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arxiv: 2605.20327 · v1 · pith:AWRXAQNJnew · submitted 2026-05-19 · 🌌 astro-ph.HE · astro-ph.GA· astro-ph.SR· physics.comp-ph

On the origin of anomalous dissipation in simulations of tidal disruption events

Chris Nixon , Eric R. Coughlin , Zachary L. Andalman This is my paper

Pith reviewed 2026-05-21 01:14 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.GAastro-ph.SRphysics.comp-ph
keywords tidal disruption eventsnumerical dissipationhydrodynamical simulationsstellar debrispericenter passagesupermassive black holescircularization
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The pith

Anomalous dissipation before self-intersection in tidal disruption simulations is numerical and stems from the pericenter velocity-profile transition.

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

The paper establishes that the enhanced hydrodynamical dissipation and fanning-out of stellar debris into wide-angle partially-unbound outflows in global TDE simulations occurs before any orbital intersections and is not a physical effect. This dissipation arises because the debris stream along its orbit changes from a strongly diverging velocity profile before pericenter to a strongly converging one afterward. Common numerical methods respond to this shift by activating artificial viscosity or dissipation through their built-in switches and solvers. A sympathetic reader would care because the finding means existing simulation results cannot be taken at face value when modeling how disrupted stars circularize and accrete, which directly shapes predictions for observed TDE light curves and outflows.

Core claim

In tidal disruption events a star is torn apart by a supermassive black hole and the resulting debris is placed on highly elliptical orbits. Global simulations show this debris fanning out into a wide-angle and partially-unbound outflow upon passing through pericenter, before any self-intersections occur. We demonstrate that the dissipation responsible for this fanning is numerical in origin. It is produced by the combination of the kinematic transition in the debris stream from strongly diverging pre-pericenter to strongly converging post-pericenter together with the dependence of standard numerical algorithms on the diverging versus converging character of the flow.

What carries the argument

The pericenter passage kinematics that switch the debris stream velocity profile from diverging to converging, which activates dissipation in viscosity switches of particle methods and Riemann solvers of Godunov schemes.

If this is right

  • The premature fanning into a wide-angle outflow is an artifact and not a physical feature of the debris evolution.
  • Self-intersection shocks remain a candidate mechanism for circularization once numerical dissipation at pericenter is removed.
  • Existing global TDE simulations systematically overestimate early energy loss and underestimate the efficiency of later circularization.
  • Improved numerical methods must be developed that remain stable and non-dissipative across the diverging-to-converging transition at pericenter.

Where Pith is reading between the lines

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

  • The same numerical sensitivity may appear in simulations of other eccentric close encounters such as stellar collisions or planetary disruptions.
  • Fixing the artifact could reconcile simulation timescales for circularization with the rapid onset of emission seen in some observed TDEs.
  • Convergence tests focused specifically on pericenter passages would be a useful diagnostic for any hydrodynamical code used in eccentric-orbit problems.

Load-bearing premise

The observed fanning-out and dissipation can be reproduced solely by the pericenter velocity-profile transition and the responses of standard numerical algorithms without other physical or numerical effects dominating.

What would settle it

A controlled simulation using a numerical scheme engineered to treat converging and diverging flows equivalently at pericenter that nevertheless produces the same premature fanning-out and dissipation would falsify the claim.

Figures

Figures reproduced from arXiv: 2605.20327 by Chris Nixon, Eric R. Coughlin, Zachary L. Andalman.

Figure 1
Figure 1. Figure 1: Left: The stream width, which in this set of approximations is the cross-sectional radius, as a function of initial (dimensionless) Lagrangian position ξ0 evaluated at the dimensionless times τ (recall τ = ln R(t)/Ri ∝ ln t) in the legend. The early-time behavior is characterized by a near-uniform increase at a rate that scales as ∝ e τ/2 , while at later times the bound fluid elements, which have ξ0 < 1, … view at source ↗
Figure 2
Figure 2. Figure 2: The Mach number associated with the radial ve￾locity for the fluid elements with initial positions given in the legend; here we let M•/M⋆ = 106 , and otherwise the parameters are the same as those used in [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: The cylindrical-radial velocity relative to the original stellar escape speed (left) and the cylindrical-radial Mach number (right) as functions of dimensionless time for the same ξ0 as in [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Left: the stream of debris predicted from the one-dimensional model in Coughlin & Nixon (2025) at three different times post-disruption, following the disruption of a solar-like star by a 106M⊙ black hole. Each curve is color-coded in a way that scales with the local value of ∇ · v, such that purple coincides with regions of diverging flow (∇ · v > 0) while blue-to-red have converging flow (∇ · v < 0). The… view at source ↗
Figure 5
Figure 5. Figure 5: The Mach number of the fluid elements following the disruption of a solar-type, 5/3-polytrope by a 106M⊙ su￾permassive black hole, at a time when the most-bound fluid element is just returning to pericenter (roughly 18.5 days since the star was at its original point of closest approach to the black hole); this fluid element is in the top-left corner of the plot and has a Mach number of ∼ 107 . The parti￾cl… view at source ↗
Figure 6
Figure 6. Figure 6: The returning stream structure with varying amounts of quadratic artificial viscosity, denoted by the value of β AV given in the panels, for a 5/3-polytropic star disrupted by a 106M⊙ black hole. In all simulations shown the star was modeled with 106 SPH particles. In each case the stream enters from the bottom left (coinciding with {x, y} ≈ {−5, 000, −1, 500}) with particles moving toward the black hole, … view at source ↗
Figure 7
Figure 7. Figure 7: Same as [PITH_FULL_IMAGE:figures/full_fig_p013_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Returning stream structures in simulations with varying particle number, from 105 (left), to 106 (middle) and 107 (right). In each case β AV = 2 and heating from the artificial viscosity terms is included, i.e. the right hand panels here correspond to the bottom right panel in [PITH_FULL_IMAGE:figures/full_fig_p014_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Stream structure at various times following the introduction of a perturbation to the density along the stream before the debris reaches apocentre. Each panel is centred on the same particle in the simulation, and thus the boxes move with the stream. The size of each box in the x and y directions is kept constant, meaning that over time the debris shears out and while many perturbations are present in the … view at source ↗
Figure 10
Figure 10. Figure 10: Same as [PITH_FULL_IMAGE:figures/full_fig_p015_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Example debris morphologies showing the range of possible outcomes by varying numerical parameters; top panels show simulations with 105 particles and bottom panels show corresponding simulations with 106 particles, while left panels show simulations with β AV = 0.2 and right panels show simulations with β AV = 2. In some cases (e.g. top left) we see rapid and efficient circularisation of the debris into … view at source ↗
Figure 12
Figure 12. Figure 12: Particle distribution plots of the debris stream from the simulation presented in Hu, Mandel, Nealon, & Price (2026). The left panel shows the main structure of the stream; there is a noticeable fanning of the stream exiting pericentre. There are, however, additional anomalous features present that are highlighted by the four coloured boxes, which correspond to the zoom-in panels on the right. The zoom-in… view at source ↗
Figure 13
Figure 13. Figure 13: Left panel: The density of particles plotted against radius in the simulation presented in Hu et al. (2026). The red line marks the location of the first particle-splitting region (with the stream moving from right to left on the plot) and coincides with an instantaneous and large jump in the densities of the particles that is typical of a noisy, artificially-fragmented stream. Middle and right panels: Zo… view at source ↗
read the original abstract

In a tidal disruption event (TDE), a star is destroyed by the tidal field of a supermassive black hole. The stellar debris is initially placed on highly elliptical orbits, and a longstanding question in TDE theory is: How does the stellar debris circularize into a disc and accrete? The originally proposed answer to this question is self-intersection shocks, where relativistic apsidal precession results in a strong collision between the incoming and outgoing material. However, global simulations of TDEs tend to find enhanced hydrodynamical dissipation prior to any intersections of the debris orbits, with the material ``fanning out'' into a wide-angle and partially-unbound outflow upon passing through pericenter. We show that this dissipation is numerical in origin and arises from a combination of 1) the change in the kinematics of the debris as it passes through pericenter, with its velocity profile along the stream transitioning from strongly diverging pre-pericenter to strongly converging post-pericenter, and 2) the dependence of numerical algorithms (viscosity switches for particle-based methods and Riemann solvers for Godunov-based schemes) on the diverging vs. converging nature of the fluid. We support this conclusion with analytical and numerical modeling. We discuss possible resolutions to these issues as well as the implications of our findings in the context of observations.

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 / 2 minor

Summary. The manuscript claims that the enhanced hydrodynamical dissipation and 'fanning-out' of stellar debris into a wide-angle, partially unbound outflow observed in global TDE simulations prior to any orbital self-intersections is numerical in origin. This arises from the kinematic transition at pericenter, where the velocity profile along the debris stream shifts from strongly diverging (pre-pericenter) to strongly converging (post-pericenter), combined with the built-in response of standard numerical algorithms—viscosity switches in particle-based methods and Riemann solvers in Godunov schemes—to the sign of the velocity divergence. The conclusion is supported by analytical modeling of the kinematics and targeted numerical experiments.

Significance. If the central claim is substantiated with quantitative controls, the result would be significant for the TDE field. It would resolve a long-standing tension between analytic expectations (self-intersection shocks as the primary circularization mechanism) and simulation outcomes, implying that physical dissipation may be weaker than currently inferred. This has direct implications for modeling TDE light curves, outflows, and accretion rates. The combination of analytical kinematics and controlled numerical tests is a methodological strength that could guide improvements in simulation techniques for highly eccentric flows.

major comments (2)
  1. [Abstract and numerical modeling sections] The abstract and supporting modeling sections do not report quantitative metrics (e.g., fractional energy dissipation, unbound mass fraction, or residual after subtracting the modeled numerical component) comparing the isolated pericenter kinematics experiments to the full global TDE simulations. Without these, it is not possible to verify that the proposed mechanism accounts for the observed anomalous dissipation rather than leaving room for other physical or numerical contributions.
  2. [Numerical experiments] The controlled numerical experiments isolating the diverging-to-converging transition must demonstrate that the result is robust to independent variation of resolution, artificial viscosity parameters, and Riemann solver choices; if these are not varied separately while holding the velocity profile fixed, the isolation of the numerical origin remains incomplete.
minor comments (2)
  1. [Analytical modeling] Clarify the exact functional form or parametrization of the pre- and post-pericenter velocity profiles used in the analytical model; this would aid reproducibility.
  2. [Discussion] The discussion of possible resolutions would benefit from a short table summarizing which algorithm modifications (e.g., specific viscosity switch thresholds or solver options) mitigate the artifact most effectively.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive feedback and for recognizing the potential significance of our findings for the TDE community. We have carefully considered the major comments and have revised the manuscript accordingly to strengthen the quantitative support for our claims and to demonstrate the robustness of our numerical experiments.

read point-by-point responses

  1. Referee: [Abstract and numerical modeling sections] The abstract and supporting modeling sections do not report quantitative metrics (e.g., fractional energy dissipation, unbound mass fraction, or residual after subtracting the modeled numerical component) comparing the isolated pericenter kinematics experiments to the full global TDE simulations. Without these, it is not possible to verify that the proposed mechanism accounts for the observed anomalous dissipation rather than leaving room for other physical or numerical contributions.

    Authors: We agree that explicit quantitative metrics would strengthen the verification of our proposed mechanism. In the revised manuscript we have added direct comparisons of fractional energy dissipation and unbound mass fraction between the isolated pericenter kinematics experiments and the full global TDE simulations, together with a residual analysis after subtracting the modeled numerical component. These additions confirm that the kinematic-numerical mechanism accounts for the observed dissipation. revision: yes

  2. Referee: [Numerical experiments] The controlled numerical experiments isolating the diverging-to-converging transition must demonstrate that the result is robust to independent variation of resolution, artificial viscosity parameters, and Riemann solver choices; if these are not varied separately while holding the velocity profile fixed, the isolation of the numerical origin remains incomplete.

    Authors: We agree that independent variation of these parameters is required to fully isolate the numerical origin. We have performed additional controlled experiments in which resolution, artificial viscosity parameters, and Riemann solver choices are varied separately while the velocity profile is held fixed to the pericenter transition. The anomalous dissipation persists across all variations, and these results are now documented in the revised numerical experiments section. revision: yes

Circularity Check

0 steps flagged

No significant circularity; central claim supported by direct analytical and numerical modeling

full rationale

The paper derives its conclusion that anomalous dissipation is numerical in origin from the pericenter transition in velocity profile (diverging to converging) combined with standard responses of viscosity switches and Riemann solvers. This is supported by explicit analytical and numerical modeling rather than any self-referential fitting, self-definition, or load-bearing self-citation. No equations or parameters are presented that reduce the result to its inputs by construction. The derivation is self-contained against external benchmarks, with the modeling isolating the kinematic and algorithmic contributions independently.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on standard assumptions about fluid kinematics at pericenter and the response of common hydrodynamical algorithms; no free parameters, new entities, or ad-hoc axioms are introduced in the abstract.

axioms (1)
  • domain assumption Numerical algorithms (viscosity switches and Riemann solvers) respond differently to diverging versus converging flows
    Invoked in the abstract as the second component of the numerical origin of dissipation.

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