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arxiv: 2606.22927 · v1 · pith:EBIDM6LHnew · submitted 2026-06-22 · 🌌 astro-ph.SR

Influence of mass transfer stability on the formation of post-common-envelope binaries

Yanxu Shi , Hongwei Ge , Zhenwei Li , Diogo Belloni , Rizhong Zheng , Dengkai Jiang , Hailiang Chen , A. Santos-Garcia
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Santiago Torres Gil Alberto Rebassa-Mansergas Xuefei Chen Zhanwen Han
This is my paper

Pith reviewed 2026-06-26 07:28 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords post-common-envelope binariesmass transfer stabilitycommon envelope evolutionbinary population synthesiswhite dwarf main sequence binariesmagnetic brakingbinary stellar evolution
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The pith

Enhanced mass transfer stability reduces the predicted number of post-common-envelope binaries with solar-type companions.

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

Standard binary population synthesis overpredicts post-common-envelope binaries that contain solar-type main-sequence stars. This work updates the Binary Star Evolution code with a physically motivated stability criterion for mass transfer and a self-consistent envelope binding energy. The updated models show that greater stability during mass transfer acts as an extra filter that removes many potential systems with solar-type companions. Magnetic braking and observational selection effects contribute but do not suffice on their own. Inefficient common-envelope evolution with efficiency parameter 0.25 produces the closest match to the compiled sample of observed systems.

Core claim

The enhanced mass transfer stability is an additional mechanism responsible for the observed dearth of post-common-envelope binaries with solar-type main sequence companions; neither magnetic braking nor selection effects alone can fully account for this deficit, and a combination of all three processes is most likely required. Models with inefficient common envelope evolution (α_CE=0.25) provide the best overall match to the observed population.

What carries the argument

Physically motivated mass transfer stability criterion in the Binary Star Evolution code, which decides whether mass transfer remains stable or triggers common-envelope evolution and thereby filters the predicted population.

If this is right

  • The observed population is best reproduced only when mass transfer stability, magnetic braking, and selection effects operate together.
  • Low common-envelope efficiency (α_CE = 0.25) yields the closest agreement with the compiled white-dwarf plus main-sequence sample.
  • Systems with M-dwarf companions remain largely unaffected by the change in stability criterion.
  • Traditional polytropic stability criteria systematically overproduce solar-type post-common-envelope binaries.

Where Pith is reading between the lines

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

  • The same stability criterion could alter predicted rates for other common-envelope outcomes such as double white dwarfs or Type Ia supernova progenitors.
  • Detailed stellar-structure calculations could test whether the adopted stability boundary shifts with metallicity or rotation.
  • Future Gaia or LSST samples of post-common-envelope binaries with precise masses and periods offer a direct test of the combined three-mechanism explanation.

Load-bearing premise

The mass transfer stability criterion used in the code accurately reflects the conditions under which real stars avoid common-envelope evolution.

What would settle it

A volume-complete survey that finds a substantially higher fraction of post-common-envelope binaries with solar-type companions than the updated models predict would falsify the claim that stability provides the missing reduction.

Figures

Figures reproduced from arXiv: 2606.22927 by Alberto Rebassa-Mansergas, A. Santos-Garcia, Dengkai Jiang, Diogo Belloni, Hailiang Chen, Hongwei Ge, Rizhong Zheng, Santiago Torres Gil, Xuefei Chen, Yanxu Shi, Zhanwen Han, Zhenwei Li.

Figure 1
Figure 1. Figure 1: The effect of critical mass ratio and CE descrip￾tion on the binary evolution and the formation of WD+MS PCEBs. Over the past two decades, significant advances in our understanding of CE evolution have been made through observational surveys of PCEBs (M. Zorotovic et al. 2011; A. Nebot G´omez-Mor´an et al. 2011; S. Toonen & G. Nelemans 2013; J. Camacho et al. 2014; R. Cojo￾caru et al. 2017; N. Yamaguchi et… view at source ↗
Figure 2
Figure 2. Figure 2: Critical mass ratio adopted in our simulations, plotted on the stellar mass-radius diagram. Black and white dashed lines represent the radii of ZAMS stars and the minimum radii of RGB at different masses, respectively. Note that not all regions shown are physically valid, as the AGB boundary is not plotted here. white dwarfs. We therefore adopt corrected white dwarf masses for these affected systems in thi… view at source ↗
Figure 3
Figure 3. Figure 3: Initial primary versus initial secondary mass dis￾tribution of PCEB progenitors. Points are color-coded by the final WD type: red for He WDs, blue for carbon-oxygen (C/O) WDs, and green for oxygen-neon (O/Ne) WDs. Dark points in the foreground correspond to the Ge et al. qc pre￾scription (model a), and are overlaid on top of lighter points representing the polytropic qc prescription (model d). The grey das… view at source ↗
Figure 4
Figure 4. Figure 4: Distribution of observed (pink dots) and simulated PCEBs in the MWD − MMS plane. The point color encodes the local number density of simulated PCEBs, normalized independently to the maximum density in each panel for visual clarity. Peak-normalized marginal histograms are shown at the top (MWD) and right (MMS), where grey lines represent the observed distributions, red represents the simulated MWD distribut… view at source ↗
Figure 5
Figure 5. Figure 5: Distribution of observed (pink dots) and simulated PCEBs in the MMS − Porb plane. The color intensity scale is identical to [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Distribution of observed (pink dots) and simulated PCEBs in the MWD − Porb plane. The color intensity scale is identical to Figures 4 and 5. tional torque are the largest convective cells; when the difference between Ω and Ωeq is too large, these cells can [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Distribution of observed (pink dots) and simulated PCEBs using the CARB MB prescription, plotted in the MWD − MMS, MMS − Porb, and MWD − Porb planes. The color scheme is identical to [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Our compiled PCEB sample and long-period WD+MS binaries from (E. Kruse & E. Agol 2014; H. Kawahara et al. 2018; N. Yamaguchi et al. 2024a) plotted in the MWD − Porb plane (adapted from N. Yamaguchi et al. 2024a and S. G. Parsons et al. 2023). The point color encodes the mass of the MS companion in each system. We mark the position of the well-known PCEB IK Peg for reference. The dashed line and grey region… view at source ↗
Figure 9
Figure 9. Figure 9: Distribution of observed (pink dots, classic PCEBs and long-period WD+MS binaries) and simulated PCEBs adopting half of internal energy contribution, plotted in the MWD − MMS, MMS − Porb, and MWD − Porb planes. The αCE is set to 0.25. The color scheme is identical to [PITH_FULL_IMAGE:figures/full_fig_p014_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Distribution of observed (pink dots) and simu￾lated PCEBs in the MWD −MMS plane. We exclude systems discovered via UV excess from this plot, as they are sub￾ject to totally different selection effects. The color scheme is identical to [PITH_FULL_IMAGE:figures/full_fig_p015_10.png] view at source ↗
read the original abstract

Post-common-envelope binaries are the natural laboratories for constraining the physics of common envelope evolution, which is one of the most uncertain phases in binary stellar evolution. Traditional binary population synthesis models, adopting mass transfer stability criteria based on polytropic stellar models, systematically overpredict the number of post-common-envelope binaries with solar-type main-sequence companions. In this work, we present an updated binary population synthesis model using the rapid binary evolution code \textit{Binary Star Evolution}, incorporating a physically motivated mass transfer stability criterion and a self-consistent envelope binding energy prescription. We compile a comprehensive sample of classic white dwarf + main sequence post-common-envelope binaries with well-measured parameters, hosting both M-dwarf and A/F/G/K- stars. We find that the enhanced mass transfer stability is an additional mechanism responsible for the observed dearth of post-common-envelope binaries with solar-type main sequence companions; neither magnetic braking nor selection effects alone can fully account for this deficit, and a combination of all three processes is most likely required. Models with inefficient common envelope evolution ($\alpha_{\rm CE}=0.25$) provide the best overall match to the observed population. These results highlight the critical role of MT stability in shaping the observed post-common-envelope binaries population and provide new constraints on common envelope 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 / 1 minor

Summary. The paper claims that an updated BSE population synthesis model incorporating a physically motivated mass transfer stability criterion (replacing the polytropic one) and a self-consistent envelope binding energy prescription shows that enhanced MT stability is an additional mechanism (beyond magnetic braking and selection effects) responsible for the observed dearth of post-common-envelope binaries with solar-type main-sequence companions; models with α_CE=0.25 provide the best overall match to a compiled sample of WD+MS PCEBs.

Significance. If the new stability criterion is shown to be accurate, the work would strengthen the case that mass transfer stability shapes the PCEB population and provide useful constraints on common-envelope efficiency. The compilation of an observational sample with both M-dwarf and A/F/G/K companions is a positive contribution.

major comments (2)
  1. [Abstract and §2] Abstract and model description: the claim that the new criterion explains part of the dearth relies on the assumption that it correctly identifies the stable-MT/CE boundary for ~1 M⊙ donors, but the manuscript supplies no validation against detailed stellar models or hydrodynamical calculations; without this, the population synthesis result could be an artifact of the criterion rather than a physical explanation.
  2. [Results (comparison to observations)] Results section comparing models to the compiled sample: α_CE=0.25 is selected because it yields the best overall match; this makes the central assertion that the combination of the stability criterion plus this specific efficiency reproduces the data circular rather than an independent prediction.
minor comments (1)
  1. [Abstract] The abstract would benefit from including at least one quantitative metric (e.g., a goodness-of-fit value or ratio of predicted-to-observed numbers) rather than stating only that the model provides the 'best overall match'.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the detailed and constructive report. We address each major comment below. Revisions have been made to clarify the physical basis of the stability criterion, add discussion of its limitations, and distinguish the independent role of the new criterion from the choice of α_CE. These changes strengthen the manuscript without altering its core conclusions.

read point-by-point responses

  1. Referee: [Abstract and §2] Abstract and model description: the claim that the new criterion explains part of the dearth relies on the assumption that it correctly identifies the stable-MT/CE boundary for ~1 M⊙ donors, but the manuscript supplies no validation against detailed stellar models or hydrodynamical calculations; without this, the population synthesis result could be an artifact of the criterion rather than a physical explanation.

    Authors: We agree that direct validation against detailed stellar models or hydrodynamical simulations for the ~1 M⊙ regime is not presented in the current manuscript. The criterion is physically motivated by the response of the stellar structure to mass loss (as described in §2), but we acknowledge this leaves open the possibility of systematic bias. In the revised manuscript we have added a dedicated paragraph in §2 that (i) summarizes the derivation from the adiabatic response and (ii) cites existing comparisons in the literature between similar stability criteria and both 1D stellar models and limited hydrodynamical work. We also explicitly state the assumption and its uncertainty so that readers can assess the robustness of the population-synthesis results. revision: partial

  2. Referee: [Results (comparison to observations)] Results section comparing models to the compiled sample: α_CE=0.25 is selected because it yields the best overall match; this makes the central assertion that the combination of the stability criterion plus this specific efficiency reproduces the data circular rather than an independent prediction.

    Authors: The stability criterion itself is independent of α_CE; it is fixed by the donor response and is applied before any common-envelope phase is invoked. The main result—that enhanced stability reduces the predicted number of solar-type PCEBs—is present for all tested values of α_CE. We select α_CE=0.25 only as the value that simultaneously reproduces the observed period and mass-ratio distributions once the new stability boundary is adopted. In the revised text we have rephrased the abstract and §4 to emphasize that the stability effect operates across the α_CE range and that the low-efficiency value is a secondary constraint, not a prerequisite for the stability conclusion. This removes any appearance of circularity. revision: partial

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The paper implements an updated mass transfer stability criterion in the BSE code, compiles an observed PCEB sample, and compares population synthesis outputs for different α_CE values against that external sample. The statement that α_CE=0.25 provides the best match is the direct result of running the models and inspecting the match to data, not a self-referential definition or a fitted input relabeled as a prediction. The central claim that enhanced MT stability contributes to the observed dearth rests on the new criterion's effect on the synthesized population and is independent of the α_CE tuning step. No load-bearing derivation step reduces to its own inputs by construction; the work is a standard parameter study benchmarked against observations.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim rests on the accuracy of the new mass-transfer stability criterion (whose derivation is not shown), the assumption that the compiled observational sample is unbiased, and the choice of alpha_CE fitted to the same data used for validation.

free parameters (1)
  • alpha_CE = 0.25
    Value selected because models with alpha_CE=0.25 provide the best overall match to the observed PCEB population.
axioms (2)
  • domain assumption Polytropic stellar models yield inaccurate mass-transfer stability criteria for solar-type stars in binaries.
    Invoked to explain why traditional models overpredict the number of PCEBs with solar-type companions.
  • domain assumption The updated mass-transfer stability criterion implemented in BSE is physically motivated and more accurate than polytropic prescriptions.
    Central modeling choice whose validity is required for the conclusion that stability is an additional mechanism.

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discussion (0)

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