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arxiv: 2606.02692 · v1 · pith:YFTIIXYUnew · submitted 2026-06-01 · 🌌 astro-ph.HE

The Role of Stellar Spin in Repeating Partial Tidal Disruption Events

Ananya Bandopadhyay , Benjamin Amend , Eric R. Coughlin , C. J. Nixon , Dheeraj R. Pasham , T. Wevers This is my paper

Pith reviewed 2026-06-28 12:59 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords repeating partial tidal disruption eventsstellar spinsupermassive black holeshydrodynamical simulationsHills mechanismmass losstransient light curves
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The pith

Initial rapid prograde spin of the star produces successively dimmer outbursts in repeating partial tidal disruptions.

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

The paper establishes that a star placed on a tight orbit around a supermassive black hole through binary breakup starts with rapid rotation aligned to its orbit. Hydrodynamical simulations of repeated partial disruptions then show that this spin reduces the mass stripped in each later encounter, producing a sequence of fainter peaks. This trend matches observations that earlier models without spin failed to recover. The result supplies indirect support for the binary-disruption channel as the origin of these repeating events.

Core claim

When a main-sequence star enters its first encounter with a supermassive black hole already spinning at tens of percent of breakup speed in the prograde direction, each successive partial stripping removes progressively less mass. The resulting light curve therefore exhibits a clear decline in peak luminosity from one outburst to the next. Simulations of stars more massive than one solar mass around a million-solar-mass black hole recover this dimming only for high, aligned spins.

What carries the argument

The magnitude and direction of the star's spin relative to orbital angular momentum, which alters the star's internal structure and the amount of mass removed at each pericenter passage.

If this is right

  • High prograde spin recovers the observed dimming trend across multiple encounters.
  • Low or retrograde spin does not produce the same decline in outburst strength.
  • The dimming therefore constitutes indirect evidence that the Hills binary-breakup process seeds the stars in rpTDEs.

Where Pith is reading between the lines

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

  • Light-curve morphology of rpTDEs could be used to infer the spin distribution of stars on tight orbits around supermassive black holes.
  • The same spin dependence may determine whether a star survives many encounters or is eventually fully disrupted.

Load-bearing premise

The star begins its first encounter already rotating rapidly because it formed through the breakup of a tight, tidally locked binary.

What would settle it

A set of simulations with zero initial stellar spin that nevertheless produces a clear sequence of dimmer outbursts would falsify the proposed mechanism.

Figures

Figures reproduced from arXiv: 2606.02692 by Ananya Bandopadhyay, Benjamin Amend, C. J. Nixon, Dheeraj R. Pasham, Eric R. Coughlin, T. Wevers.

Figure 1
Figure 1. Figure 1: Top [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Same as [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 4
Figure 4. Figure 4: shows the fallback rates, accreted mass, and angular velocity for the first four pericenter passages of a 3M⊙ MAMS star with λ = 0.8 and β = 1.0. Similar to the TAMS star, it undergoes a substantial increase in its average density as a result of mass loss. Thus, despite the tidal spin up on this orbit (with Ω < Ωp), it maintains a declining trend in the amount of mass stripped per encounter and in the peak… view at source ↗
Figure 5
Figure 5. Figure 5: Snapshots of the density profile for a 1M⊙ ZAMS star with λ = 0.7 (top), a 3M⊙ MAMS star with λ = 0.8 (middle panel) a 3M⊙ TAMS star with λ = 0.8 (bottom panel), at different stages in the relax phase with damping (left) and in isolation (right). We note that all of the curves lie essentially on top of one another, demonstrating that our relaxation procedure has produced an accurate, stable configuration … view at source ↗
read the original abstract

The repeated tidal stripping of a star by a supermassive black hole, known as a repeating partial tidal disruption event (rpTDE), can give rise to a transient that rebrightens months to years after the first outburst. Among the rpTDE candidates so far observed, some exhibit dimmer peak luminosities during each successive outburst, which is a trend that has not been reproduced from theoretical models when the star survives more than one encounter with the black hole. Here we suggest that this trend can be recovered if the partially disrupted star is initially (i.e., prior to its first mass-stripping event) rapidly rotating, which is expected if the star was placed on its orbit through the Hills breakup of a tidally locked and tight binary. We test this hypothesis with hydrodynamical simulations of high-mass ($\geqslant 1 M_{\odot}$) main sequence stars repeatedly partially disrupted by a $10^6 M_{\odot}$ black hole, and demonstrate that successively dimmer outbursts are indeed recovered for high (tens of percent breakup) and prograde (i.e., aligned with the orbital angular momentum) stellar spins. Our results provide strong indirect evidence for the operation of the Hills mechanism in seeding the stars in rpTDEs.

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 the observed trend of successively dimmer peak luminosities in some repeating partial tidal disruption events (rpTDEs) can be reproduced if the star begins with high (tens of percent of breakup) prograde spin prior to the first encounter. This initial spin state is posited as a natural outcome of the Hills mechanism acting on a tidally locked tight binary. Hydrodynamical simulations of ≥1 M⊙ main-sequence stars around a 10^6 M⊙ black hole are used to demonstrate that only high prograde spins recover the dimming trend, providing what the authors describe as strong indirect evidence for Hills seeding of rpTDE stars.

Significance. If the reported spin dependence is robust, the work supplies a concrete physical mechanism that can explain an otherwise unexplained observational trend in rpTDE candidates and connects the events to binary dynamics near supermassive black holes. The forward nature of the hydrodynamical simulations (no fitting or self-referential equations) is a methodological strength that permits direct comparison with future observations of spin-sensitive signatures.

major comments (2)
  1. [Introduction] Introduction and abstract: the statement that high prograde spin 'is expected' from the Hills breakup of a tidally locked tight binary is asserted without any supporting calculation, reference, or citation. This assumption is load-bearing for the claim of 'strong indirect evidence' for the Hills mechanism; without it the simulation results demonstrate only a possible spin dependence, not evidence for a specific seeding channel.
  2. [Methods] Simulation methods (likely §2 or §3): the manuscript provides no information on the hydrodynamical code, spatial resolution, initial stellar structure model, or the procedure used to convert simulated mass-loss rates into luminosity. These details are required to evaluate whether the recovered dimming trend for high prograde spins is converged and independent of numerical choices.
minor comments (1)
  1. Figure captions and axis labels should explicitly state the spin parameter values (fraction of breakup speed and direction) for each run to allow immediate comparison with the text.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed report. We address each major comment below and will revise the manuscript accordingly to improve clarity and completeness.

read point-by-point responses

  1. Referee: [Introduction] Introduction and abstract: the statement that high prograde spin 'is expected' from the Hills breakup of a tidally locked tight binary is asserted without any supporting calculation, reference, or citation. This assumption is load-bearing for the claim of 'strong indirect evidence' for the Hills mechanism; without it the simulation results demonstrate only a possible spin dependence, not evidence for a specific seeding channel.

    Authors: We acknowledge that the expectation of high prograde spin arising from the Hills breakup of a tidally locked tight binary is asserted in the introduction and abstract without an explicit supporting calculation or citation. This is a valid observation, as the interpretation as 'strong indirect evidence' for the Hills mechanism depends on this being a natural outcome. We will revise the introduction to include a short justification based on angular momentum conservation during binary disruption and relevant references to the literature on the Hills mechanism and tidally locked binaries, thereby strengthening the connection without altering the simulation results. revision: yes

  2. Referee: [Methods] Simulation methods (likely §2 or §3): the manuscript provides no information on the hydrodynamical code, spatial resolution, initial stellar structure model, or the procedure used to convert simulated mass-loss rates into luminosity. These details are required to evaluate whether the recovered dimming trend for high prograde spins is converged and independent of numerical choices.

    Authors: We agree that the methods section is missing these critical details, which are necessary for assessing convergence and reproducibility. We will expand the methods section to specify the hydrodynamical code, the spatial resolution employed, the initial stellar structure models, and the procedure for converting mass-loss rates to luminosity estimates. These additions will allow evaluation of whether the dimming trend for high prograde spins is robust. revision: yes

Circularity Check

0 steps flagged

No circularity; forward hydrodynamical simulations test spin hypothesis independently

full rationale

The paper's core result—that high prograde stellar spins produce successively dimmer outbursts—is obtained directly from hydrodynamical simulations of repeated partial disruptions. This is a forward-modeling output, not a fitted parameter, self-defined quantity, or result derived from self-citations. The initial-spin assumption (from Hills breakup of a tidally locked binary) is presented as the hypothesis under test rather than an input that forces the outcome by construction. No equations reduce the claimed prediction to the inputs, and no load-bearing self-citation or ansatz smuggling is present in the derivation chain. The paper is self-contained against external benchmarks via explicit simulation setup.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The claim depends on the domain assumption that hydrodynamical simulations faithfully capture mass-loss and luminosity evolution, plus the modeling choice that the star begins with high prograde spin; no new entities are postulated and no parameters are fitted to the target data.

free parameters (1)
  • initial stellar spin fraction of breakup speed
    Selected at high values (tens of percent) to test the hypothesis rather than fitted to observed luminosities.
axioms (2)
  • domain assumption The star survives more than one partial disruption encounter
    Invoked in the setup of repeating events and the comparison to observed candidates.
  • domain assumption Hydrodynamical codes accurately model the interaction between stellar spin, orbital motion, and mass stripping
    Standard assumption in the field but required for the simulation results to map to real events.

pith-pipeline@v0.9.1-grok · 5773 in / 1461 out tokens · 32889 ms · 2026-06-28T12:59:43.068340+00:00 · methodology

discussion (0)

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