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arxiv: 2605.22927 · v1 · pith:3URQEVZInew · submitted 2026-05-21 · 🌌 astro-ph.SR

The first 3D MHD core-collapse progenitors I: General properties, convection and nuclear burning

Adam Griffiths , Miguel-\'Angel Aloy , Martin Obergaulinger This is my paper

Pith reviewed 2026-05-25 05:45 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords 3D MHD simulationspre-supernova progenitorsturbulent mixingnuclear burningcore-collapse supernovaestellar convectionWolf-Rayet starsmultidimensional stellar evolution
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The pith

Three-dimensional MHD models show turbulent velocities in oxygen-burning shells exceed mixing-length theory by a factor of two.

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

The paper constructs the first three-dimensional magnetohydrodynamic pre-supernova progenitors by mapping one-dimensional models from GENEC and MESA into a multidimensional code several minutes before collapse. It evolves these rotating, magnetized Wolf-Rayet models forward until core collapse to examine convection and nuclear burning in the oxygen and silicon shells. The simulations find that turbulent velocities in extended oxygen-burning shells reach roughly twice the values predicted by standard mixing-length theory, while a thin silicon-burning shell exhibits reduced mixing near its boundaries and an effective diffusion profile that departs from one-dimensional prescriptions. These multidimensional effects alter the spatial extent and efficiency of nuclear burning, prompting the authors to propose updated prescriptions for one-dimensional stellar evolution codes. The resulting models are presented as initial conditions for future core-collapse and explosion calculations.

Core claim

We used Aenus-ALCAR to perform three-dimensional magnetohydrodynamic simulations of two compact Wolf-Rayet progenitors obtained from the stellar evolution codes GENEC and MESA. The models were mapped into the multidimensional domain several minutes before collapse and evolved until the onset of core collapse. We find that in extended oxygen-burning shells, turbulent velocities exceed the standard mixing-length-theory predictions by approximately a factor of two. In contrast, a thin silicon-burning shell is poorly described by MLT: mixing is reduced near both shell boundaries, and the inferred effective diffusion profile departs significantly from the standard one-dimensional prescription. We

What carries the argument

Three-dimensional magnetohydrodynamic evolution of mapped one-dimensional stellar models to measure deviations of convective velocities and effective diffusion from mixing-length theory in oxygen and silicon shells.

If this is right

  • Turbulent velocities in extended oxygen-burning shells exceed mixing-length theory predictions by a factor of approximately two.
  • Mixing in the thin silicon-burning shell is reduced near both boundaries and the effective diffusion profile departs from the standard one-dimensional prescription.
  • These differences directly change the spatial extent and efficiency of nuclear burning in the shells.
  • Updated prescriptions can be incorporated into one-dimensional stellar evolution codes to account for multidimensional effects in advanced phases.
  • The constructed models serve as physically consistent initial conditions for subsequent core-collapse and supernova explosion simulations.

Where Pith is reading between the lines

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

  • Incorporating these 3D progenitors into explosion calculations may produce different remnant masses or explosion energies than those obtained from purely one-dimensional initial conditions.
  • Revised mixing prescriptions could alter predicted nucleosynthesis yields from massive stars and the chemical enrichment of galaxies.
  • The results motivate attempts to extend similar 3D MHD simulations over longer evolutionary times to test whether the reported deviations persist or saturate.

Load-bearing premise

The one-dimensional stellar-evolution models from GENEC and MESA, when mapped into the 3D domain several minutes before collapse, provide initial conditions whose subsequent turbulent and nuclear evolution accurately represent real pre-supernova interiors without dominant numerical artifacts from the mapping or limited simulation duration.

What would settle it

A longer-duration simulation begun at an earlier evolutionary stage, or a remapping performed with a different numerical technique, that fails to recover the reported factor-of-two excess in oxygen-shell turbulent velocities would indicate the deviations are numerical rather than physical.

Figures

Figures reproduced from arXiv: 2605.22927 by Adam Griffiths, Martin Obergaulinger, Miguel-\'Angel Aloy.

Figure 1
Figure 1. Figure 1: Chemical structure for key species at mapping for [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Radial velocity profiles of the corrected (red) and non [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Angularly averaged turbulent radial Mach number, [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Power spectra of the spherical-harmonic decomposition [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Diffusion coefficients for convection in region C1 (left) and C2 (right) of M13. Estimation of the effective diffusion coef￾ficient using Eq. (17) (black), the standard MLT prediction (red), and the corrected MLT prescription of Eq. (19) (green). thin silicon-burning shell C1, the reconstructed profile exhibits a clear bell-like shape, with strongly reduced mixing at both shell boundaries relative to the s… view at source ↗
Figure 7
Figure 7. Figure 7: Total energy generation in the 3D models at di [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p010_9.png] view at source ↗
read the original abstract

The most energetic core-collapse supernovae are thought to arise from rapidly rotating, magnetised progenitors, yet the three-dimensional structure of their pre-collapse interior remains poorly constrained, and realistic distributions of magnetic fields, angular momentum, and convective asphericities are still lacking. We construct physically consistent three-dimensional pre-supernova progenitors including rotation and magnetic fields. In this first paper, we focus on the behaviour of turbulence and nuclear burning in the shells surrounding the stellar core, and assess their deviations from one-dimensional stellar-evolution models. We used Aenus-ALCAR to perform three-dimensional magnetohydrodynamic (MHD) simulations of two compact Wolf--Rayet progenitors obtained from the stellar evolution codes GENEC and MESA. The models were mapped into the multidimensional domain several minutes before collapse and evolved until the onset of core collapse. We find that in extended oxygen-burning shells, turbulent velocities exceed the standard mixing-length-theory (MLT) predictions by approximately a factor of two. In contrast, a thin silicon-burning shell is poorly described by MLT: mixing is reduced near both shell boundaries, and the inferred effective diffusion profile departs significantly from the standard one-dimensional prescription. These differences directly affect the spatial extent and efficiency of nuclear burning. We present the first 3D MHD pre-supernova progenitors of this kind, suitable for subsequent collapse and explosion calculations, and show that multidimensional effects can significantly modify turbulent mixing and shell burning during the final stages of massive-star evolution. We propose prescriptions to account for these effects in the advanced phases of stellar evolution.

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 paper presents the first 3D MHD simulations of two compact Wolf-Rayet pre-supernova progenitors obtained by mapping 1D GENEC and MESA models into the Aenus-ALCAR code several minutes before collapse and evolving them to core-collapse onset. It reports that turbulent velocities in extended oxygen-burning shells exceed standard MLT predictions by a factor of approximately two, while a thin silicon-burning shell exhibits reduced mixing near both boundaries with an effective diffusion profile that departs significantly from the 1D MLT prescription; these differences alter the spatial extent and efficiency of nuclear burning. The authors propose updated prescriptions for 1D stellar evolution codes and position the models as initial conditions for subsequent collapse and explosion calculations.

Significance. If the reported deviations from MLT are shown to be intrinsic rather than mapping artifacts, the work would supply the first 3D MHD pre-supernova progenitors with rotation and magnetic fields, directly constraining multidimensional effects on late-stage convection and burning. This would improve the fidelity of 1D pre-SN models used in supernova population synthesis and provide realistic initial conditions for core-collapse simulations. The direct numerical integration of the MHD equations on mapped initial conditions is a clear methodological strength.

major comments (2)
  1. [Abstract] Abstract and mapping description: the central claim that turbulent velocities exceed MLT by a factor of two and that the silicon-shell diffusion profile departs from the standard prescription requires that the several-minute post-mapping evolution has reached a statistically steady state. No resolution study, time-step convergence test, or mapping-time sensitivity run is referenced to bound the contribution of relaxation transients from the initially zero-velocity, spherically symmetric state.
  2. [Results (silicon shell)] Silicon-shell results: the reported reduction in near-boundary mixing and departure of the effective diffusion profile from MLT is load-bearing for the claim that multidimensional effects modify nuclear burning. Because silicon-burning timescales are short, any non-equilibrated profile measured at collapse onset could reflect the imposed 1D initial condition rather than intrinsic turbulence; the manuscript must demonstrate that the measured diffusion coefficient has converged with respect to both grid resolution and elapsed time after mapping.
minor comments (2)
  1. Notation for the effective diffusion coefficient should be defined explicitly when first introduced and kept consistent between text, figures, and the proposed 1D prescriptions.
  2. Figure captions for velocity and diffusion profiles should state the exact post-mapping time at which the snapshots are taken and whether they represent time averages.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed comments. The concerns about demonstrating statistical steady state after mapping from 1D models are well taken and directly relevant to the robustness of our central claims. We respond point by point below.

read point-by-point responses

  1. Referee: [Abstract] Abstract and mapping description: the central claim that turbulent velocities exceed MLT by a factor of two and that the silicon-shell diffusion profile departs from the standard prescription requires that the several-minute post-mapping evolution has reached a statistically steady state. No resolution study, time-step convergence test, or mapping-time sensitivity run is referenced to bound the contribution of relaxation transients from the initially zero-velocity, spherically symmetric state.

    Authors: We agree that explicit verification of statistical steady state is necessary to support the reported deviations from MLT. The several-minute post-mapping interval was selected to exceed multiple convective turnover times (estimated at ~100-200 s for the oxygen shell and shorter for silicon). In the revised manuscript we will add a dedicated subsection (or appendix) presenting time series of domain-integrated kinetic energy and shell-averaged turbulent velocities, showing that initial transients decay within the first ~60-90 s and that the reported velocity amplitudes and diffusion profiles are measured after this relaxation. We will also explicitly note the lack of dedicated resolution or mapping-time sensitivity experiments and discuss the associated caveats. revision: yes

  2. Referee: [Results (silicon shell)] Silicon-shell results: the reported reduction in near-boundary mixing and departure of the effective diffusion profile from MLT is load-bearing for the claim that multidimensional effects modify nuclear burning. Because silicon-burning timescales are short, any non-equilibrated profile measured at collapse onset could reflect the imposed 1D initial condition rather than intrinsic turbulence; the manuscript must demonstrate that the measured diffusion coefficient has converged with respect to both grid resolution and elapsed time after mapping.

    Authors: This point is valid and we acknowledge that the thin silicon shell is particularly sensitive to initial-condition transients. We will revise the relevant results section to include time-dependent profiles of the inferred effective diffusion coefficient in the silicon shell, demonstrating stabilization several minutes prior to collapse. Regarding grid resolution, the runs were performed at the highest resolution feasible for the 3D MHD setup; a formal resolution study was not conducted. In the revision we will add a limitations paragraph stating that the qualitative departure from MLT (reduced near-boundary mixing) is supported by the resolved flow morphology but that quantitative convergence with resolution remains to be demonstrated in future work. revision: partial

Circularity Check

0 steps flagged

No circularity: results from direct numerical integration of mapped initial conditions

full rationale

The paper reports outcomes of 3D MHD simulations evolved from mapped GENEC/MESA 1D profiles. Turbulent velocities, mixing profiles, and deviations from MLT are measured directly from the evolved fields; no parameter is fitted to a subset and then re-predicted, no self-citation supplies a uniqueness theorem or ansatz, and no equation reduces the reported quantities to the initial mapping by algebraic identity. The proposed prescriptions are post-hoc empirical fits to the simulation data, not load-bearing inputs. This is the standard non-circular case for a simulation study.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the assumption that 1D-to-3D mapping of GENEC/MESA models several minutes before collapse yields physically consistent initial conditions whose subsequent evolution is not dominated by mapping artifacts or insufficient simulation time.

axioms (1)
  • domain assumption The 1D stellar evolution models from GENEC and MESA provide accurate initial conditions for 3D mapping several minutes before collapse.
    Simulations begin from mapped 1D profiles; any error in those profiles propagates directly into the reported turbulent velocities and mixing profiles.

pith-pipeline@v0.9.0 · 5821 in / 1287 out tokens · 21299 ms · 2026-05-25T05:45:15.123578+00:00 · methodology

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Reference graph

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