of rTDEs with multiple flares over a few-year baseline are likely to be rpTDEs, and that a significant fraction of systems may produce only two observable flares. This has important implications for the use of r(p)TDEs as probes of TDE physics and dynamical processes in the nuclei of other galaxies, in addition to the expected yield from upcoming surveys.

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 / 1 minor

Summary. The paper claims that TDE 2022dbl and TDE 2020vdq are repeating partial TDEs (rpTDEs) rather than independent TDEs or binary disruptions. This follows from a ≲0.5% probability of two independent TDEs in the same galaxy within ~2 yr (using measured rates, with an 'extreme intrinsic dispersion' caveat), inconsistency with binary TDE predictions, and semi-analytical modeling that favors a main-sequence star promptly placed on a bound orbit with a deep initial pericenter encounter. The modeling is used to explain the observation of only two flares of similar energetics together with the non-detection of a third flare to L_UV/optical ≲ 10^42 erg s^{-1} (~30× fainter) in early 2026, under the assumption of periodicity for the observed flares.

Significance. If the central conclusions hold, the work constrains the demographics of rTDEs, indicating that many systems with multiple flares over a few-year baseline are rpTDEs and that a significant fraction may produce only two observable flares. This carries implications for the use of r(p)TDEs as probes of TDE physics and galactic nuclei dynamics, as well as for survey yields. Strengths include the grounding in external measured TDE rates for the probability estimates and the deployment of semi-analytical modeling to derive specific orbital and stellar-type preferences.

major comments (2)
  1. [Abstract] Abstract and modeling section: The conclusion that the sources are rpTDEs and that semi-analytical modeling 'strongly favors' a main-sequence star on a bound orbit with deep initial pericenter is derived specifically to explain only two observable flares given the non-detection. This non-detection supplies the key constraint only under the periodicity assumption used to predict a third flare in early 2026. The manuscript should include a quantitative assessment of how the modeling posteriors and favored parameters shift if the two flares are treated as aperiodic (or if the inferred period is allowed a broad uncertainty range), as this assumption is load-bearing for the rpTDE interpretation over the independent-TDE scenario.
  2. [Probability section] Probability calculation (likely §2 or equivalent): The ≲0.5% probability for two independent TDEs is presented as evidence against that scenario, but the text already notes the 'extreme intrinsic dispersion' escape clause. The manuscript should report the sensitivity of this probability to the dispersion parameter (including the value at which the probability rises above a few percent) and any error bars or Poisson uncertainties on the underlying TDE rate measurements used.
minor comments (1)
  1. [Abstract] The abstract states the non-detection limits but does not specify the exact observation epochs or instruments used for the 2026 limits; this should be clarified with a brief reference to the relevant data section or table.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive report. The two major comments identify load-bearing assumptions in the rpTDE interpretation. We address each below and will revise the manuscript to strengthen the presentation of uncertainties.

read point-by-point responses

  1. Referee: [Abstract] Abstract and modeling section: The conclusion that the sources are rpTDEs and that semi-analytical modeling 'strongly favors' a main-sequence star on a bound orbit with deep initial pericenter is derived specifically to explain only two observable flares given the non-detection. This non-detection supplies the key constraint only under the periodicity assumption used to predict a third flare in early 2026. The manuscript should include a quantitative assessment of how the modeling posteriors and favored parameters shift if the two flares are treated as aperiodic (or if the inferred period is allowed a broad uncertainty range), as this assumption is load-bearing for the rpTDE interpretation over the independent-TDE scenario.

    Authors: We agree that the periodicity assumption is central to using the non-detection as a strong constraint on the orbital parameters. The two observed flares have comparable peak luminosities and similar rise times separated by ~2 yr, which motivates the periodic interpretation, but we acknowledge that the data do not yet rule out aperiodic behavior. In revision we will add a dedicated subsection that re-runs the semi-analytical grid allowing the second flare to be either the first or second return (i.e., relaxing strict periodicity) and that marginalizes over a broad prior on the period (uniform in log P from 0.5–5 yr). We will report the resulting shifts in the posterior probability for main-sequence vs. giant stars and for deep vs. shallow encounters, together with the fraction of models that still produce only two observable flares above the survey limits. revision: yes

  2. Referee: [Probability section] Probability calculation (likely §2 or equivalent): The ≲0.5% probability for two independent TDEs is presented as evidence against that scenario, but the text already notes the 'extreme intrinsic dispersion' escape clause. The manuscript should report the sensitivity of this probability to the dispersion parameter (including the value at which the probability rises above a few percent) and any error bars or Poisson uncertainties on the underlying TDE rate measurements used.

    Authors: The referee correctly notes that the quoted probability depends on both the mean rate and the assumed dispersion. In the revised manuscript we will (i) tabulate the two-TDE probability as a function of the log-normal dispersion parameter σ from 0 to 2 dex, explicitly marking the σ at which the probability exceeds 5 %, and (ii) propagate the published 1σ uncertainties on the volumetric TDE rate (from the ZTF and ASAS-SN samples) through the calculation, quoting the resulting range on the joint probability. This will make the robustness (or lack thereof) to the dispersion caveat fully quantitative. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation uses external rates and explicit assumption

full rationale

The paper's chain proceeds from observed flares, an explicitly stated periodicity assumption to predict a third flare, non-detection limits, external literature TDE rates for the ~0.5% independent-TDE probability, inconsistency with binary TDE predictions, and semi-analytical modeling favoring a specific rpTDE scenario. None of these steps reduce by the paper's own equations to quantities defined only in terms of parameters fitted from the same dataset, nor rely on self-citation load-bearing, uniqueness imported from authors, or ansatz smuggling. The periodicity assumption is flagged as such and does not create a self-definitional loop. The result is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Abstract-only review limits visibility into full set of modeling parameters; key domain assumption on periodicity is identifiable from text.

axioms (1)
  • domain assumption The two observed flares follow a periodic orbit allowing prediction of a third flare in early 2026
    Invoked explicitly to set expectation for non-detection and to compare against rpTDE models

pith-pipeline@v0.9.1-grok · 5913 in / 1345 out tokens · 30417 ms · 2026-06-28T00:05:52.498085+00:00 · methodology

discussion (0)

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Reference graph

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