Building three-dimensional giant stellar models for common envelope simulations

Israel); Noam Soker (Technion; Ron Schreier; Shlomi Hillel

REVIEW 2 major objections 299 references

Building three-dimensional giant stellar models for common envelope simulations

T0 review · 2 major / 0 minor · reviewed 2026-06-27 · grok-4.3

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Pith's one-line read Depositing stellar luminosity in an inner shell while cooling low-density outer cells produces stable pulsating 3D giant star models without any relaxation step.

desk verdict The paper gives a usable initialization recipe for 3D red supergiant models by mapping from 1D, adding inner luminosity deposition, cooling the outer low-density cells, and skipping relaxation. read the letter →

arxiv 2606.11927 v1 pith:LWBXKZZZ submitted 2026-06-10 astro-ph.SR

Ron Schreier , Shlomi Hillel , Noam Soker (Technion , Israel) This is my paper · ORCID

classification astro-ph.SR

keywords 3Dstellarmodelscommonenvelopeevolutionredsupergiantstarspulsationshydrodynamicsimulationsnumericalstructure

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper maps a one-dimensional red supergiant model onto a three-dimensional grid and tests ways to sustain its structure for common-envelope simulations. It deposits energy in an inner shell at the star's actual luminosity rate to stand in for nuclear burning and cools grid cells below photospheric density to stand in for surface emission. When both steps are used, the model develops sustained radial pulsations with a roughly one-year period plus non-radial modes and vigorous convection; without the outer cooling the oscillations decay. The authors conclude this combination prepares usable initial conditions more simply than traditional relaxation procedures.

What carries the argument

Inner-shell energy deposition at the stellar luminosity rate combined with cooling of low-density outer cells, which together replace nuclear burning and photospheric emission while letting the 3D model evolve its own pulsations.

What would settle it

A 3D simulation run lasting several dynamical times in which both inner-shell heating and outer cooling are applied, then checking whether the pulsation amplitude remains roughly constant or continues to grow instead of decaying.

Watch

Extended reading notes

Core claim

Transporting a 1D stellar model to a 3D grid, depositing energy at the stellar luminosity in an inner shell above the inert core, and cooling cells with densities below the photospheric value allows the model to execute its natural pulsations without relaxation. With both energy deposition and cooling active the oscillations do not decay and their amplitude slowly grows; the dominant period is about one year, comparable to the dynamical time, and the model also develops non-spherical structure, radius variations, and vigorous convection.

Load-bearing premise

That replacing nuclear burning with inner-shell energy input at the observed luminosity and replacing surface emission with cooling of low-density cells will reproduce the essential dynamical behavior of a real giant star on a 3D grid.

Editorial extensions

If this is right

The resulting model shows a dominant pulsation period of about one year that matches the stellar dynamical timescale.
Non-spherical density structure and slow changes in average radius appear, indicating superposed non-radial modes.
Vigorous convection develops naturally inside the model.
The same preparation can be used directly for grazing-envelope evolution simulations.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

This preparation might allow simulations to begin from a more realistic pulsating state rather than an artificially static one.
The sustained pulsations could influence the efficiency of envelope ejection during common-envelope interactions.
The approach might be tested on other giant-star masses or metallicities to check whether the same inner-shell plus outer-cooling recipe remains sufficient.

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Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

The main thing to know is that the authors describe a concrete way to set up 3D giant-star models for common-envelope work. They map a 1D stellar model onto a 3D grid, deposit energy at the stellar luminosity rate in an inner shell above the core, cool cells below photospheric density to stand in for radiation, and then evolve without any relaxation phase. The model is allowed to pulsate on its own.

What stands out is the direct comparison they run. Without the outer cooling, oscillations decay on a short timescale. With both inner deposition and outer cooling active, the oscillations persist or grow slowly, show a roughly one-year period close to the dynamical time, include non-radial components, and produce vigorous convection. That combination and the choice to skip relaxation is the practical contribution.

The work is straightforward and the reported behavior is internally consistent with the procedure they describe. It gives people running CEE simulations a clear starting point they can test.

The limitation is that the evidence stays qualitative. The abstract supplies no amplitude measurements, no resolution or parameter-sensitivity checks, and no direct comparison against relaxed models or other codes. The claim that this is the best preparation method therefore rests on the outcomes of their particular runs.

This is a methods paper aimed at researchers who need initial conditions for 3D hydro simulations of binary interactions. It is the sort of technical note that deserves referee time so the details can be checked and the approach can be tried by others.

Referee Report

2 major / 0 minor

Summary. The manuscript presents a procedure for constructing 3D red supergiant models from 1D stellar models for common-envelope evolution simulations. The approach maps the 1D structure to a 3D grid, deposits energy at the stellar luminosity rate in an inner shell above the inert core to mimic nuclear burning, and cools low-density cells to mimic photospheric emission, without any relaxation step. The authors report that oscillations decay in the absence of cooling, remain stable or grow slowly when both energy deposition and cooling are active, exhibit a dominant ~1 yr period consistent with the dynamical timescale (suggesting a fundamental radial mode), display non-radial modes via non-spherical structure and radius variations, and produce vigorous convection. They conclude that this combination is the optimal preparation method and that relaxation is unnecessary.

Significance. If validated, the method supplies a parameter-free initialization route that directly imports quantities from the input 1D model and permits natural pulsations and convection to emerge, potentially reducing computational overhead for CEE and grazing-envelope simulations. The absence of invented entities or fitted parameters in the core procedure is a clear strength.

major comments (2)

[Abstract] Abstract and results description: the statements that oscillations 'slowly decay', 'do not decay', or 'slowly increase' with time are presented without any quantitative metrics (e.g., e-folding times, amplitude growth rates, or time-series statistics of radius or kinetic energy), error estimates, or resolution studies. These quantitative diagnostics are load-bearing for the central claim that the combined inner-shell deposition plus low-density cooling produces sustained natural pulsations without relaxation.
[Abstract] Abstract and method description: no grid-resolution tests, convergence checks, or direct comparisons to 1D linear pulsation calculations or other 3D codes are reported to confirm that the ~1 yr period, non-radial mode content, and convection are physical rather than numerical artifacts. Such tests are required to substantiate the assertion that the procedure accurately represents essential stellar physics.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments on our manuscript. We address each major comment below and indicate the revisions we will make.

read point-by-point responses

Referee: [Abstract] Abstract and results description: the statements that oscillations 'slowly decay', 'do not decay', or 'slowly increase' with time are presented without any quantitative metrics (e.g., e-folding times, amplitude growth rates, or time-series statistics of radius or kinetic energy), error estimates, or resolution studies. These quantitative diagnostics are load-bearing for the central claim that the combined inner-shell deposition plus low-density cooling produces sustained natural pulsations without relaxation.

Authors: We agree that quantitative support would improve the abstract and results. In the revised manuscript we will add time-series statistics of the average stellar radius and total kinetic energy, together with estimates of e-folding times or growth rates extracted from the existing simulation data. These metrics will be described in the results section and briefly summarized in the abstract. revision: yes
Referee: [Abstract] Abstract and method description: no grid-resolution tests, convergence checks, or direct comparisons to 1D linear pulsation calculations or other 3D codes are reported to confirm that the ~1 yr period, non-radial mode content, and convection are physical rather than numerical artifacts. Such tests are required to substantiate the assertion that the procedure accurately represents essential stellar physics.

Authors: The manuscript demonstrates the initialization procedure and reports the emergent behavior from the simulations performed. We did not carry out resolution studies or comparisons to other codes. In revision we will add a limitations paragraph in the discussion noting the absence of these tests and reiterating that the dominant period is consistent with the dynamical timescale of the input 1D model. We maintain that the method's parameter-free character remains a useful contribution for CEE simulations, while acknowledging that further validation lies beyond the present scope. revision: partial

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity; procedure is self-contained numerical construction

full rationale

The paper presents a direct numerical method: map a 1D stellar model to a 3D grid, deposit energy in an inner shell at the input stellar luminosity rate, and cool low-density cells to mimic photospheric emission. Outcomes such as oscillation decay/growth, ~1 yr period matching dynamical time, non-radial modes, and convection are reported as simulation results, not used to define or fit the inputs. No equations reduce by construction to outputs, no fitted parameters are renamed as predictions, and no self-citations or uniqueness theorems are invoked as load-bearing. The central claim (this preparation method works without relaxation) rests on the described procedure's internal consistency with known stellar timescales, which is externally falsifiable via the reported behavior.

Assumptions & free parameters 0 free parameters · 3 assumptions · 0 invented entities

The central claim depends on the validity of three domain assumptions about physical mimicking and the suitability of the input 1D model; no free parameters are explicitly fitted in the abstract, and no new entities are postulated.

assumptions (3)

domain assumption A 1D stellar evolution model provides an accurate initial structure for a red supergiant that can be directly transported to a 3D grid.
The method begins by transporting a 1D model to the 3D numerical grid.
domain assumption Depositing energy at the stellar luminosity rate into an inner shell above the inert core accurately mimics core nuclear power production.
Used to mimic core nuclear power by depositing energy to an inner shell.
domain assumption Cooling grid cells with densities below the photospheric density accurately mimics stellar photospheric emission.
Used to mimic stellar emission by cooling grid cells with densities below the photospheric density.

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Cite this review

Pith. "Pith review of Building three-dimensional giant stellar models for common envelope simulations." pith.science (2026). https://pith.science/paper/LWBXKZZZ

@misc{pith2026260611927,
  author       = {Pith},
  title        = {Pith review of: Building three-dimensional giant stellar models for common envelope simulations},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/LWBXKZZZ}},
  note         = {Machine review of arXiv:2606.11927}
}

read the original abstract

We build a three-dimensional (3D) red supergiant (RSG) stellar model for common envelope evolution (CEE) simulations by transporting a 1D stellar model to a 3D numerical grid, mimicking core nuclear power by depositing energy to an inner shell, and mimicking stellar emission by cooling grid cells with densities below the photospheric density. We do not relax the model; rather, we let it perform its natural pulsation. We find that when we mimic photospheric emission by cooling low-density grid cells, the oscillations slowly decay on a time scale much longer than in the absence of photospheric cooling. When we mimic both nuclear energy production, by depositing the stellar luminosity in an inner shell above the inert core of the stellar model, and the photospheric cooling, the oscillations do not decay and their amplitude slowly increases with time. The main pulsational period is about 1 year, comparable to the stellar dynamical time, suggesting a fundamental radial pulsation mode. The non-spherical structure of the stellar model and rapid low-amplitude temporal variations in the average stellar radius testify to the presence of non-radial oscillation modes on top of the fundamental radial mode. We also obtain vigorous convection, as RSG stars have. We conclude that the best way of preparing a giant star to simulate CEE and grazing-envelope evolution is to deposit energy with the stellar luminosity in an inner shell, and to cool the outer low-density numerical shell. There is no need to relax the model.

Figures

Figures reproduced from arXiv: 2606.11927 by the authors.

**Figure 1.** Maps of the two tracers in the energy-deposition simulation starting in the inner shell 503R⊙ < r < 647R⊙ (Shell 1; left column), and in the outer shell 647R⊙ < r < 790R⊙ (Shell 2; right column) in the plane z = 0, at three times as indicated. We recall that we set a numerical spherical boundary at Rw = 100×1012 cm (Section 2); this is why the tracer does not expand beyond that radius [PITH_FULL_IMAGE:figures/full_… view at source ↗

**Figure 2.** The average radii of the tracers of two initial spherical shells: 35 × 1012 cm = 503R⊙ < r < 45 × 1012 cm = 647R⊙ and 45 × 1012 cm = 647R⊙ < r < 55 × 1012 cm = 790R⊙. Dashed lines are for the no-energy simulation, while solid lines are for the simulation with energy deposition. By t ≃ 3 yr, convection mixes the two shells almost completely, and the material that started in separate shells becomes indistinguishable. … view at source ↗

**Figure 3.** The kinetic (upper panel) and thermal energy (lower panel) of the two simulations inside two fixed shells: 35 × 1012 cm = 503R⊙ < r < 45 × 1012 cm = 647R⊙ and 45 × 1012 cm = 647R⊙ < r < 55 × 1012 cm = 790R⊙. The kinetic energy line of each simulation of the inner shell is above that of the outer shell because of the larger mass in the inner shell; the thermal energy line of the inner shell is much higher than that o… view at source ↗

Figures from the paper (2 more)

**Figure 4.** Figure 4: Velocity and density maps in the plane z = 0 for the energy-deposition simulation at four times as indicated. The four times of these panels are marked with red down-pointing arrows in [PITH_FULL_IMAGE:figures/full_fig_p007_4.png]

**Figure 5.** Figure 5: Density maps in the plane z = 0 for the No-energy-deposition simulation (left column) and the energy deposition simulation (right column), each at three times; note that times differ between the two simulations. We mark the times of these six panels in [PITH_FULL_IMAG…

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Pith tools

Reviewed June 27, 2026 · model on record in the stance chip above.

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SN 2006jc: A Wolf-Rayet Star Exploding in a Dense He-Rich Circumstellar Medium

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2022, MNRAS, 511, 176, doi: 10.1093/mnras/stab3776

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