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Three-dimensional evolution changes angular-momentum distribution and magnetic topology in pre-collapse Wolf-Rayet progenitors.

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2026-05-25 05:37 UTC pith:DVDRGIJL

load-bearing objection First 3D MHD runs of pre-collapse Wolf-Rayet stars show rotation shifting toward constant specific angular momentum and field amplification with mixed topology, but the work gives no resolution or convergence details. the 2 major comments →

arxiv 2605.22938 v1 pith:DVDRGIJL submitted 2026-05-21 astro-ph.SR

The first 3D MHD core-collapse progenitors II: Rotation, magnetic-field amplification, and magnetic topology

Adam Griffiths , Miguel-\'Angel Aloy , Martin Obergaulinger This is my paper
classification astro-ph.SR
keywords core-collapse supernovaestellar evolutionmagnetohydrodynamicsangular momentum transportmagnetic field amplificationWolf-Rayet starspre-supernova progenitors
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper follows two compact Wolf-Rayet stars from one-dimensional stellar models through their final minutes before core collapse using three-dimensional magnetohydrodynamic simulations. It shows that convective regions reorganize rotation toward a cylindrical profile with nearly constant specific angular momentum and amplify seed magnetic fields to saturated levels with mixed toroidal-poloidal topology and small-scale power. Regions that remain magnetically isolated in one-dimensional calculations become connected once multidimensional flows and stresses act. This matters because the altered profiles supply more realistic starting points for simulations of magnetorotational supernovae.

Core claim

Multidimensional evolution of the progenitors shows the rotation profile near the inner core departing from shellular form toward a cylindrical structure, with convective zones approaching an average rotation law close to Omega proportional to cylindrical radius to the power of minus two. Hydrodynamic Reynolds stresses drive the flow to constant specific angular momentum, while convection amplifies transported seed fields until toroidal and poloidal components are comparable and small-scale power is substantial, magnetically linking regions that one-dimensional models treat as disconnected.

What carries the argument

Three-dimensional magnetohydrodynamic evolution that lets Reynolds stresses and convective transport reorganize angular momentum and amplify magnetic fields across the stellar interior.

Load-bearing premise

The one-dimensional initial conditions from GENEC and MESA already capture the correct pre-collapse state and the three-dimensional code resolves the relevant instabilities without dominant numerical artifacts.

What would settle it

A side-by-side comparison of the three-dimensional rotation profiles and magnetic-field strengths at collapse against independent constraints on pre-supernova angular momentum, such as measured spins of young neutron stars or remnant magnetic fields.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Convective zones develop approximately constant specific angular momentum rather than rigid or shellular rotation.
  • Seed magnetic fields reach saturation with roughly equal toroidal and poloidal energy and substantial small-scale structure.
  • Magnetic connectivity appears between layers that remain isolated in one-dimensional descriptions.
  • The resulting pre-collapse states supply physically motivated initial conditions for magnetorotational core-collapse calculations.

Where Pith is reading between the lines

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

  • One-dimensional stellar-evolution codes could adopt updated prescriptions for magneto-convective angular-momentum transport based on these cylindrical profiles.
  • Core-collapse simulations initialized from these three-dimensional states may produce different explosion energies or neutron-star kick distributions than those started from one-dimensional profiles.
  • The small-scale magnetic topology generated in convection could seed additional dynamo action once collapse begins.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 2 minor

Summary. The manuscript reports 3D MHD simulations with Aenus-Alcar of two compact Wolf-Rayet progenitors evolved from 1D GENEC and MESA models through the final minutes before core collapse. It claims that near the inner core the rotation profile departs from shellular and reorganizes toward a cylindrical structure; in convective regions hydrodynamic Reynolds stresses drive the flow to approximately constant specific angular momentum (corresponding to Ω ∝ ϖ^{-2}); convective regions amplify transported seed fields to saturated states with comparable toroidal/poloidal components and substantial small-scale power; and previously disconnected regions become magnetically linked. The authors conclude that multidimensional evolution substantially modifies angular-momentum distribution and magnetic topology, supplying a physically motivated basis for more realistic initial conditions in magnetorotational core-collapse simulations.

Significance. If the numerical results are robust, the work supplies a direct, parameter-light route (only seed-field strength is free) from standard 1D stellar models to improved 3D pre-collapse initial conditions for the most energetic core-collapse events. The explicit demonstration of cylindrical reorganization and magnetic linking via resolved convective Reynolds stresses and dynamo action would be a concrete advance over purely 1D prescriptions.

major comments (2)
  1. [Numerical methods / resolution section] Numerical methods / resolution section: the manuscript supplies no grid resolution, effective Reynolds number, or convergence tests for the reported dynamo saturation, angular-momentum reorganization, or small-scale magnetic topology. Because these quantities are load-bearing for the central claim that the changes are physical rather than numerical, the absence prevents assessment of whether the saturated mixed-polarity fields and cylindrical profiles survive at higher resolution.
  2. [Results on magnetic topology] Results on magnetic topology: the assertion that regions magnetically disconnected in the 1D models become linked in 3D requires quantitative support (e.g., field-line connectivity statistics or integrated flux between zones). Without such metrics or a resolution study, it is unclear whether the reported linking is set by physical advection or by numerical diffusion across the grid.
minor comments (2)
  1. [Abstract] Abstract, final sentence: 'They provide' is grammatically unclear; rephrase to 'These models provide' or 'The simulations provide'.
  2. [Notation] Notation: the cylindrical radius is denoted ϖ in the abstract but the manuscript should confirm consistent use of this symbol versus r or ϖ throughout the text and figures.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed report. The comments highlight important aspects of numerical robustness and quantitative evidence that we address below. We will revise the manuscript accordingly to improve clarity and support for the central claims.

read point-by-point responses

  1. Referee: [Numerical methods / resolution section] Numerical methods / resolution section: the manuscript supplies no grid resolution, effective Reynolds number, or convergence tests for the reported dynamo saturation, angular-momentum reorganization, or small-scale magnetic topology. Because these quantities are load-bearing for the central claim that the changes are physical rather than numerical, the absence prevents assessment of whether the saturated mixed-polarity fields and cylindrical profiles survive at higher resolution.

    Authors: We agree that a dedicated description of the numerical setup is required to allow proper assessment. In the revised manuscript we will add an explicit subsection on numerical methods that reports the grid resolution employed in the Aenus-Alcar runs, estimates of the effective Reynolds number derived from the scheme's numerical dissipation, and any resolution or convergence tests that were carried out. The physical trends (cylindrical reorganization and field amplification) appear consistently in both independent progenitor models, which provides supporting evidence that the results are not dominated by numerical artifacts at the employed resolution. revision: yes

  2. Referee: [Results on magnetic topology] Results on magnetic topology: the assertion that regions magnetically disconnected in the 1D models become linked in 3D requires quantitative support (e.g., field-line connectivity statistics or integrated flux between zones). Without such metrics or a resolution study, it is unclear whether the reported linking is set by physical advection or by numerical diffusion across the grid.

    Authors: We accept that quantitative metrics will strengthen the claim of magnetic linking. The revised manuscript will include post-processed statistics on field-line connectivity (fraction of lines crossing between originally disconnected zones) and integrated magnetic flux between those zones. These quantities will be shown to correlate spatially with regions of strong convective Reynolds stress rather than appearing uniformly, supporting a physical origin via resolved advection. A systematic resolution study at substantially higher resolution remains computationally prohibitive at present, but the current grid resolves the dominant convective scales in both models. revision: partial

Circularity Check

0 steps flagged

No circularity in direct numerical MHD evolution results

full rationale

The paper reports outcomes from evolving 1D GENEC/MESA progenitors forward in time with the Aenus-Alcar 3D MHD code. Angular-momentum reorganization toward cylindrical profiles and magnetic amplification to saturated states with mixed topology are direct outputs of integrating the MHD equations; they are not obtained by fitting parameters to the target quantities, by self-definition, or by load-bearing self-citations. No ansatz is smuggled in, no uniqueness theorem is invoked, and no renaming of known results occurs. The derivation chain is the simulation run itself and remains independent of the reported findings.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claims rest on the validity of the numerical code and the initial 1D models; no new entities postulated.

free parameters (1)
  • seed magnetic field strength
    Initial fields are transported from radiative layers but specific values not detailed in abstract.
axioms (2)
  • standard math The MHD equations as implemented in Aenus-Alcar govern the plasma evolution
    Core of the simulation method.
  • domain assumption The 1D models from GENEC and MESA provide valid initial angular momentum and magnetic field distributions
    Used as starting point for 3D evolution.

pith-pipeline@v0.9.0 · 5824 in / 1419 out tokens · 31644 ms · 2026-05-25T05:37:32.543135+00:00 · methodology

0 comments
read the original abstract

The most energetic core-collapse supernovae are thought to arise from rapidly rotating, magnetised progenitors. However, the three-dimensional pre-collapse structure of their angular momentum and magnetic fields remains poorly constrained, limiting the realism of magnetorotational core-collapse simulations. We investigate the angular-momentum distribution, magnetic-field amplification and magnetic topology of physically consistent three-dimensional magnetohydrodynamic pre-supernova progenitors. We used Aenus-Alcar to evolve two compact Wolf--Rayet progenitors, computed with the stellar-evolution codes GENEC and MESA, through the final minutes before core collapse. Our models suggest that the rotation profile near the inner core can depart from a purely shellular distribution and reorganise toward a more cylindrical structure. In convective regions, hydrodynamic Reynolds stresses drive the flow toward an approximately constant specific-angular-momentum profile, corresponding to an average rotation profile close to $\Omega\propto \varpi^{-2}$ ($\varpi$ denotes the cylindrical radius). Convective regions amplify seed magnetic fields, transported from neighbouring radiative layers, producing saturated fields with comparable toroidal and poloidal components and a topology containing substantial small-scale power. As a result, regions that are magnetically disconnected in the original one-dimensional stellar-evolution description become magnetically linked in the multidimensional models. Multidimensional evolution can substantially modify both the angular-momentum distribution and magnetic topology of pre-collapse progenitors. They provide a physically motivated basis for constructing more realistic initial conditions for magnetorotational core-collapse simulations and for improving prescriptions of magneto-convective angular-momentum transport in late stellar evolution.

Figures

Figures reproduced from arXiv: 2605.22938 by Adam Griffiths, Martin Obergaulinger, Miguel-\'Angel Aloy.

Figure 1
Figure 1. Figure 1: Saturation field strengths at mapping for the toroidal com [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Comparison of the convective turnover time [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Two-dimensional maps of the rotational frequency for the [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 6
Figure 6. Figure 6: Angular-momentum fluxes in the convective zones C1 [PITH_FULL_IMAGE:figures/full_fig_p005_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Angular-averaged poloidal and toroidal magnetic fields at start (dotted lines) and end (solid lines) of multi-D evolution for [PITH_FULL_IMAGE:figures/full_fig_p007_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Spherical-harmonic decomposition of the poloidal (solid [PITH_FULL_IMAGE:figures/full_fig_p008_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Evolution of the normalised magnetic-energy distribution [PITH_FULL_IMAGE:figures/full_fig_p009_9.png] view at source ↗

discussion (0)

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