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arxiv: 2606.26262 · v1 · pith:RSUWOPHWnew · submitted 2026-06-24 · 🌌 astro-ph.SR · astro-ph.HE

A Stellar Role Reversal: Multiple Features in the Mass and Mass Ratio Distributions of Merging Binary Black Holes from Stable Mass Transfer

Gina Chen , Katelyn Breivik , Lieke A. C. van Son This is my paper

Pith reviewed 2026-06-26 01:18 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.HE
keywords binary black holesstable mass transfermass ratio reversalgravitational wave populationsmass distributionbinary population synthesismass transfer stability
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The pith

Stable mass transfer produces two distinct subpopulations in binary black hole masses and mass ratios.

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

The paper demonstrates that under conservative mass transfer the stable mass transfer channel for binary black hole formation yields two observationally distinct groups. A high-primary-mass population with near-equal mass ratios forms through mass ratio reversal, while a low-primary-mass population forms without reversal. Stability criteria that depend on the donor star's evolutionary stage divide the primary-mass versus mass-ratio plane into complementary regions, placing the two groups into separate peaks. This imprint means the observed mass function of merging black holes carries direct information about the physics of mass transfer and accretion efficiency.

Core claim

Under the assumption of conservative mass transfer, the SMT channel produces two observationally distinct subpopulations: a high primary mass, near equal mass ratio population formed through mass ratio reversal (MRR), and a low primary mass non-MRR subpopulation. The mass range where MRR occurs is determined by assumptions about binary SMT. In particular, the stability criteria for mass transfer at different stellar evolutionary stages carve out complementary regions in the primary-mass--mass-ratio plane, separating the MRR and non-MRR populations into distinct peaks at high and low primary mass respectively.

What carries the argument

Stability criteria for mass transfer at different stellar evolutionary stages, which divide the primary-mass--mass-ratio plane into complementary MRR and non-MRR regions.

If this is right

  • The binary black hole mass function develops distinct peaks at high and low primary mass.
  • Near-equal mass ratios become associated with the higher-mass peak.
  • The locations of the peaks shift when assumptions about mass-transfer stability or accretion efficiency change.
  • Current and near-future gravitational-wave detectors can resolve these separate subpopulations.

Where Pith is reading between the lines

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

  • Observed distributions lacking the predicted peaks would point toward non-conservative mass transfer or different stability rules.
  • The separation supplies a potential way to isolate the stable mass transfer contribution from other formation channels in future catalogs.
  • Varying the accretion efficiency in population models would move the boundary between the two subpopulations in a predictable way.

Load-bearing premise

Mass transfer is fully conservative so that all transferred mass is accreted, combined with the specific stability criteria applied at each evolutionary stage.

What would settle it

A catalog of merging binary black holes whose primary-mass and mass-ratio distribution shows a single continuous population without separated high-mass equal-ratio and low-mass peaks.

Figures

Figures reproduced from arXiv: 2606.26262 by Gina Chen, Katelyn Breivik, Lieke A. C. van Son.

Figure 1
Figure 1. Figure 1: A schematic showing the major evolutionary stages in the stable mass transfer (SMT) only channel. transfer are subject to stability criteria and both in￾stances of core collapse can produce natal kicks. 80% of the merging BBHs in our cosmerge simulation fol￾low these stages of evolution. An additional 15% of the merging population experiences three phases of RLOF, where the first instance of RLOF occurs wh… view at source ↗
Figure 2
Figure 2. Figure 2: Merger rates as a function of the chirp mass (top left), BBH mass ratio (bottom left), and individual component masses (right) for the merging BBH population evaluated at z = 0.1. Black solid lines denote the entire SMT-only population, while pink and blue lines denote the non-MRR and MRR subpopulations respectively. The gray histogram on the right panel is the GTWC-5 component mass distribution, using the… view at source ↗
Figure 3
Figure 3. Figure 3: The primary masses and initial mass ratios of the merging SMT-only BBHs. We normalize each population separately, and use the opacity to indicate the relative size of each subpopulation. The gray dotted contours and shading show the full SMT-only population. Left panel: BBHs are classified by the donor star’s evolutionary state during MT1. Vertical lines denote qcrit,1 for each type of donor star, which is… view at source ↗
Figure 4
Figure 4. Figure 4: The minimum mass of each component of a BBH formed through the SMT-only channel according to our an￾alytic model for the five β1 values we simulated. Increasing β1 results in a higher minimum limit for both MBH,a and MBH,b In order to determine the effect of β1 on the merger rate and mass and qBBH distributions, we simulate BBHs at an additional four fixed β1 values (0, 0.25, 0.5, and 0.75) and compare to … view at source ↗
Figure 5
Figure 5. Figure 5: The merger rate as a function of primary mass for different β1 values. In the top row, the population is split into MRR (blue) and non-MRR (pink) subpopulations, and in the bottom row, the population is split by donor star type during MT1. The full SMT-only merger rate Rtot evaluated at z = 0.1 is given in units of Gpc−3 yr−1 . Black lines denote the full SMT-only population in both rows. We do not include… view at source ↗
Figure 6
Figure 6. Figure 6: The merger rate as a function of BBH mass ratio for different β1 values. As in [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
read the original abstract

Observations of gravitational wave events have enabled the measurement of the merging binary black hole (BBH) mass function. This mass function encodes the physical interactions which shape the formation and evolution of BBHs. In this work we investigate how the stable mass transfer (SMT) channel of BBH formation imprints onto the BBH primary mass and mass ratio distributions. We use both an analytic framework and binary population synthesis to show how assumptions about mass transfer accretion efficiency and mass transfer stability affect the BBH mass distribution. Under the assumption of conservative mass transfer, we find that the SMT channel produces two observationally distinct subpopulations: a high primary mass, near equal mass ratio population formed through mass ratio reversal (MRR), and a low primary mass non-MRR subpopulation. The mass range where MRR occurs is determined by assumptions about binary SMT. In particular, we find that the stability criteria for mass transfer at different stellar evolutionary stages carve out complementary regions in the primary-mass--mass-ratio plane, separating the MRR and non-MRR populations into distinct peaks at high and low primary mass respectively. Our results imply that the physics of SMT creates distinct features in gravitational wave populations which current and near future gravitational wave detectors may be able to resolve.

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

0 major / 1 minor

Summary. The manuscript claims that under the assumption of conservative mass transfer, the stable mass transfer (SMT) channel for binary black hole formation produces two observationally distinct subpopulations in the primary-mass and mass-ratio distributions: a high-primary-mass, near-equal-q population formed via mass ratio reversal (MRR) and a low-primary-mass non-MRR subpopulation. These subpopulations arise because stability criteria for mass transfer at different stellar evolutionary stages carve complementary regions in the primary-mass--mass-ratio plane. The result is demonstrated with both an analytic framework and binary population synthesis.

Significance. If the result holds, it supplies a direct physical mechanism linking SMT assumptions to distinct, potentially resolvable features in the BBH mass function measured by gravitational-wave detectors. Explicit credit is due for the dual use of analytic modeling and population synthesis, which maps the input physics (accretion efficiency and stability criteria) onto observable distributions in a falsifiable way.

minor comments (1)
  1. [Abstract] The abstract and introduction should more explicitly flag that all reported subpopulations are conditional on the conservative-mass-transfer assumption and the adopted stability criteria; this is already stated but could be highlighted earlier to avoid misreading as a general prediction.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive and accurate summary of our manuscript, as well as the recommendation for minor revision. The report correctly identifies the central result that conservative stable mass transfer produces two distinct subpopulations in the primary-mass and mass-ratio distributions via mass ratio reversal, with the separation arising from evolutionary-stage-dependent stability criteria. No specific major comments were raised.

Circularity Check

0 steps flagged

No significant circularity; derivation is self-contained from stated assumptions

full rationale

The paper derives the claimed subpopulations (high-mass MRR and low-mass non-MRR) directly from explicit inputs: conservative mass transfer plus adopted stability criteria at different evolutionary stages. These inputs are used in both analytic modeling and population synthesis to produce complementary regions in the primary-mass--mass-ratio plane. No parameter is fitted to data and then relabeled as a prediction, no self-citation chain supplies a load-bearing uniqueness theorem, and no ansatz is smuggled in. The result is conditional on the stated physics assumptions and does not reduce to those assumptions by construction.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

Only the abstract is available, so the ledger is limited to explicitly stated assumptions. Full paper likely contains additional free parameters inside the population-synthesis code and further domain assumptions about binary evolution.

axioms (2)
  • domain assumption Mass transfer is conservative (all mass lost by donor is accreted by companion)
    Explicitly invoked in the abstract as the assumption under which the two subpopulations appear.
  • domain assumption Stability criteria for mass transfer depend on stellar evolutionary stage and carve complementary regions in the primary-mass--mass-ratio plane
    Stated in the abstract as the mechanism that separates MRR and non-MRR populations into distinct peaks.

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