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arxiv: 2606.22919 · v1 · pith:25OCQAEFnew · submitted 2026-06-22 · 🌌 astro-ph.HE

Are most detected tidal disruption events partial?

Megha Sharma (Monash University) , Daniel J. Price (Monash University , Univ. Grenoble Alpes) , Alexander Heger (Monash University) , Katie Auchettle (University of Melbourne , University of California , Santa Cruz) This is my paper

Pith reviewed 2026-06-26 08:11 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords tidal disruption eventspartial tidal disruptionsmass fallback ratereprocessing layerEddington limitSPH simulationsoptical luminosityblack hole accretion
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The pith

Partial tidal disruptions produce reprocessing layers and luminosities matching most detected events for beta at least 0.8.

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

The paper models the partial disruption of a one-solar-mass star by a million-solar-mass black hole on zero-energy orbits using smoothed particle hydrodynamics, focusing on cases with up to fifty percent mass loss. For impact parameters giving beta of 0.8 or higher the mass fallback rate exceeds the Eddington limit, so the returning debris can form an optically thick layer that reprocesses light from any inner accretion disc in the same way full disruptions do. The fallback rate declines more slowly than the usual t to the minus five-thirds power, staying closer to t to the minus nine-fourths. Under the assumptions of thermal emission from the debris, trapped shock heating, electron-scattering opacity and a color correction of 1.7, the models give temperatures near ten thousand kelvin, optical luminosities between ten to the forty-two and ten to the forty-four erg per second, and blackbody radii of ten to one hundred astronomical units. These values line up with observed optical and ultraviolet TDEs and with the properties of known repeating partial events, supporting the idea that some events classified as full disruptions are actually partial.

Core claim

Using SPH simulations of partial TDEs with mass loss up to fifty percent, the authors find that for beta greater than or equal to 0.8 the mass fallback rate exceeds the Eddington limit, allowing the debris to form a reprocessing layer that obscures the accretion disc and produces optical emission similar to full TDEs. The fallback rate follows a power law closer to t to the minus nine-fourths than the canonical t to the minus five-thirds. With the stated thermal-emission assumptions the models yield blackbody temperatures of about ten thousand kelvin, bolometric luminosities of ten to the forty-two to ten to the forty-four erg per second, and radii of ten to one hundred au, values that match

What carries the argument

the mass fallback rate exceeding the Eddington limit for beta greater than or equal to 0.8, which permits the returning debris to form an optically thick reprocessing layer around the accretion disc

If this is right

  • Mass fallback tracks closer to t to the minus nine-fourths than the usual t to the minus five-thirds.
  • Derived temperatures near ten thousand kelvin and optical luminosities of ten to the forty-two to ten to the forty-four erg per second match detected optical and ultraviolet TDEs.
  • Properties are similar to those of repeating partial TDEs such as ASASSN-19dj, ASASSN-14ko, ASASSN-18ul, ASASSN-22ci, AT2020vdq and AT2022dbl.
  • Some events currently classified as full disruptions may instead be partial ones that leave a stellar remnant.

Where Pith is reading between the lines

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

  • If the reprocessing mechanism works the same way, the observational boundary between full and partial TDEs becomes harder to draw from light curves alone.
  • The fraction of partial events among all detected TDEs may be larger than current estimates that assume only full disruptions produce bright optical flares.
  • Simulations that include non-zero energy orbits would test whether the same Eddington-exceeding fallback and reprocessing still occur for more typical stellar encounters.

Load-bearing premise

The emission calculation assumes thermal emission from the debris, that shock heating is trapped, that electron scattering dominates the opacity, and a color correction f_col of 1.7.

What would settle it

A well-observed TDE with estimated beta around 0.8 that shows bright X-rays without any optical reprocessing signature, or a light curve whose decay slope is measured to be inconsistent with t to the minus nine-fourths.

Figures

Figures reproduced from arXiv: 2606.22919 by Alexander Heger (Monash University), Daniel J. Price (Monash University, Katie Auchettle (University of Melbourne, Megha Sharma (Monash University), Santa Cruz), University of California, Univ. Grenoble Alpes).

Figure 1
Figure 1. Figure 1: Debris evolution over the initial 4 days of the simulation since t = 0. Pericentre passage occurs around 6.8−7.6 hours in all models. Each panel shows different ratios of the tidal radius to the pericentre distance (β; top to bottom), showing the column density perpendicular to the orbital plane (y-x). The grey circle corresponds to the tidal radius around the 106M⊙ black hole. Snapshots are shown super-im… view at source ↗
Figure 2
Figure 2. Figure 2: Debris evolution, showing column density perpendicular to the orbital plane at t = 95 days post-disruption for different ratios of the tidal radius to pericentre distance (β; top to bottom). The size of the reprocessing layer changes with the amount of material available in fallback material with low β disruptions producing a small/low mass reprocessing layer compared to high β disruptions. Each panel is 3… view at source ↗
Figure 3
Figure 3. Figure 3: Long term evolution of the β = 0.8 simulation, using adiabatic (top row) and isentropic (bottom row) approximations for the heating and cooling. The material returns to the pericentre around t = 26 days. Pericentre occurs at t ∼ 7.9 hours. Stream-stream collisions at apocentre result in the formation of a disc and (in the adiabatic case; top row) outflow structure around the black hole. With fast cooling (… view at source ↗
Figure 5
Figure 5. Figure 5: Temperature rendered z = 0 slice in y − x plane for β = 0.8 isentropic simulation at 98.9 days. Panel is 8 au × 8 au. The peak temperature is ∼ 4 × 105 K, implying hard X-ray emission. ends up as part of the expanding cloud of material. The size of this cloud varies between simulations, with higher β calculations producing clouds roughly ten times larger than lower β at around 100 days [PITH_FULL_IMAGE:fi… view at source ↗
Figure 4
Figure 4. Figure 4: tdiffuse as function of time for β = 0.8 (top panel) and β = 1.6 (bottom panel) for adiabatic simulations. The photon diffusion time is ∼ 1 day for β = 0.8, whereas for β = 1.6, its about 100 days. apocentre (the outer shock), which in turn allows ma￾terial to fall towards the black hole and drive kinetic outflows. Only a small amount of material forms a Ke￾plerian disc around the black hole, and most mate… view at source ↗
Figure 6
Figure 6. Figure 6: Spatial distribution of density (top), temperature (middle) and radial velocity (bottom) for β = 1.0 disruption at 98.9 days. Colours represent the density of points (mass per pixel) on the plot, with orange being a high density of points and blue being low. The x-axis represents the location of particles with respect to to the black hole placed at origin. The blackbody radius of this model is 32 au. The s… view at source ↗
Figure 7
Figure 7. Figure 7: Mass fallback rate as a function of time for all our models determined using material that enters 1,000 GM•/c2 (left panel, solid lines) and 6 GM•/c2 (right panel, solid lines), and calculated using the Newtonian energy to determine period at ∼ 4 days post-disruption (left panel, dash-dot-dot line). Solid and dash-dot-dot curves in the left panel match within a few percent, with higher β showing slight dif… view at source ↗
Figure 8
Figure 8. Figure 8: Synthetic spectral energy distributions computed for all models at 95 days (blue line). The blue line represents the observer in z axis and orange shows single temperature blackbody fit to the optical band. The green line represents the blackbody fit to the X-ray band. The total bolometric and inferred optical bolometric luminosity, and blackbody temperature for each model are listed in each panel. β reduc… view at source ↗
Figure 9
Figure 9. Figure 9: Evolution of bolometric (top panel) luminosity derived from the area under the orange curve in [PITH_FULL_IMAGE:figures/full_fig_p012_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: X-ray luminosity, radius and temperature of β = 0.8 isentropic simulation. Dotted line corresponds to circularisation radius of 2 rp, dashed is the ISCO and dash-- dotted is the Schwarzschild radius. probe the effect of different β have on the mass accreted onto the black hole. Our results demonstrate that even partial TDEs (i.e., where the mass loss is < 50%) can produce outflows with velocities of order… view at source ↗
Figure 11
Figure 11. Figure 11: Blackbody radius as function of time for β = 0.8 model. Brown, mustard, and teal-green show three resolu￾tions of the simulation after we replace the remnant with a point mass potential at 4 days, and use Splitpart to in￾crease resolution. Our estimated values of Rbb are converged with numerical resolution up to ∼ 100 days. around the black hole as shown in Figure A We see a similar behaviour in all of ou… view at source ↗
Figure 12
Figure 12. Figure 12: Column density of particles at 98.9 days since the start of the simulation. Pericentre approach takes place around 7.8 hours for β = 0.8 model. Left, middle and right panels corresponds to 1,021,464, 113,496 and 18,916 particles in our simulations. More particles results in disc formation even at 98 days. Each panel is 1,380 au × 580 au [PITH_FULL_IMAGE:figures/full_fig_p017_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Our fiducial β = 1.6 simulation (left panel; see [PITH_FULL_IMAGE:figures/full_fig_p017_13.png] view at source ↗
Figure 15
Figure 15. Figure 15: Spectral energy distributions at times ranging from 10 − 90 days for all simulations. As time increases, the colors of the lines moves towards darker shades of blue. Except for β = 0.6 simulation, other simulations show soft X-ray emission. Lau, M. Y. M., Hirai, R., González-Bolívar, M., et al. 2022, MNRAS, 512, 5462, doi: 10.1093/mnras/stac049 Law-Smith, J. A. P., Coulter, D. A., Guillochon, J., Mockler,… view at source ↗
read the original abstract

During a tidal disruption event (TDE), a star loses mass due to the tidal gravitational forces of the black hole. In a partial tidal disruption event, a stellar remnant is left behind. Several dozen TDEs have been detected so far, including repeating partial events. We use the Phantom smoothed particle hydrodynamics code to model the disruption of a 1 Msun star around a 10^6 Msun black hole for impact parameters resulting in less than equal to 50 % mass loss. We only consider zero energy orbits. Our simulations show that the mass fallback rate can exceed the Eddington limit for beta greater than or equal to 0.8, allowing debris to obscure the accretion disc by forming a reprocessing layer, similar to full TDEs. The mass fallback rate is shallower than t^{-5/3}, tracking closer to t^{-9/4}. Assuming thermal emission from the debris, that shock heating is trapped, that electron scattering dominates the opacity, and a color correction f_{col} of 1.7, we find temperatures of ~10^4 K, optical bolometric luminosities of ~ 10^{42-44} erg/s and blackbody radii ranging from 10-100 au for our simulations. We compare our values with observations and find support for the previous argument that some TDEs classified as full disruptions might actually be partial. Moreover, our results explain the detected optical/UV TDEs. We also find that our zero energy partial TDEs have properties similar to the repeating partial TDEs such as ASSASN-19dj, ASSASN-14ko, ASSASN-18ul, ASSASN-22ci, AT2020vdq and AT2022dbl. In the beta=0.8, isentropic simulation where radiation is assumed to escape, we find X-ray luminosities of ~ 10^{44-45} erg/s and radii lower than the inner most stable circular orbit.

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

3 major / 2 minor

Summary. The paper uses Phantom SPH simulations to model partial tidal disruptions (≤50% mass loss) of a 1 M⊙ star by a 10^6 M⊙ black hole on zero-energy orbits. For β ≥ 0.8 the mass fallback rate exceeds Eddington, enabling a reprocessing layer. Post-processing assuming thermal emission, trapped shock heating, electron-scattering opacity and f_col=1.7 yields T≈10^4 K, L_bol≈10^{42-44} erg/s and R_bb≈10-100 au. These are compared to observations to argue that some TDEs classified as full disruptions are actually partial, that this explains optical/UV TDEs, and that zero-energy partials resemble repeating events such as ASASSN-19dj.

Significance. If the emission post-processing is robust, the result would imply that partial TDEs with β≥0.8 can reproduce the luminosities, temperatures and radii of many observed optical/UV TDEs, potentially revising event classification and the inferred fraction of full versus partial disruptions. The hydrodynamic fallback rates are generated independently of the observational sample, which is a methodological strength.

major comments (3)
  1. [Abstract] Abstract (emission calculation): The mapping from simulated fallback rates to the reported T~10^4 K, L_bol~10^{42-44} erg/s and R_bb~10-100 au rests entirely on four assumptions (thermal emission, trapped shocks, electron-scattering opacity, fixed f_col=1.7). No sensitivity tests or radiative-transfer validation are shown for the super-Eddington debris regime; if absorption opacity contributes or heating is not fully trapped, the match to observations does not hold. This is load-bearing for the central claim.
  2. [Results (X-ray case)] X-ray results (β=0.8 isentropic case): X-ray luminosities ~10^{44-45} erg/s and radii below the ISCO are obtained only when radiation is assumed to escape. The justification for switching from trapped to escaping radiation between the optical and X-ray cases is not provided and directly affects the claimed distinction between emission regimes.
  3. [Comparison with observations] Comparison with observations: The argument that some events classified as full TDEs are partial, and that partial TDEs explain optical/UV detections, relies on the derived quantities matching data. No error bars, convergence tests on the fallback rates, or quantitative fit statistics are reported, so the strength of the observational support cannot be assessed.
minor comments (2)
  1. [Abstract] The fallback rate is stated to track closer to t^{-9/4} than t^{-5/3}; specify the time interval over which this power-law holds and any β dependence.
  2. Clarify the precise range of β values simulated that correspond to ≤50% mass loss.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive report and positive assessment of the methodological approach. We address each major comment below. Where the comments identify areas needing clarification or additional discussion, we have revised the manuscript accordingly.

read point-by-point responses

  1. Referee: [Abstract] Abstract (emission calculation): The mapping from simulated fallback rates to the reported T~10^4 K, L_bol~10^{42-44} erg/s and R_bb~10-100 au rests entirely on four assumptions (thermal emission, trapped shocks, electron-scattering opacity, fixed f_col=1.7). No sensitivity tests or radiative-transfer validation are shown for the super-Eddington debris regime; if absorption opacity contributes or heating is not fully trapped, the match to observations does not hold. This is load-bearing for the central claim.

    Authors: We agree that the post-processing relies on standard assumptions also used in prior TDE modeling (e.g., thermal emission and electron-scattering opacity in super-Eddington flows). Full radiative-transfer calculations are beyond the scope of this hydrodynamic study. In revision we have expanded the methods section to discuss the sensitivity of the derived T, L_bol and R_bb to variations in f_col (tested between 1.5-2.0) and to the assumption of trapped heating, noting that the optical/UV match holds provided electron scattering remains dominant. We have also added a caveat paragraph on the limitations of the simple post-processing. revision: partial

  2. Referee: [Results (X-ray case)] X-ray results (β=0.8 isentropic case): X-ray luminosities ~10^{44-45} erg/s and radii below the ISCO are obtained only when radiation is assumed to escape. The justification for switching from trapped to escaping radiation between the optical and X-ray cases is not provided and directly affects the claimed distinction between emission regimes.

    Authors: The switch is motivated by the lower mass-loss fraction and correspondingly lower column density in the β=0.8 isentropic run, which permits radiation to escape rather than being trapped. We have added an explicit paragraph in the results section justifying this choice on physical grounds and clarifying that the optical case assumes trapping while the X-ray case does not. revision: yes

  3. Referee: [Comparison with observations] Comparison with observations: The argument that some events classified as full TDEs are partial, and that partial TDEs explain optical/UV detections, relies on the derived quantities matching data. No error bars, convergence tests on the fallback rates, or quantitative fit statistics are reported, so the strength of the observational support cannot be assessed.

    Authors: We acknowledge that quantitative fit statistics and formal error bars on the fallback rates would allow a more rigorous assessment. The SPH runs use standard Phantom resolution; we have added a brief convergence note in the methods. The comparison is presented as qualitative consistency rather than a statistical claim, given the limited parameter space explored. We have revised the discussion to emphasize this indicative nature and to avoid overstatement of the observational support. revision: partial

Circularity Check

0 steps flagged

No significant circularity; forward modeling from independent hydrodynamics

full rationale

The derivation begins with Phantom SPH simulations that generate mass fallback rates for partial disruptions (beta <=1) on zero-energy orbits. These rates are then post-processed under four explicitly listed assumptions (thermal emission from debris, trapped shock heating, electron-scattering opacity, f_col=1.7) to obtain T~10^4 K, L_bol~10^42-44 erg/s and R_bb~10-100 au. The resulting quantities are compared to observations rather than fitted to them; no equation reduces the predicted luminosities or temperatures to a quantity derived from the same observational sample, and no load-bearing step relies on self-citation or an imported uniqueness theorem. The central claim therefore remains an independent prediction from the hydrodynamic inputs.

Axiom & Free-Parameter Ledger

2 free parameters · 3 axioms · 0 invented entities

The central claim rests on hydrodynamic simulations plus several explicit post-processing assumptions for radiation; these are domain-standard but not independently verified within the work.

free parameters (2)
  • f_col = 1.7
    Color correction factor fixed at 1.7 for temperature-to-luminosity conversion
  • beta threshold = 0.8
    Impact parameter cutoff (beta >= 0.8) chosen to produce super-Eddington fallback
axioms (3)
  • domain assumption Only zero-energy orbits are considered
    Stated restriction on orbital energy in the simulation setup
  • domain assumption Thermal emission, trapped shock heating, electron-scattering opacity
    Explicit assumptions used to convert fallback rates into luminosities and temperatures
  • domain assumption Mass fallback rate directly sets the reprocessing-layer properties
    Core modeling link between hydrodynamics and observed emission

pith-pipeline@v0.9.1-grok · 5923 in / 1685 out tokens · 21490 ms · 2026-06-26T08:11:58.645801+00:00 · methodology

discussion (0)

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