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arxiv: 2606.13567 · v1 · pith:MI5XZVOFnew · submitted 2026-06-11 · 🌌 astro-ph.SR

The effect of near-core mixing on rejuvenation and the asteroseismic properties of massive accretors

Jan Henneco , Dominic M. Bowman This is my paper

Pith reviewed 2026-06-27 05:32 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords asteroseismologymassive starsbinary mass transferconvective boundary mixingsemiconvectionperiod spacing patternsstellar rejuvenation
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The pith

Convective boundary mixing, not semiconvection, sets the asteroseismic imprint of mass accretion in massive stars.

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

This paper uses one-dimensional stellar models to test how mixing near the cores of massive stars that gained mass in binaries shapes their internal structure and pulsation signals. It finds that the seismic signature recovered from period spacing patterns stays largely the same when semiconvective mixing efficiency is varied, yet shifts sharply once convective boundary mixing is removed. The post-accretion thermal relaxation phase emerges as the process that fixes the final near-core structure and therefore the observable imprint. The work shows that Fourier transforms of those spacing patterns can separate the effects of different mixing choices and accretion rates.

Core claim

The central claim is that the asteroseismic imprint of accretion is robust against changes in semiconvective mixing efficiency but changes drastically when convective boundary mixing is omitted. Post-accretion thermal relaxation determines the final near-core structure and the resulting seismic signal. Fourier transforms of period spacing patterns quantify how different near-core mixing and accretion-rate assumptions affect the signals.

What carries the argument

Near-core mixing region outside convective cores, controlled by convective boundary mixing and post-accretion thermal relaxation, which determines the shape of period spacing patterns.

If this is right

  • Semiconvective mixing efficiency variations leave the recovered seismic imprint of accretion largely unchanged.
  • Absence of convective boundary mixing produces markedly different asteroseismic properties after accretion.
  • Thermal relaxation after mass transfer fixes the near-core structure that asteroseismology later probes.
  • Fourier analysis of period spacing patterns can distinguish mixing and accretion-rate scenarios in observations.

Where Pith is reading between the lines

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

  • Binary evolution calculations that omit convective boundary mixing may systematically misestimate the ages and core structures of accreted stars.
  • Multi-dimensional simulations of the post-accretion phase could test whether the 1D thermal relaxation picture holds.
  • Targeted asteroseismic surveys of known post-mass-transfer binaries could place empirical bounds on accretion rates once boundary mixing is included.

Load-bearing premise

One-dimensional stellar evolution models with the chosen mixing and accretion prescriptions accurately capture the near-core structure and thermal relaxation that occur in real mass-accreting stars.

What would settle it

A confirmed mass-accreting star whose observed period spacing pattern matches the predictions of models that omit convective boundary mixing would contradict the claim that boundary mixing dominates the imprint.

Figures

Figures reproduced from arXiv: 2606.13567 by Dominic M. Bowman, Jan Henneco.

Figure 1
Figure 1. Figure 1: Kippenhahn diagrams of the near-core region for a 3.0 + 0.5 M⊙ accretor star with different values of semiconvective mixing efficiency, 𝛼sc. ‘Schw.’ stands for ‘Schwarzschild’ and indicates the only model that uses the Schwarzschild criterion for convection instead of the Ledoux criterion. Each Kippenhahn diagram is shown from the onset of mass transfer at 𝑡 = 161.62 Myr until roughly one global thermal ti… view at source ↗
Figure 2
Figure 2. Figure 2: Central hydrogen mass fraction, 𝑋c, evolution in time, shown between the onset of mass transfer until one global thermal timescale of the accretors with overshooting after the end of mass transfer. The model from Wagg et al. (2024) with 𝛼sc = 0.1 is shown in black. The solid black vertical line indicates the end of mass transfer. This CBM-driven rejuvenation can also be seen in the model from Miszuda et al… view at source ↗
Figure 3
Figure 3. Figure 3: Period spacing patterns (PSPs) for dipole zonal (ℓ = 𝑙, 𝑚 = 0) gravity modes without rotation for the 3.5 M⊙ accretor models (solid blue lines) at 𝑋c = 0.30 with different values of 𝛼sc and the model using the Schwarzschild criterion for convection. The solid orange lines represent the PSPs for the equivalent single-star models of mass 𝑀s . The dashed blue and orange lines show the asymptotic period spacin… view at source ↗
Figure 4
Figure 4. Figure 4: Brunt-Väisälä frequency 𝑁˜ profiles (solid blue and dashed orange lines for the accretor and single star, respectively, left y-axis) and Fourier transforms (light blue and gold lines for the accretor and single star, respec￾tively, right y-axis) of the corresponding normalised PSPs for accretors and equivalent single stars as a function of the buoyancy coordinate 𝑢(𝑟 ) for dif￾ferent 𝛼sc at 𝑋c = 0.30. The … view at source ↗
Figure 5
Figure 5. Figure 5: Hydrogen mass fraction 𝑋 (Panel a), BV frequency 𝑁˜ profile (Panel b), and Kippenhahn diagram (Panel c) for the 𝛼sc = 0.1 accretor model at different times. Each panel only shows the near-core region and contains information from right before the onset of mass transfer until roughly the mid-main sequence of the rejuvenated accretor. The Kippenhahn diagram uses the MESA model number for its x-axis for clari… view at source ↗
Figure 6
Figure 6. Figure 6: Same as [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Same as [PITH_FULL_IMAGE:figures/full_fig_p012_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Same as [PITH_FULL_IMAGE:figures/full_fig_p013_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Same as [PITH_FULL_IMAGE:figures/full_fig_p013_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Same as [PITH_FULL_IMAGE:figures/full_fig_p014_10.png] view at source ↗
read the original abstract

The relatively recent revelation of the high occurrence rate of binary interactions, especially in intermediate- and high-mass systems, has prompted multiple investigations into their asteroseismic imprints. The near-core region just outside the convective cores of mass-accreting early-type main-sequence stars in binaries has been theorised to be sensitive to assumptions about mixing (notably semiconvection) and accretion physics. In turn, the predicted asteroseismic properties depend strongly on the physical properties of this near-core region. We explore how robust the previously identified asteroseismic imprints of mass accretion are to changes in semiconvective mixing. Using one-dimensional stellar structure and evolution models, this parameter study shows the dominant effect of convective boundary mixing on rejuvenation and the post-accretion asteroseismic properties. The recovered seismic imprint, largely robust to variations in semiconvective mixing efficiency, changes drastically when convective boundary mixing is not included in the models. We find that the post-accretion thermal relaxation is key in determining the final near-core structure and the asteroseismic imprint of accretion. We reaffirm the potential of Fourier transforms of period spacing patterns to quantify the effects of different near-core mixing and accretion-rate assumptions on asteroseismic signals. Overall, this work highlights the sensitivity of the asteroseismic imprint of accretion not only on stellar structure and evolution modelling assumptions, but also on the accretion physics. The logical next step is to arrive at a more general picture of the asteroseismic imprint of mass transfer by exploring its properties in a multi-dimensional parameter study including single- and binary-star assumptions.

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 conducts a parameter study with one-dimensional stellar evolution models to assess the impact of near-core mixing (semiconvective efficiency and convective boundary mixing) on rejuvenation and asteroseismic properties of massive main-sequence accretors in binaries. It reports that the asteroseismic imprint is largely robust to variations in semiconvective mixing efficiency but changes drastically in the absence of convective boundary mixing, attributes this to the role of post-accretion thermal relaxation in setting the final near-core structure, and reaffirms the utility of Fourier transforms of period spacing patterns as a diagnostic while calling for future multi-dimensional explorations.

Significance. If the modeled trends hold, the work isolates convective boundary mixing as the dominant control on post-accretion near-core profiles and asteroseismic signals, providing concrete guidance for interpreting g-mode pulsations in binary products. The explicit parameter variation and emphasis on thermal relaxation timescales constitute a clear, falsifiable contribution within the 1D framework; the methodological suggestion regarding Fourier analysis of period spacings is a reusable diagnostic strength.

major comments (2)
  1. [Abstract and parameter-study results section] Abstract and the parameter-study results section: the central claim that the seismic imprint 'changes drastically' without convective boundary mixing is load-bearing for the conclusion that CBM dominates over semiconvection. No quantitative metric (e.g., shift in the dominant Fourier frequency, change in peak amplitude, or fractional change in the period-spacing slope) is supplied to substantiate the adverb 'drastically,' preventing assessment of whether the effect exceeds the numerical or physical uncertainties of the 1D implementation.
  2. [post-accretion thermal relaxation section] The section discussing post-accretion thermal relaxation: the assertion that thermal relaxation is 'key' in determining the final near-core structure rests on the 1D model's treatment of the thermal adjustment timescale. No explicit comparison is shown between the relaxation timescale with and without CBM, nor is a test provided against the expected multi-dimensional flow timescales, leaving open whether the reported sensitivity is an artifact of the chosen 1D mixing-length and boundary prescriptions.
minor comments (2)
  1. [Methods section] Methods section: the definitions and numerical values adopted for the semiconvective mixing efficiency and the CBM diffusion coefficient should be tabulated for each model sequence to allow direct reproduction.
  2. [Figure captions] Figure captions: captions for the period-spacing and Fourier-transform figures should list the exact accretion rate, initial mass, and mixing parameters used in each panel rather than referring only to 'standard' or 'no-CBM' cases.

Simulated Author's Rebuttal

2 responses · 1 unresolved

We thank the referee for the constructive comments on our manuscript. We respond point-by-point to the major comments below, indicating planned revisions where appropriate.

read point-by-point responses

  1. Referee: [Abstract and parameter-study results section] Abstract and the parameter-study results section: the central claim that the seismic imprint 'changes drastically' without convective boundary mixing is load-bearing for the conclusion that CBM dominates over semiconvection. No quantitative metric (e.g., shift in the dominant Fourier frequency, change in peak amplitude, or fractional change in the period-spacing slope) is supplied to substantiate the adverb 'drastically,' preventing assessment of whether the effect exceeds the numerical or physical uncertainties of the 1D implementation.

    Authors: We agree that the adverb 'drastically' would benefit from quantitative support to allow readers to judge its magnitude relative to model uncertainties. In the revised manuscript we will add explicit metrics, including the shift in the dominant Fourier frequency of the period-spacing pattern and the fractional change in the period-spacing slope, for the cases with and without convective boundary mixing. These will be reported in the parameter-study results section alongside the existing figures. revision: yes

  2. Referee: [post-accretion thermal relaxation section] The section discussing post-accretion thermal relaxation: the assertion that thermal relaxation is 'key' in determining the final near-core structure rests on the 1D model's treatment of the thermal adjustment timescale. No explicit comparison is shown between the relaxation timescale with and without CBM, nor is a test provided against the expected multi-dimensional flow timescales, leaving open whether the reported sensitivity is an artifact of the chosen 1D mixing-length and boundary prescriptions.

    Authors: We will add explicit comparisons of the post-accretion thermal relaxation timescales between models that include and exclude convective boundary mixing, derived directly from the 1D evolutionary sequences. A quantitative test against multi-dimensional flow timescales lies outside the scope of the present 1D study; the manuscript already identifies multi-dimensional explorations as the logical next step. revision: partial

standing simulated objections not resolved
  • Direct comparison of 1D thermal relaxation timescales against multi-dimensional hydrodynamic simulations.

Circularity Check

0 steps flagged

No circularity: results from direct parameter variation in 1D models

full rationale

The paper performs a numerical parameter study in one-dimensional stellar evolution models, varying semiconvective mixing efficiency and the inclusion of convective boundary mixing to observe effects on rejuvenation, near-core structure, and asteroseismic properties. All load-bearing claims (robustness to semiconvection, drastic change without boundary mixing, role of post-accretion thermal relaxation) are direct outputs of these simulations rather than reductions of any equation or fitted parameter to itself. No self-citations are invoked as load-bearing uniqueness theorems or ansatzes; the work explicitly builds on prior identifications but derives its new findings from the present model grid. The derivation chain is therefore self-contained against the stated modeling assumptions.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard 1D stellar structure assumptions and the numerical implementation of mixing processes; no new entities postulated.

free parameters (2)
  • semiconvective mixing efficiency
    Varied in the parameter study to test robustness of the seismic imprint.
  • convective boundary mixing inclusion
    Tested with and without to demonstrate dominant effect on rejuvenation and asteroseismic properties.
axioms (2)
  • domain assumption One-dimensional stellar structure and evolution equations accurately represent near-core mixing and thermal relaxation in main-sequence accretors
    Invoked by reliance on 1D models for all simulations.
  • domain assumption Accretion can be parameterized with specific rates and physics that affect post-accretion structure
    The abstract notes sensitivity of results to accretion physics assumptions.

pith-pipeline@v0.9.1-grok · 5822 in / 1364 out tokens · 40106 ms · 2026-06-27T05:32:58.938104+00:00 · methodology

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