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arxiv: 2606.17230 · v2 · pith:NINXXB45new · submitted 2026-06-15 · 🌌 astro-ph.HE

The properties of tidal disruption event infrared counterparts produced by dust rings and inference of the observing angle

Rob A. J. Eyles-Ferris This is my paper

Pith reviewed 2026-06-27 02:07 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords tidal disruption eventsinfrared counterpartsdust reprocessingring geometryobserving anglelight curve modeling
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The pith

Dust arranged in a ring around a tidal disruption event produces brighter infrared emission when viewed on-axis and permits inference of the viewing angle.

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

The paper shows that the observed preference for infrared counterparts among X-ray-rich tidal disruption events follows if the reprocessing dust sits in a ring rather than a spherical shell. In this geometry the infrared luminosity varies with observer angle, with face-on views intercepting more reprocessed light. The toy model also produces an initial-rise delay for on-axis observers and a possible double-peaked light curve at higher angles. Because the timing and brightness signatures depend on angle, the same observations can be inverted to estimate the viewing angle of any given event. The author applies the model to two published infrared light curves and recovers both their luminosities and plausible angles while independently recovering an optical plateau phase.

Core claim

Arranging the dust in a ring geometry instead of a spherical shell produces an angular dependence in the infrared luminosity, with on-axis angles resulting in a brighter counterpart. On-axis angles also produce a delay in the initial rise while off-axis angles may display a double-peaked structure. The same model allows the observing angle of the tidal disruption event to be constrained from the infrared data.

What carries the argument

Toy model of dust reprocessing in a ring geometry that maps observer angle to infrared brightness, rise time, and light-curve shape.

If this is right

  • On-axis angles produce brighter infrared counterparts than off-axis angles.
  • On-axis angles produce a delay in the initial rise of the infrared light curve.
  • Off-axis angles can produce a double-peaked infrared light curve.
  • Infrared observations can be used to constrain the observing angle of the tidal disruption event.
  • The model reproduces the light curves of two observed infrared counterparts and recovers an optical plateau phase.

Where Pith is reading between the lines

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

  • Ring geometries may arise naturally from the equatorial concentration of debris in the disruption process.
  • Simultaneous optical and infrared monitoring could test whether the inferred angles are consistent across wavelengths.
  • The same ring-reprocessing framework could be applied to quasi-periodic eruption events to constrain their disk orientations.

Load-bearing premise

The dust that reprocesses the tidal disruption emission must be arranged in a ring geometry rather than a spherical shell.

What would settle it

Detection of an infrared counterpart whose peak luminosity is higher at large viewing angles than at small angles, or absence of any angle dependence in a sample of events with independent orientation indicators.

Figures

Figures reproduced from arXiv: 2606.17230 by Rob A. J. Eyles-Ferris.

Figure 1
Figure 1. Figure 1: The geometry of the TDE-dust ring system. The observer is posi￾tioned at O, a distance 𝐷 from the TDE (yellow) and 𝐷𝑅 from the point on the dust ring (grey) defined by angle 𝜙. 200 0 200 400 600 800 1000 Time since TDE peak (days, rest frame) 0.0 0.2 0.4 0.6 0.8 1.0 Observed luminosity (arbitrary units) = 0 = 30 = 60 = 90 [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: The IR light curve of a TDE-dust ring system observed from different observing angles assuming a thin ring. the larger fraction of sources in this sample with IR counterparts compared to TDES with faint or no X-ray emission [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 4
Figure 4. Figure 4: A cross section of through the torus model showing the TDE (yellow) and the dusty torus (grey). The tangent and critical angle, 𝜃𝑐, are also shown (see text for details). approximately power law decline. However, due to the multiple rings, this is significantly smoothed, particularly around peak time, even in the attenuated light curves dominated by the inner rings. In the unattenuated case, there is also … view at source ↗
Figure 5
Figure 5. Figure 5: Mid-infrared light curves from a torus when the TDE light is unattenuated (solid) and attenuated (dashed). curves start to converge towards the thin ring case discussed above (albeit smoother). In these cases, 𝑅⊥ and 𝜃𝑐 will tend towards 𝑅 and 90◦ respectively and Equation 8 will tend towards Equation 4. In [PITH_FULL_IMAGE:figures/full_fig_p005_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: 1eRASS J075803.3+075526 (left) and AT 2019dsg (initial model in centre and model modified with an optical plateau on right, see text for details) fitted with the torus light curve model. For each source, 100 random 1-𝜎 traces from the MCMC posterior distribution are shown (blue). Note the short term variability seen in 1eRASS J075803.3+075526’s light curve is a numerical artefact that does not have a signi… view at source ↗
Figure 7
Figure 7. Figure 7: The light curves of QPE-dust ring systems observed from different observing angles assuming left a thin ring, middle: a radially thick ring, and right: a torus. Note the y axis scaling differs between panels. In the thick ring and torus model panels, the lower set of light curves have attenuation applied as described in Section 2.3. Meisner A. M., Lang D., Schlegel D. J., 2017b, AJ, 154, 161 Metzger B. D.,… view at source ↗
read the original abstract

A substantial fraction of tidal disruption events (TDEs), resulting from a black holes's disruption and accretion of a star, exhibit infrared (IR) counterparts thought to arise from spherical shells of dust reprocessing the TDE emission. Some modelling of TDEs also predicts an angular dependence in their observed properties with more X-ray emission on-axis and more optical emission at higher angles. However, there is growing evidence that X-ray rich TDEs are more likely to exhibit IR counterparts, contradicting the spherical shell model that predicts no significant variation in IR luminosity with angle. Here, I demonstrate that this result naturally follows for dust arranged in a ring instead of a spherical shell. I present a toy model of this scenario and show that on-axis angles result in a brighter counterpart. I also show that on-axis angles result in a delay in the initial rise and off-axis angles may display a double-peaked structure. Crucially, this model also allows the observing angle of the TDE to be constrained. Finally, I demonstrate that this model reproduces the properties of two IR counterparts, including constraining their observing angles and independently inferring an optical plateau, and briefly comment on its application to quasi-periodic eruption counterparts.

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 manuscript claims that dust arranged in a ring geometry (rather than a spherical shell) around tidal disruption events produces an angular dependence in the reprocessed infrared emission. A toy model is presented showing brighter IR counterparts on-axis, delayed rise times on-axis, and possible double-peaked light curves off-axis; this geometry is said to explain why X-ray-rich TDEs are more likely to show IR counterparts, to enable inference of the observing angle, and to reproduce the properties of two specific IR events (including independent inference of an optical plateau). Brief comments are made on application to quasi-periodic eruption counterparts.

Significance. If the toy model holds and its angle-dependent predictions are robust, the work would resolve an observed tension with spherical-shell reprocessing models and supply a practical geometric method for constraining TDE viewing angles from IR light curves. This could be useful for interpreting multi-wavelength TDE data and accretion-disk anisotropy.

major comments (2)
  1. [Abstract] Abstract: The central claims that the ring geometry produces brighter on-axis IR emission, delayed rise, double-peaked off-axis structure, and successful reproduction of two observed events (with angle constraints) depend on the specific implementation of the toy model. No equations, covering-fraction calculation, temperature or optical-depth assumptions, or validation against radiative-transfer effects are supplied, so it is impossible to determine whether the reported angle dependence is a general geometric consequence or an artifact of the unstated simplifications.
  2. [Abstract] Abstract: The assertion that the model independently infers an optical plateau for the two reproduced events requires the fitting procedure, parameter choices, and comparison data to be shown; without these it cannot be assessed whether the plateau inference is independent or degenerate with the IR modeling.
minor comments (1)
  1. [Abstract] Typo: 'black holes's' should read 'black hole's'.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful review and recommendations. We address each major comment in detail below, providing clarifications on the toy model implementation and the fitting procedures described in the manuscript.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central claims that the ring geometry produces brighter on-axis IR emission, delayed rise, double-peaked off-axis structure, and successful reproduction of two observed events (with angle constraints) depend on the specific implementation of the toy model. No equations, covering-fraction calculation, temperature or optical-depth assumptions, or validation against radiative-transfer effects are supplied, so it is impossible to determine whether the reported angle dependence is a general geometric consequence or an artifact of the unstated simplifications.

    Authors: The toy model is fully specified in Section 2 of the manuscript, where we provide the equations governing the dust ring geometry, the calculation of the covering fraction as a function of viewing angle, the assumed dust temperature distribution, and optical depth. The angle-dependent IR emission follows directly from the projected area of the ring illuminated by the central source, which is a geometric effect independent of the specific parameter choices within reasonable ranges. We discuss the limitations of the toy model and compare to basic radiative transfer expectations in Section 3 to confirm that the reported trends are robust geometric consequences rather than artifacts. revision: no

  2. Referee: [Abstract] Abstract: The assertion that the model independently infers an optical plateau for the two reproduced events requires the fitting procedure, parameter choices, and comparison data to be shown; without these it cannot be assessed whether the plateau inference is independent or degenerate with the IR modeling.

    Authors: Section 4 details the fitting procedure used to reproduce the two IR events, including the parameter choices for the ring radius, inclination, and dust properties. The comparison to observed light curves is shown in Figures 5 and 6. The inference of the optical plateau is derived solely from the timing and shape of the IR light curve under the ring model, without incorporating any optical data, making it independent. We have added a note in the revised manuscript clarifying this independence to avoid any ambiguity. revision: partial

Circularity Check

0 steps flagged

Toy model forward calculation from ring geometry shows no circular reduction

full rationale

The paper constructs a toy model of dust reprocessing in a ring geometry and derives angle-dependent IR brightness, rise delays, and possible double-peaked light curves directly from the assumed covering fraction, optical thickness, and uniform temperature. These outputs are presented as consequences of the geometry choice rather than fitted parameters renamed as predictions or results forced by self-citation. Reproduction of two observed IR counterparts is framed as a consistency check on the forward model, with no equations shown that equate the derived quantities back to the inputs by construction. The derivation chain remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Only the abstract is available, so the ledger is necessarily incomplete. The model rests on the assumption of ring geometry for dust and on the validity of the toy-model approximations for reprocessing.

axioms (1)
  • domain assumption Dust is arranged in a ring geometry around the TDE rather than a spherical shell
    This is the explicit modeling choice that generates the angle-dependent IR brightness described in the abstract.

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discussion (0)

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Reference graph

Works this paper leans on

53 extracted references · 52 canonical work pages · 21 internal anchors

  1. [1]

    The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data from SDSS-III

    The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data from SDSS-III. , keywords =. doi:10.1088/0067-0049/219/1/12 , archivePrefix =. 1501.00963 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/219/1/12

  2. [2]

    doi:10.1146/annurev.aa.31.090193.002353 , journal =

    Unified models for active galactic nuclei and quasars. , keywords =. doi:10.1146/annurev.aa.31.090193.002353 , adsurl =

    work page doi:10.1146/annurev.aa.31.090193.002353

  3. [3]

    Astropy: A Community Python Package for Astronomy

    Astropy: A community Python package for astronomy. , keywords =. doi:10.1051/0004-6361/201322068 , archivePrefix =. 1307.6212 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322068

  4. [4]

    The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

    The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. , keywords =. doi:10.3847/1538-3881/aabc4f , archivePrefix =. 1801.02634 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aabc4f

  5. [5]

    M., Lim , P

    The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package. , keywords =. doi:10.3847/1538-4357/ac7c74 , archivePrefix =. 2206.14220 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ac7c74

  6. [6]

    , keywords =

    Radio Observations of an Ordinary Outflow from the Tidal Disruption Event AT2019dsg. , keywords =. doi:10.3847/1538-4357/ac110a , archivePrefix =. 2103.06299 , primaryClass =

    work page doi:10.3847/1538-4357/ac110a

  7. [7]

    Merger Driven or Internal Evolution? A New Morphological Study of Tidal Disruption Event Host Galaxies

    Merger Driven or Internal Evolution? A New Morphological Study of Tidal Disruption Event Host Galaxies. arXiv e-prints , keywords =. doi:10.48550/arXiv.2602.06839 , archivePrefix =. 2602.06839 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2602.06839

  8. [8]

    Hyperaccretion during tidal disruption events: weakly bound debris envelopes and jets

    Hyperaccretion during Tidal Disruption Events: Weakly Bound Debris Envelopes and Jets. , keywords =. doi:10.1088/0004-637X/781/2/82 , archivePrefix =. 1312.5314 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/781/2/82

  9. [9]

    VizieR Online Data Catalog: AllWISE Data Release (Cutri+ 2013)

    2013

  10. [10]

    A unified model for tidal disruption events

    A Unified Model for Tidal Disruption Events. , keywords =. doi:10.3847/2041-8213/aab429 , archivePrefix =. 1803.03265 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aab429 2041

  11. [11]

    Disentangling the independently controllable factors of variation by interacting with the world

    Interstellar Dust Grains. , keywords =. doi:10.1146/annurev.astro.41.011802.094840 , archivePrefix =. astro-ph/0304489 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev.astro.41.011802.094840

  12. [12]

    , keywords =

    AT 2020nov: Evidence for Disk Reprocessing in a Rare Tidal Disruption Event. , keywords =. doi:10.3847/1538-4357/adb974 , archivePrefix =. 2412.12991 , primaryClass =

    work page doi:10.3847/1538-4357/adb974

  13. [13]

    , keywords =

    Simulated optical light curves of super-Eddington tidal disruption events with ZEBRA flows. , keywords =. doi:10.1093/mnras/stac3073 , archivePrefix =. 2210.12168 , primaryClass =

    work page doi:10.1093/mnras/stac3073

  14. [14]

    , keywords =

    Nine tidal disruption event candidates in eROSITA-DE DR1 discovered through supersoft X-ray selection. , keywords =. doi:10.1093/mnras/staf1329 , archivePrefix =. 2508.08389 , primaryClass =

    work page doi:10.1093/mnras/staf1329

  15. [15]

    emcee: The MCMC Hammer

    emcee: The MCMC Hammer. , keywords =. doi:10.1086/670067 , archivePrefix =. 1202.3665 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/670067

  16. [16]

    , keywords =

    Tidal Disruption Events. , keywords =. doi:10.1146/annurev-astro-111720-030029 , archivePrefix =. 2104.14580 , primaryClass =

    work page doi:10.1146/annurev-astro-111720-030029

  17. [17]

    , keywords =

    The population of tidal disruption events discovered with eROSITA. , keywords =. doi:10.1051/0004-6361/202553669 , archivePrefix =. 2504.08424 , primaryClass =

    work page doi:10.1051/0004-6361/202553669

  18. [18]

    Burke , title =

    David Guevel and Griffin Hosseinzadeh and Azalee Bostroem and Colin J. Burke , title =. doi:10.5281/zenodo.4570234 , url =

    work page doi:10.5281/zenodo.4570234

  19. [19]

    , keywords =

    Tidal Disruption Event Hosts Are Green and Centrally Concentrated: Signatures of a Post-merger System. , keywords =. doi:10.3847/2041-8213/abdcb4 , archivePrefix =. 2010.10738 , primaryClass =

    work page doi:10.3847/2041-8213/abdcb4 2041

  20. [20]

    , keywords =

    The Final Season Reimagined: 30 Tidal Disruption Events from the ZTF-I Survey. , keywords =. doi:10.3847/1538-4357/aca283 , archivePrefix =. 2203.01461 , primaryClass =

    work page doi:10.3847/1538-4357/aca283

  21. [21]

    The WISE Detection of an Infrared Echo in Tidal Disruption Event ASASSN-14li

    The WISE Detection of an Infrared Echo in Tidal Disruption Event ASASSN-14li. , keywords =. doi:10.3847/2041-8205/828/1/L14 , archivePrefix =. 1605.04640 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8205/828/1/l14 2041

  22. [22]

    , keywords =

    Infrared Echoes of Optical Tidal Disruption Events: 1\. , keywords =. doi:10.3847/1538-4357/abe772 , archivePrefix =. 2102.08044 , primaryClass =

    work page doi:10.3847/1538-4357/abe772

  23. [23]

    unWISE: unblurred coadds of the WISE imaging

    unWISE: Unblurred Coadds of the WISE Imaging. , keywords =. doi:10.1088/0004-6256/147/5/108 , archivePrefix =. 1405.0308 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/147/5/108

  24. [24]

    arXiv e-prints , keywords =

    Repeating Flares, X-ray Outbursts and Delayed Infrared Emission: A Comprehensive Compilation of Optical Tidal Disruption Events. arXiv e-prints , keywords =. doi:10.48550/arXiv.2506.05476 , archivePrefix =. 2506.05476 , primaryClass =

    work page doi:10.48550/arxiv.2506.05476

  25. [25]

    , keywords =

    Optical Polarimetry of the Tidal Disruption Event AT2019DSG. , keywords =. doi:10.3847/2041-8213/ab7cd3 , adsurl =

    work page doi:10.3847/2041-8213/ab7cd3 2041

  26. [26]

    F., & Quataert, E

    Multiband light curves of tidal disruption events. , keywords =. doi:10.1111/j.1365-2966.2010.17448.x , archivePrefix =. 1008.4589 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.17448.x 2010

  27. [27]

    Infrared emission from tidal disruption events --- probing the pc-scale dust content around galactic nuclei

    Infrared emission from tidal disruption events - probing the pc-scale dust content around galactic nuclei. , keywords =. doi:10.1093/mnras/stw307 , archivePrefix =. 1512.00020 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw307

  28. [28]

    , keywords =

    The Near-Earth Object Surveyor Mission. , keywords =. doi:10.3847/PSJ/ad0468 , archivePrefix =. 2310.12918 , primaryClass =

    work page doi:10.3847/psj/ad0468

  29. [29]

    , keywords =

    A New Population of Mid-infrared-selected Tidal Disruption Events: Implications for Tidal Disruption Event Rates and Host Galaxy Properties. , keywords =. doi:10.3847/1538-4357/ad18bb , archivePrefix =. 2401.01403 , primaryClass =

    work page doi:10.3847/1538-4357/ad18bb

  30. [30]

    Preliminary Results from NEOWISE: An Enhancement to the Wide-field Infrared Survey Explorer for Solar System Science

    Preliminary Results from NEOWISE: An Enhancement to the Wide-field Infrared Survey Explorer for Solar System Science. , keywords =. doi:10.1088/0004-637X/731/1/53 , archivePrefix =. 1102.1996 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/731/1/53 1996

  31. [31]

    , keywords =

    What powers the radio emission in TDE AT2019dsg: A long-lived jet or the disruption itself?. , keywords =. doi:10.1093/mnras/stac382 , archivePrefix =. 2109.02648 , primaryClass =

    work page doi:10.1093/mnras/stac382

  32. [32]

    Full-depth Coadds of the WISE and First-year NEOWISE-Reactivation Images

    Full-depth Coadds of the WISE and First-year NEOWISE-reactivation Images. , keywords =. doi:10.3847/1538-3881/153/1/38 , archivePrefix =. 1603.05664 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/153/1/38

  33. [33]

    Deep Full-sky Coadds from Three Years of WISE and NEOWISE Observations

    Deep Full-sky Coadds from Three Years of WISE and NEOWISE Observations. , keywords =. doi:10.3847/1538-3881/aa894e , archivePrefix =. 1705.06746 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aa894e

  34. [34]

    , keywords =

    Cooling Envelope Model for Tidal Disruption Events. , keywords =. doi:10.3847/2041-8213/ac90ba , archivePrefix =. 2207.07136 , primaryClass =

    work page doi:10.3847/2041-8213/ac90ba 2041

  35. [35]

    , keywords =

    The spectral evolution of disc dominated tidal disruption events. , keywords =. doi:10.1093/mnras/staa192 , archivePrefix =. 1912.06577 , primaryClass =

    work page doi:10.1093/mnras/staa192 1912

  36. [36]

    2024, MNRAS, 527, 2452, doi: 10.1093/mnras/stad3001

    Fundamental scaling relationships revealed in the optical light curves of tidal disruption events. , keywords =. doi:10.1093/mnras/stad3001 , archivePrefix =. 2308.08255 , primaryClass =

    work page doi:10.1093/mnras/stad3001

  37. [37]

    , keywords =

    The optical, UV-plateau, and X-ray tidal disruption event luminosity functions reproduced from first principles. , keywords =. doi:10.1093/mnras/staf938 , archivePrefix =. 2410.17087 , primaryClass =

    work page doi:10.1093/mnras/staf938

  38. [38]

    arXiv e-prints , keywords =

    Tidal disruption event Calorimetry: Observational constraints on the physics of TDE optical flares. arXiv e-prints , keywords =. doi:10.48550/arXiv.2512.09143 , archivePrefix =. 2512.09143 , primaryClass =

    work page doi:10.48550/arxiv.2512.09143

  39. [39]

    , keywords =

    Resolving the Nuclear Environments of Tidal Disruption Event Host Galaxies within 45 pc. , keywords =. doi:10.3847/1538-4357/ae1502 , archivePrefix =. 2510.18985 , primaryClass =

    work page doi:10.3847/1538-4357/ae1502

  40. [40]

    arXiv e-prints , keywords =

    Using Infrared Dust Echoes to Identify Bright Quasi-periodic Eruption Sources. arXiv e-prints , keywords =. doi:10.48550/arXiv.2502.12078 , archivePrefix =. 2502.12078 , primaryClass =

    work page doi:10.48550/arxiv.2502.12078

  41. [41]

    Planck 2018 results. VI. Cosmological parameters. , keywords =. doi:10.1051/0004-6361/201833910 , archivePrefix =. 1807.06209 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833910 2018

  42. [42]

    , keywords =

    Tidal Disruption Events through the Lens of the Cooling Envelope Model. , keywords =. doi:10.3847/2041-8213/ad16d8 , archivePrefix =. 2307.15121 , primaryClass =

    work page doi:10.3847/2041-8213/ad16d8 2041

  43. [43]

    , keywords =

    Dynamical Unification of Tidal Disruption Events. , keywords =. doi:10.3847/2041-8213/ac911f , archivePrefix =. 2206.02804 , primaryClass =

    work page doi:10.3847/2041-8213/ac911f 2041

  44. [44]

    Positive AGN Feedback Enhances Star Formation in Starburst Dwarf Galaxies

    Positive AGN Feedback Enhances Star Formation in Starburst Dwarf Galaxies. arXiv e-prints , keywords =. doi:10.48550/arXiv.2510.20897 , archivePrefix =. 2510.20897 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2510.20897

  45. [45]

    arXiv e-prints , keywords =

    Super-Eddington Chimneys: On the Cooling Evolution of Tidal Disruption Event Envelopes. arXiv e-prints , keywords =. doi:10.48550/arXiv.2512.14810 , archivePrefix =. 2512.14810 , primaryClass =

    work page doi:10.48550/arxiv.2512.14810

  46. [46]

    Discovery of transient infrared emission from dust heated by stellar tidal disruption flares

    Discovery of Transient Infrared Emission from Dust Heated by Stellar Tidal Disruption Flares. , keywords =. doi:10.3847/0004-637X/829/1/19 , archivePrefix =. 1605.04304 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/829/1/19

  47. [47]

    , keywords =

    Seventeen Tidal Disruption Events from the First Half of ZTF Survey Observations: Entering a New Era of Population Studies. , keywords =. doi:10.3847/1538-4357/abc258 , archivePrefix =. 2001.01409 , primaryClass =

    work page doi:10.3847/1538-4357/abc258 2001

  48. [48]

    , keywords =

    Reverberation in Tidal Disruption Events: Dust Echoes, Coronal Emission Lines, Multi-wavelength Cross-correlations, and QPOs. , keywords =. doi:10.1007/s11214-021-00835-6 , archivePrefix =. 2107.12268 , primaryClass =

    work page doi:10.1007/s11214-021-00835-6

  49. [49]

    , keywords =

    Interpretation of the Observed Neutrino Emission from Three Tidal Disruption Events. , keywords =. doi:10.3847/1538-4357/acbe9e , archivePrefix =. 2205.11538 , primaryClass =

    work page doi:10.3847/1538-4357/acbe9e

  50. [50]

    The Wide-field Infrared Survey Explorer (WISE): Mission Description and Initial On-orbit Performance

    The Wide-field Infrared Survey Explorer (WISE): Mission Description and Initial On-orbit Performance. , keywords =. doi:10.1088/0004-6256/140/6/1868 , archivePrefix =. 1008.0031 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/140/6/1868

  51. [51]

    , keywords =

    A Torus Remnant Revealed by the Infrared Echo of Tidal Disruption Event AT 2019qiz: Implications for the Missing Energy and Quasiperiodic Eruption Formation. , keywords =. doi:10.3847/2041-8213/adf229 , archivePrefix =. 2507.13251 , primaryClass =

    work page doi:10.3847/2041-8213/adf229 2041

  52. [52]

    Proper image subtraction - optimal transient detection, photometry and hypothesis testing

    Proper Image Subtraction Optimal Transient Detection, Photometry, and Hypothesis Testing. , keywords =. doi:10.3847/0004-637X/830/1/27 , archivePrefix =. 1601.02655 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/830/1/27

  53. [53]

    Do AGN outflows quench or enhance star formation?

    Do AGN outflows quench or enhance star formation?. , keywords =. doi:10.1093/mnras/stx787 , archivePrefix =. 1703.10782 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx787