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arxiv: 2605.22911 · v1 · pith:EUURF7CTnew · submitted 2026-05-21 · 🌌 astro-ph.SR

Mergers via failed common envelope as a route towards intermediate-mass stripped stars

Annachiara Picco , Pablo Marchant , Daniel Pauli , Hugues Sana This is my paper

Pith reviewed 2026-05-25 02:15 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords stripped starscommon envelope evolutionbinary mergersintermediate-mass starsblue stragglershelium burning starshierarchical triples
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The pith

Failed common envelope mergers can form intermediate-mass stripped stars spanning 6 to 14 solar masses.

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

This paper explores how mergers from failed common envelope evolution between a stripped star and its companion can produce intermediate-mass stripped stars. Detailed binary simulations at Galactic metallicity show these merger products contribute to stripped star populations across the Hertzsprung-Russell diagram and create a blue-straggler effect. The resulting objects are long-lived core helium-burning stars with thin hydrogen envelopes, appearing as single stars or in wide binaries originally from hierarchical triples.

Core claim

Merger products from failed common envelopes between stripped stars and post-main sequence companions can contribute to the population of stripped stars, with masses from 6 to 14 solar masses, consistent with long-lived core He-burning stars retaining thin hydrogen envelopes after partial CE ejection.

What carries the argument

Failed common envelope merger process modeled through detailed interacting binary simulations at Galactic metallicity, leading to partial ejection and retention of thin hydrogen envelope.

If this is right

  • These objects span masses from 6 to 14 solar masses.
  • They produce a blue-straggler effect in the Hertzsprung-Russell diagram.
  • They appear as single stars or members of wide binaries from original hierarchical triples.
  • They are consistent with long-lived core helium-burning phase.

Where Pith is reading between the lines

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

  • This channel could explain the formation of magnetic intermediate-mass stripped stars like HD 45166.
  • Population synthesis models may need to include this merger route to accurately predict stripped star populations.
  • Observations of stripped stars in wide binaries could test this formation path.

Load-bearing premise

The detailed interacting binary simulations at Galactic metallicity accurately capture the outcome of a failed common envelope merger, including retention of a thin hydrogen envelope and subsequent long-lived core helium burning.

What would settle it

A survey finding no stripped stars with masses between 6 and 14 solar masses in positions consistent with core helium burning and thin envelopes, or absence of such stars in wide binaries, would challenge the contribution of this channel.

Figures

Figures reproduced from arXiv: 2605.22911 by Annachiara Picco, Daniel Pauli, Hugues Sana, Pablo Marchant.

Figure 1
Figure 1. Figure 1: Sketch of the merger via failed CE channel towards [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 3
Figure 3. Figure 3: Parameter space in initial period Pi and mass ratio qi for failed-CE stripped stars for a selection of values of initial pri￾mary masses M1, i (color-coded). The part of the parameter space that undergoes case A MT in the first interaction is also indicated with x scatter points. Full grids similar to [PITH_FULL_IMAGE:figures/full_fig_p003_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Bottom panel: fractions of systems with di [PITH_FULL_IMAGE:figures/full_fig_p004_5.png] view at source ↗
read the original abstract

Stripped stars are a common product of binary stellar systems and span a wide mass range from Wolf-Rayet stars to hot subdwarfs and helium white dwarfs. The recent discovery of intermediate-mass stripped stars, with masses between those of WRs and subdwarfs, provides a continuous evolutionary sequence and valuable test beds for binary interaction models. Population synthesis studies explain the formation of stripped products through stable mass transfer or common envelope evolution. Recently, however, a merger scenario (or, "failed common envelope") between a stripped star and a post-main sequence companion was suggested to explain the formation of the magnetic intermediate-mass stripped star HD 45166. In this Letter, we investigate this channel using detailed interacting binary simulations at Galactic metallicity and model their stripped merger products. We find that these merger products can contribute to the population of stripped stars across the Hertzsprung-Russell diagram and produce a blue-straggler effect, with merger masses spanning from 6 to 14 solar masses. These objects would be consistent with long-lived core He-burning stars retaining thin hydrogen envelopes after a partial CE ejection, and they would appear as single or members of wide binaries that were originally hierarchical triples.

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 manuscript investigates the formation of intermediate-mass stripped stars (6-14 M⊙) via mergers in failed common-envelope evolution between a stripped star and a post-main-sequence companion. Using detailed interacting binary simulations at Galactic metallicity, the authors conclude that the resulting merger products are long-lived core He-burning stars retaining thin hydrogen envelopes after partial CE ejection; these objects can populate the HR diagram, produce a blue-straggler effect, and appear as single stars or wide binaries originally from hierarchical triples, providing a channel that complements stable mass transfer and standard CE evolution and potentially explaining objects such as HD 45166.

Significance. If the post-merger envelope retention and evolutionary outcomes hold, the work identifies a previously under-explored route to intermediate-mass stripped stars that bridges the mass gap between Wolf-Rayet stars and hot subdwarfs. The concrete mass range and the link to hierarchical triples supply falsifiable predictions for both single-star and binary populations that could be tested with current and upcoming surveys.

major comments (2)
  1. [binary simulation description (abstract and methods)] The headline result—that merger products retain a thin yet sufficient H envelope to sustain long-lived core He-burning—depends on the specific implementation of partial CE ejection, energy budget, and mass-loss prescription in the 1D code. No validation against 3D hydrodynamics or anchoring to the observed properties of HD 45166 is reported, leaving the central structural outcome untested.
  2. [results on merger products] The reported merger masses (6–14 M⊙) and the claim that these objects contribute across the HR diagram are presented without error bars, sensitivity tests to the free parameters (initial binary parameters and CE physics prescriptions), or discussion of numerical limitations, which directly affects the robustness of the population-synthesis implication.
minor comments (1)
  1. [Abstract] The abstract would be clearer if it stated the stellar evolution code employed and the number of binary models computed.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments on our manuscript. We address each major point below and indicate where revisions will be made to improve clarity and robustness.

read point-by-point responses

  1. Referee: [binary simulation description (abstract and methods)] The headline result—that merger products retain a thin yet sufficient H envelope to sustain long-lived core He-burning—depends on the specific implementation of partial CE ejection, energy budget, and mass-loss prescription in the 1D code. No validation against 3D hydrodynamics or anchoring to the observed properties of HD 45166 is reported, leaving the central structural outcome untested.

    Authors: We agree that the envelope retention outcome is sensitive to the 1D code's CE treatment. Our work is motivated by the HD 45166 scenario but does not include a direct parameter fit to its observed properties. We will revise the methods and discussion sections to explicitly describe the CE energy budget and mass-loss assumptions, add caveats regarding the lack of 3D hydrodynamical validation, and note this as a limitation requiring future work. revision: partial

  2. Referee: [results on merger products] The reported merger masses (6–14 M⊙) and the claim that these objects contribute across the HR diagram are presented without error bars, sensitivity tests to the free parameters (initial binary parameters and CE physics prescriptions), or discussion of numerical limitations, which directly affects the robustness of the population-synthesis implication.

    Authors: The quoted mass range is the outcome of the specific simulation grid presented. We will add text in the results section discussing sensitivity to initial binary parameters and CE prescriptions, along with numerical limitations of the 1D approach. As this is a deterministic grid study rather than a full population synthesis, we will clarify the explored parameter space instead of adding formal error bars. revision: yes

Circularity Check

0 steps flagged

No circularity: forward simulations generate outputs from initial conditions

full rationale

The paper runs detailed 1D binary evolution simulations at Galactic metallicity to evolve hierarchical triples through a failed common-envelope phase and produce post-merger stripped stars. The reported mass range (6–14 M⊙), thin H-envelope retention, and core-He-burning lifetimes are direct numerical outputs of those simulations rather than quantities fitted to the target population or redefined by self-citation. The single reference to the HD 45166 scenario supplies context only and is not invoked as a uniqueness theorem or load-bearing premise. No equation or result is shown to equal its own input by construction.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

Only the abstract is available; the simulations rest on standard 1D binary evolution assumptions and numerous unspecified initial conditions and physics parameters.

free parameters (1)
  • Initial binary parameters and CE physics prescriptions
    Masses, periods, mass-transfer efficiencies, and common-envelope ejection criteria must be chosen to run the simulations; none are listed in the abstract.
axioms (1)
  • domain assumption 1D stellar structure codes accurately model the merger and post-merger evolution of stripped stars
    Invoked by the use of detailed interacting binary simulations to produce the reported merger products.

pith-pipeline@v0.9.0 · 5745 in / 1289 out tokens · 33883 ms · 2026-05-25T02:15:05.566343+00:00 · methodology

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