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Binary stars take what they get: Evidence for Efficient Mass Transfer from Stripped Stars with Rapidly Rotating Companions

T0 review · 3 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read Mass transfer in Be+sdOB binaries is mostly conservative: half of the systems require at least 50 percent accretion efficiency, contradicting standard binary models.

desk verdict First multi-system lower bounds on mass transfer efficiency in Be+sdOB binaries; the rotationally-limited result is robust, but the 'half >50%' headline rests on the best-guess stripped-mass relation and needs a qualifier. read the letter →

arxiv 2505.14780 v2 pith:OFAZEQCG submitted 2025-05-20 astro-ph.SR astro-ph.HE

Thibault Lechien , Selma E. de Mink , Ruggero Valli , Amanda C. Rubio , Lieke A. C. van Son , Robert Klement , Harim Jin , Onno Pols This is my paper · ORCID
classification astro-ph.SRastro-ph.HE
keywords BinarystarsStellaraccretionRochelobeoverflowBeSubdwarfevolutionarymodelsMasstransferefficiency
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

This paper uses a new sample of 16 Be+sdOB binaries—pairs where a rapidly spinning Be star orbits a stripped hot subdwarf—to measure how much mass the Be star actually kept when its companion transferred mass to it. The authors argue that mass transfer in these systems was predominantly efficient: about half of the sample requires that at least 50 percent of the transferred mass was retained by the accretor, and several systems require considerably more. If true, this contradicts the widely used rotationally limited accretion prescription in detailed binary evolution codes, which predicts that only a few percent can be accreted once the gainer spins up, and it also strains thermally limited prescriptions used in population synthesis. The result matters because the mass transfer efficiency sets the final masses and orbits of almost all interacting binary products, from white dwarfs and blue stragglers to X-ray binaries and gravitational-wave sources.

What carries the argument

The load-bearing object is the initial-mass–stripped-mass relation: a mapping from a star's zero-age main-sequence mass to the helium-core mass it has when hydrogen-shell burning begins, computed from a grid of single-star models and used as a lower bound on the final stripped-star mass, with a plus-20-percent variant as a best guess. Combined with the evolutionary constraint that the donor must have started out more massive than the accretor, it yields analytical expressions for the minimum mass transfer efficiency $\beta_{\min}$ as a function of the two observed masses. This relation converts a static snapshot—present-day masses of the Be star and the subdwarf—into a statement about the integrated history of mass transfer.

What would settle it

A volume-limited survey of Be+sdOB binaries that fills the currently empty lower-right region of the accretor-mass versus stripped-mass diagram with systems whose inferred efficiencies fall below 0.3 would contradict the claim that mass transfer is predominantly conservative; the present sample's emptiness in that region is suggestive, but a selection-corrected census could turn it into a decisive test.

Watch

Extended reading notes

Core claim

The central claim is that stable Case B mass transfer in binaries with initial donor masses of 2 to 9 solar masses is largely conservative, with the accretor keeping more than half of the donated mass in many systems. The argument works by treating each present-day hot subdwarf as the helium core of the original donor: a calibrated initial-mass–stripped-mass relation gives the donor's initial mass, and the requirement that the donor was initially the more massive star gives a lower bound on how much mass the Be star must have gained. Applying this to the 16 systems, the authors find that 4 of the 14 non-Case-A systems require efficiencies above 50 percent even under strict lower-limit assumptions, and that the sample as a whole is incompatible with rotationally limited accretion, which allows only a few percent. They further argue that a thermally limited model is consistent only if nearly all systems originate from a narrow 10 percent sliver of initial parameter space, which they deem unlikely.

Load-bearing premise

The whole calculation assumes that the present-day mass of the stripped subdwarf maps uniquely to the donor's initial mass through a stellar-evolution relation; if the true stripped mass is lower than the adopted helium-core mass, the inferred donor mass, donated mass, and minimum efficiency all shrink.

Editorial extensions

If this is right

  • Rotationally limited accretion as implemented in detailed binary evolution codes cannot reproduce the sample; the inferred lower bounds require far more accretion than those models allow.
  • Rapid population synthesis codes using thermally limited accretion face tension: the observed systems would have to be drawn from a narrow band covering about 10 percent of the stable mass transfer parameter space.
  • A constant mass transfer efficiency of 60 to 80 percent can explain the whole sample, suggesting that simple fixed-efficiency prescriptions may be closer to reality than spin-up-based limits.
  • The empty lower-right region of the mass diagram may indicate that systems with very low mass transfer efficiency are rare or do not survive stable mass transfer, though the sample selection is not homogeneous enough to be conclusive.
  • If the same efficiency applies to higher-mass binaries, predictions for supernova types, X-ray binaries, and gravitational-wave merger rates would shift toward heavier and more widely separated remnants.

Reading between the lines

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

  • A natural test is to measure projected rotation velocities of the Be accretors: efficient disk accretion that still removes angular momentum should leave many accretors rotating below critical speed, which can be checked against the observed distribution.
  • Extending the same analysis to Be X-ray binaries, whose progenitors pass through the same channel above 10 solar masses, would test whether conservative mass transfer persists at higher masses.
  • The empty lower-right corner of the mass diagram could be a selection effect or a real absence; a volume-limited, bias-corrected census of Be+sdOB binaries would distinguish these and would double as a direct falsification test of the paper's main claim.
  • The closed-form $\beta_{\min}$ formulas could be applied as a fast observational prior in future binary population synthesis, so that each newly measured Be+sdOB system immediately updates the inferred accretion efficiency distribution.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. This paper compiles a sample of 16 Be+sdOB binaries with mass determinations of both components, and uses the relation between the present-day stripped-star mass and the initial donor mass (from MESA models) to derive lower limits on the mass transfer efficiency beta. The central result is that mass transfer in these systems must often have been highly efficient: more than a quarter of the 14 systems relevant to early Case B require beta_min > 0.5 under a strict lower-limit stripped-mass relation, and about half do so under a best-guess relation that includes a residual envelope. The authors argue that these constraints are inconsistent with rotationally limited accretion and in tension with a thermally limited accretion scheme as implemented in rapid population-synthesis codes.

Significance. If the result holds, it is a significant observational constraint on mass transfer efficiency in intermediate-mass (2-9 Msun) binaries, directly challenging widely used prescriptions in binary evolution and population synthesis. The paper's method is clean: beta_min follows from observed masses, an independent MESA initial-mass--stripped-mass relation, and the evolutionary constraint that the donor was initially more massive than the accretor; it does not fit beta to the data. The authors are transparent about the sample's heterogeneous quality, provide analytical fitting formulas (Eqs. B3 and B4), and make their MESA inlists and history files publicly available on Zenodo. The main weakness is that the headline quantitative claim ('half of the systems') is sensitive to the assumed stripped-mass relation and to the adopted overshooting prescription, and this sensitivity is not fully quantified in the abstract and conclusions.

major comments (3)
  1. [Abstract and Section 3, Eqs. (B1)-(B2)] The abstract states 'half of the systems require mass transfer efficiencies above 50%' without qualification, but this number comes from the best-guess relation (2), which adds 20% residual envelope mass. Under the strict lower-limit relation (1), the count is 4 of 14 (Section 3, first bullet), not 7 of 14. The conclusion does say 'using our best-guess estimates,' but the abstract does not. Since the central headline depends on this assumption, the abstract should either state the strict-lower-limit count or explicitly attribute the 50% figure to the best-guess relation.
  2. [Appendix B, Section 4, and Fig. 5] The claim that relation (1) is a 'strict lower limit' to the stripped mass is conditional on the adopted overshooting prescription. The paper's single-star grid uses a mass-dependent overshooting calibrated by Castro et al. (2014) and Brott et al. (2011), while the Temmink et al. (2023) grid uses the Choi et al. (2016) M67 calibration, which gives smaller cores at low masses. If a lower-overshooting relation is appropriate, the inferred initial donor mass for a given observed MsdOB would be larger, and beta_min would be smaller (Section 2, Eqs. B3-B4). The paper mentions this dependence in Section 4 but does not quantify how many systems would fall below the beta_min = 0.5 threshold. Please provide a sensitivity test using a lower-overshooting initial-mass--stripped-mass relation, or otherwise justify why the adopted prescription yields a conservative (lower) bound on beta.
  3. [Section 3 and Table 1, HR 2142 and HR 6819] The analysis excludes HR 2142 and HR 6819 as likely Case A systems, but for HR 2142 the main result adopts the orbital mass of 17.6 Msun for the Be star, while a separate spectral fit (BeAtlas, Rubio et al. 2023) yields about 9.6 Msun and a companion mass of about 0.7 Msun, which would give beta_min = 0.85 and a Case-B-consistent initial period (Section 4). The paper acknowledges this but does not explicitly state how the sample-level conclusions change if HR 2142 is included under the alternative mass. Since the sample is small and the 'half of systems' statement is a count, this systematic uncertainty in one system should be made explicit in the results, not only in the discussion.
minor comments (5)
  1. [Section 3, bullet list] The robustness bullet 'Even when pessimistically considering the 1-sigma uncertainties, we still find at least 4 systems with evidence for modest accretion (beta_min > 0.15)' uses a threshold of 0.15, which is much lower than the headline threshold of 0.5; reporting the 1-sigma range for the number of systems with beta_min > 0.5 would be more directly relevant to the central claim.
  2. [Section 3, fourth paragraph] The probability 'of the order of 10^-10' that ten systems lie in the narrow consistent region of the thermally limited model is stated without derivation; please specify how it was computed (e.g., from the fractional area of the initial parameter space that is consistent) and note that it is an order-of-magnitude estimate.
  3. [Fig. 2 caption and Appendix B] The top axis of Fig. 2 is labeled 'Initial mass of the stripped star'; this is the inferred initial mass of the donor, and the label should be consistent with the text (e.g., 'Initial donor mass') to avoid confusion.
  4. [Throughout, e.g., Fig. 4 and Appendix C] The term 'CASE A' is capitalized inconsistently; use 'Case A' to match standard nomenclature.
  5. [Appendix C, Section C.1] For the Kendall rank correlation results, reporting the tau values and p-values would help the reader judge the significance; the text only says 'strong' or 'moderate but still significant.'

Circularity Check

1 steps flagged · score 2.0 of 10

Strict-lower-bound beta analysis is self-contained; only the headline 'half' count leans on the authors' own +20% residual-envelope relation.

  1. ansatz smuggled in via citation [Appendix B (Eq. B2, Figure 5); Section 5 Conclusion item 1]
    "We also analyze our systems using the relation shown as a dashed line (2), which considers an added 20% of the mass remaining. It does not provide a strict lower bound, but we consider this our best guess. ... As the paper detailing the binary grid models is forthcoming (Jin et al. in prep), we briefly summarize their key assumptions here."

    The headline that 'half of the systems require mass transfer efficiencies above 50%' is obtained with Eq. B2, not with the paper's primary strict lower bound Eq. B1. Eq. B2 is Eq. B1 augmented by an ad hoc +20% residual envelope whose justification is the authors' own binary grids, one of which is a forthcoming co-authored paper (Jin et al., in prep). Using the strict relation B1 reduces the count from 7 to 4 of 14 systems, changing 'half' to 'more than a quarter'. Thus the strong headline number is an input assumption imported from in-group models, not an independent prediction. The strict-lower-bound analysis remains self-contained and non-circular.

full rationale

The derivation of beta_min is not circular: it combines observed masses (Table 1) with an independent MESA initial-mass--stripped-mass relation (Eq. B1) and the mass-conservation constraint that the donor was initially more massive than the accretor. Eqs. B3/B4 are analytic reductions of this logic, not fits to the sample. The strict lower-bound result (more than a quarter, 4/14, beta_min > 0.5; majority beta_min >= 0.3) is robust and uses Eq. B1, which is based on public MESA models with observationally calibrated overshooting. The only in-group dependence is the 'best guess' relation Eq. B2, which adds 20% residual envelope from the authors' own binary grids (Temmink et al. 2023; Jin et al. in prep). The abstract/conclusion 'half' count switches to this best-guess relation, and changing back to the strict lower bound reduces the count to 4/14. This is a self-citation/ansatz sensitivity in the headline framing, not a circular derivation of the central method; the conclusion of predominantly efficient mass transfer holds under the strict relation, though at a lower quantitative level (majority >= 0.3). Score 2.

Assumptions & free parameters 3 free parameters · 7 assumptions · 0 invented entities

The paper introduces no new particles, forces, or physical entities. Its central result depends on a model-based mapping between stripped star mass and initial donor mass, plus standard binary evolution assumptions and a few hand-chosen thresholds (q floors, circumbinary disk fraction, residual envelope fraction). None of these are fitted to the beta values being inferred, so the beta_min constraints are not circular in the narrow sense; the headline percentages do depend on the best-guess relation (2).

free parameters (3)
  • Residual envelope fraction after stripping = 0.2
    Added to the helium core mass to construct the best-guess initial mass-stripped mass relation (dashed line 2 in Figure 5). Chosen by hand to approximate the 10-25% incomplete stripping seen in binary model grids; directly raises the inferred beta_min values and therefore underlies the 'half above 50%' headline.
  • Initial mass ratio floor for contact/stability = q_min = 0.25 (strict), 0.5 (best guess)
    Used in Section 2 to set the conservative upper bound on beta. These thresholds come from stability and contact arguments in the literature, not from the data, and restrict the allowed initial parameter space.
  • Circumbinary disk mass fraction = 0.1 (default; 0 and 0.2 tested)
    Assumed in Appendix C and D for reconstructing initial periods and for the thermally limited model comparison. The paper states constraints are rare and tests alternatives, so it is a chosen input, not a fitted value.
assumptions (7)
  • domain assumption MESA single-star models with Z=0.014 and the adopted mass-dependent overshooting prescription give the true initial mass-helium core mass relation for the sample.
    Appendix B; the relation is calibrated observationally but remains a model-based mapping between MsdOB and Mdonor,initial.
  • domain assumption The helium core mass during hydrogen-shell burning is a strict lower limit on the stripped star mass in early Case B mass transfer.
    Section B and Figure 5; used to make relation (1) conservative. If true stripped masses are lower than this, beta_min estimates fall.
  • domain assumption The donor star was initially more massive than the accretor (Mdonor,initial > Macc,initial).
    Section 2, fundamental evolutionary constraint; the basis of the lower bound on accreted mass.
  • domain assumption Initial mass ratios below 0.25 lead to unstable mass transfer and ratios below 0.5 likely lead to contact, so they are excluded when setting upper bounds on beta.
    Section 2, citing Soberman et al. 1997 and Neo et al. 1977; restricts allowed initial parameters.
  • domain assumption The 16 systems are post-mass-transfer binaries that underwent stable early Case B mass transfer, with HR 2142 and HR 6819 as likely Case A exceptions.
    Section 2 and Appendix C; asserted classification of the sample, used when excluding the two systems from the main counts.
  • domain assumption Wind mass loss is negligible during the main sequence and early post-main sequence for the masses considered.
    Appendix B, statement in the MESA model description; if winds were important, the mass budget changes.
  • domain assumption No third companion has significantly altered the component masses of the systems.
    Section 4 caveat; the authors note this is rare but cannot be excluded for individual systems.

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Cite this review

Pith. "Pith review of Binary stars take what they get: Evidence for Efficient Mass Transfer from Stripped Stars with Rapidly Rotating Companions." pith.science (2026). https://pith.science/paper/OFAZEQCG

@misc{pith2026250514780,
  author       = {Pith},
  title        = {Pith review of: Binary stars take what they get: Evidence for Efficient Mass Transfer from Stripped Stars with Rapidly Rotating Companions},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/OFAZEQCG}},
  note         = {Machine review of arXiv:2505.14780}
}
read the original abstract

Binary stars and their interactions shape the formation of compact binaries, supernovae, and gravitational wave sources. The efficiency of mass transfer - the fraction of mass retained by the accretor during binary interaction - is a critical parameter that significantly impacts the final fate of these systems. However, this parameter is observationally poorly constrained due to a scarcity of well-characterized post-mass-transfer binaries. Be+sdOB binaries, consisting of a rapidly rotating Be star and a stripped hot subdwarf companion, are particularly valuable for studying mass transfer since they represent clear examples of past binary interaction. Recently, a significantly expanded observational sample of 16 Be+sdOB binaries with well-constrained masses was obtained through combined spectroscopic and interferometric observations. In this work, we compile and analyze this sample to provide robust constraints on the mass transfer efficiency in binaries that underwent stable mass transfer during the donor's hydrogen-shell burning phase. Our analysis reveals that mass transfer was predominantly conservative: half of the systems require mass transfer efficiencies above 50%. This challenges commonly adopted assumptions of highly non-conservative mass transfer in binary evolution modeling. Our findings are inconsistent with models that account for spin-up and limit accretion due to a centrifugal barrier. We also find tension with a commonly used mass transfer model in rapid population synthesis that limits accretion based on the thermal timescale of the accretor. These results have strong implications for almost all products of binary evolution including the variety of supernovae, white dwarfs, blue stragglers, runaway stars, X-ray binaries, and gravitational-wave sources.

Figures

Figures reproduced from arXiv: 2505.14780 by the authors.

Figure 1
Figure 1. illustrates this concept using ϕ Persei: the left panel depicts a scenario with fully conservative mass transfer (β = 1), where the accretor gains all the mass lost by the donor. The right panel shows the case where the efficiency is at its minimum allowed value, βmin, which is where the progenitors had nearly equal initial masses. Any efficiency lower than βmin would necessi￾tate Mdonor,initial < Macc,initial, viol… view at source ↗
Figure 2
Figure 2. Overview of our sample of 16 Be+sdOB binaries. We plot the present-day mass of the Be star (the rapidly spinning accretor) against that of the sdOB star (the stripped star). We also mark the estimated initial mass using Equation B1 on the top axis. The background color gradi￾ent and contours show the minimum mass transfer efficiency required to explain the present-day masses of each system, using our conservative es… view at source ↗
Figure 4
Figure 4. The systems in our sample are also in tension with predictions from the thermally limited model, [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figures from the paper (4 more)
Figure 5
Figure 5. Figure 5: Relationship between the initial mass and stripped star mass. [PITH_FULL_IMAGE:figures/full_fig_p010_5.png]
Figure 6
Figure 6. Figure 6: Correlation between the constraints on the mass transfer efficiency and current parameters (left) and inferred initial parameters (right). The lower bound refers to the minimum mass transfer efficiency (βmin) that is inferred assuming the median observed masses and the…
Figure 7
Figure 7. Figure 7: The inferred initial periods for each system in our sample. [PITH_FULL_IMAGE:figures/full_fig_p014_7.png]
Figure 8
Figure 8. Figure 8: Like [PITH_FULL_IMAGE:figures/full_fig_p015_8.png]

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Forward citations

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Reference graph

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