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arxiv: 2601.16082 · v2 · submitted 2026-01-22 · 🌀 gr-qc

Recognition: 2 theorem links

· Lean Theorem

Roche limit and stellar disruption in the Simpson--Visser spacetime

Marcos V. de S. Silva
Authors on Pith no claims yet

Pith reviewed 2026-05-16 11:57 UTC · model grok-4.3

classification 🌀 gr-qc
keywords Roche limitSimpson-Visser spacetimetidal forcesblack holeneutron starwhite dwarfaffine modelstellar disruption
0
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The pith

The Simpson-Visser regularized metric shifts the Roche limit for tidal disruption of stars near black holes.

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

The paper calculates how tidal forces from a Simpson-Visser black bounce act on neutron stars, white dwarfs, and Sun-like stars, comparing the forces to each star's self-gravity to locate the Roche radius where disruption occurs. It does this for both a static observer and a radially infalling observer, finding that the choice of observer changes the measured forces. The work then checks, for black holes the mass of M87* and Sgr A*, whether the disruption point lies inside or outside the event horizon and therefore whether it could be observed. A dynamical affine model is applied to track how the stellar axes stretch and compress during infall under the regularized geometry.

Core claim

In the Simpson-Visser spacetime the tidal forces produce Roche radii that depend on the regularization parameter; for astrophysical black-hole masses these radii place some stellar disruptions outside the event horizon, making them potentially observable, while the affine model shows that the black-hole mass and the regularization together control the time evolution of the three principal axes of the infalling star.

What carries the argument

The Simpson-Visser metric (a regular black-bounce spacetime) together with the geodesic-deviation equation for tidal forces and the affine model for dynamical stellar deformation.

If this is right

  • For the same black-hole mass the Roche radius is smaller than in Schwarzschild spacetime when the regularization parameter is non-zero.
  • Neutron-star disruptions around M87* and Sgr A* occur inside the horizon and are therefore unobservable, while white-dwarf and Sun-like star disruptions can occur outside the horizon.
  • The affine model predicts that the stellar deformation rate increases with black-hole mass and is reduced by the presence of the bounce regularization.
  • Some tidal-disruption events become observable only because the regularized geometry moves the Roche surface outward relative to the horizon.

Where Pith is reading between the lines

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

  • Repeated observations of the radial distance at which stars are disrupted could place empirical bounds on the regularization parameter.
  • The same calculation framework can be applied to other regular black-hole metrics to compare their predicted disruption signatures.
  • If the affine-model axis evolution matches future gravitational-wave or electromagnetic data from stellar inspirals, it would support the use of regularized metrics for near-horizon astrophysics.

Load-bearing premise

The Simpson-Visser metric is assumed to be a realistic description of spacetime near real astrophysical black holes.

What would settle it

A measured tidal-disruption distance for a Sun-like star around Sgr A* that lies outside the calculated Roche radius for any allowed regularization parameter would falsify the model's prediction.

Figures

Figures reproduced from arXiv: 2601.16082 by Marcos V. de S. Silva.

Figure 1
Figure 1. Figure 1: Comparison of the radius at which the angular com [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Comparison of the radius at which the angular [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: In the left panel, we compare the Roche radius of a neutron star for different values of [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: In the left panel, we compare the Roche radius of a white dwarf for different values of [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: In the left panel, we compare the Roche radius of a Sun-like star for different values of [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
read the original abstract

Due to the tidal forces that a black hole can produce, certain types of compact objects may undergo disruption as they approach the black hole. This disruption point is known as the Roche limit (or Roche radius). In this work, we studied the tidal forces arising from the presence of the Simpson--Visser black bounce. We analyzed the tidal forces both for a static observer and for a radially infalling observer and showed that differences arise depending on the choice of observer. We used the tidal forces together with the stellar binding forces to determine the Roche radius for neutron stars, white dwarfs, and Sun-like stars, and to investigate how the Simpson--Visser regularization affects the tidal disruption of these astrophysical objects. We also examined whether, for astrophysical black holes such as M87* and Sgr~A*, these stellar disruption processes occur inside or outside the event horizon, and thus whether they are observable. To provide a more realistic dynamical description, we implement the Affine Model to evaluate the tidal deformation of neutron stars, white dwarfs, and main-sequence stars, assessing how the regularized geometry and the black hole mass govern the evolution of the stellar axes.

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 computes tidal forces in the Simpson-Visser regularized black-hole spacetime from the Riemann tensor for both static and radially infalling observers. These forces are set equal to Newtonian stellar binding energies to obtain Roche radii for neutron stars, white dwarfs, and Sun-like stars, and the affine model is employed to track the dynamical evolution of the stellar axes. The work further determines whether the resulting disruption radii lie inside or outside the event horizon for the supermassive black holes M87* and Sgr A*.

Significance. If the hybrid matching procedure is placed on a firmer footing, the calculation supplies a concrete, parameter-dependent prediction for how the Simpson-Visser regularization shifts the Roche limit relative to Schwarzschild, together with an assessment of observability for astrophysical black holes. The explicit comparison of static versus infalling observers and the inclusion of the affine model constitute the main technical contributions.

major comments (2)
  1. [§4] §4 (Roche-radius calculation): the tidal acceleration extracted from the Riemann tensor is equated directly to a Newtonian estimate of stellar self-gravity. This hybrid construction is inconsistent for neutron stars (and marginally for white dwarfs) once the tidal radius approaches the horizon scale, because the internal structure of the star can no longer be treated as Newtonian when the external curvature radius becomes comparable to the stellar radius.
  2. [§6] §6 (affine-model implementation): the initial conditions and restoring forces in the affine model are taken to be Newtonian, so the same mismatch between the GR tidal tensor and Newtonian binding forces propagates into the dynamical evolution of the stellar axes.
minor comments (1)
  1. [Abstract] The abstract refers to the spacetime as a 'black bounce' while the title uses 'Simpson--Visser spacetime'; a single consistent terminology should be adopted throughout.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful reading of our manuscript and for the constructive comments on the hybrid matching procedure. We address each major comment below, indicating the revisions made to strengthen the discussion of approximations and their validity.

read point-by-point responses

  1. Referee: [§4] §4 (Roche-radius calculation): the tidal acceleration extracted from the Riemann tensor is equated directly to a Newtonian estimate of stellar self-gravity. This hybrid construction is inconsistent for neutron stars (and marginally for white dwarfs) once the tidal radius approaches the horizon scale, because the internal structure of the star can no longer be treated as Newtonian when the external curvature radius becomes comparable to the stellar radius.

    Authors: We appreciate the referee's identification of this limitation in the hybrid approach. Equating the GR tidal field (from the Riemann tensor) to Newtonian stellar self-gravity is a standard approximation in the tidal-disruption literature, including studies in Schwarzschild and Kerr spacetimes. For neutron stars the approximation is indeed less reliable when the Roche radius approaches the horizon scale, as the stellar interior requires a relativistic treatment. In our calculations for the supermassive black holes M87* and Sgr A*, the neutron-star Roche radii lie inside the event horizon; we have therefore added an explicit paragraph in the revised §4 discussing the range of validity of the matching procedure, the regimes where the Newtonian self-gravity assumption breaks down, and the indicative nature of the results for compact objects. For white dwarfs and Sun-like stars the approximation remains more robust, as their Roche radii are larger relative to the horizon. revision: partial

  2. Referee: [§6] §6 (affine-model implementation): the initial conditions and restoring forces in the affine model are taken to be Newtonian, so the same mismatch between the GR tidal tensor and Newtonian binding forces propagates into the dynamical evolution of the stellar axes.

    Authors: We agree that the affine model inherits the hybrid character of the tidal-force calculation. The model is used to evolve the stellar axes under the Simpson-Visser tidal tensor while retaining Newtonian restoring forces, following the conventional implementation in the literature. We have revised §6 to state these approximations explicitly, to note that the dynamical results are subject to the same limitations discussed in §4, and to clarify that a fully relativistic hydrodynamical treatment would be needed for quantitative accuracy near the horizon, especially for neutron stars. The revised text also emphasizes that the affine-model results are intended to illustrate the qualitative dependence on the regularization parameter and black-hole mass rather than to provide precise quantitative predictions for compact objects. revision: partial

Circularity Check

0 steps flagged

Derivation self-contained from given metric and standard stellar binding energies

full rationale

The paper computes tidal accelerations directly from the Riemann tensor components of the Simpson-Visser line element for static and radially infalling observers, then sets these equal to Newtonian stellar self-gravity estimates to locate the Roche radius. No parameters are fitted to subsets of data and then relabeled as predictions; the affine model extension uses standard initial conditions without internal fitting loops. No self-citations are load-bearing for the central claim, and the metric itself is taken as an external input. The chain therefore does not reduce to its own inputs by construction.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim rests on the Simpson-Visser metric as a regularized black-hole solution and on standard Newtonian stellar binding energies; the regularization parameter is an input from the metric definition.

free parameters (1)
  • regularization parameter
    The bounce scale in the Simpson-Visser line element is a free parameter of the metric that controls the size of the regular core and must be chosen or constrained.
axioms (2)
  • domain assumption The Simpson-Visser metric solves the Einstein equations with a regular core
    The paper takes this metric as given and computes tidal forces within it.
  • domain assumption Stellar binding forces can be compared directly to geodesic deviation tidal forces
    The Roche-limit calculation equates the two without relativistic corrections to the star's internal structure.

pith-pipeline@v0.9.0 · 5497 in / 1387 out tokens · 22787 ms · 2026-05-16T11:57:38.650102+00:00 · methodology

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Reference graph

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