arxiv: 2604.21402 · v1 · submitted 2026-04-23 · 🌌 astro-ph.SR

A New Pathway to Single Be Stars: Ejected Companions from Type Ia Supernovae

Yuchen Bao , Zhenwei Li , Hongwei Ge , Hailiang Chen , Dengkai Jiang , Xuefei Chen , Zhanwen Han This is my paper

Pith reviewed 2026-05-09 20:49 UTC · model grok-4.3

classification 🌌 astro-ph.SR

keywords Be starsType Ia supernovaebinary evolutionrunaway starsmass transferstellar rotationsupernova kicks

0 comments p. Extension

The pith

Single Be stars can form as ejected companions from Type Ia supernovae in helium-main sequence binaries.

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

The paper proposes a new formation route for single Be stars in which a main-sequence star accretes mass from a helium companion, gains rapid rotation, and then is ejected as a single Be star when the helium star explodes as a Type Ia supernova. Binary evolution calculations show that roughly 0.4 percent of such helium-main sequence pairs reach this outcome. The same calculations indicate that 22 percent of the resulting Be stars receive ejection velocities high enough to qualify as runaway stars. This channel supplies an explanation for isolated, rapidly rotating B stars that does not require ongoing binary interaction.

Core claim

Approximately 0.4 percent of helium star plus main-sequence star binaries evolve into single Be stars via the Type Ia supernova channel. In this pathway the main-sequence star is spun up by mass transfer from the helium star before the helium star explodes, ejecting the now-single, rapidly rotating Be star. Detailed simulations map the initial parameter space that produces this outcome, and find that around 22 percent of the ejected Be stars have peculiar tangential velocities exceeding 24 km/s and are therefore runaways.

What carries the argument

Mass transfer from a helium star to a main-sequence companion that spins the companion to Be-star rotation rates, followed by a Type Ia explosion of the helium star that ejects the companion as a single object.

Load-bearing premise

Certain helium stars near the Chandrasekhar mass limit can explode as Type Ia supernovae through explosive oxygen burning initiated by the convective Urca process.

What would settle it

A large kinematic survey that finds the fraction of isolated Be stars with peculiar tangential velocities above 24 km/s is substantially below 22 percent would indicate that this supernova-ejection channel contributes far less than claimed.

Figures

Figures reproduced from arXiv: 2604.21402 by Dengkai Jiang, Hailiang Chen, Hongwei Ge, Xuefei Chen, Yuchen Bao, Zhanwen Han, Zhenwei Li.

**Figure 2.** Figure 2: Porb,i − MHe,i parameter space for different initial MS masses. The colorbar is the mass loss by the He star during mass transfer, defined as ∆MHe = MHe,i − MHe,f . Systems above the black dashed line will undergo an ECSN or FeCCSN, while those below the black solid line will produce a WD. The region between the dashed and solid lines corresponds to primordial binaries that produce a SN Ia. Assuming that t… view at source ↗

**Figure 3.** Figure 3: Simulated distributions of Galactic single Be stars in the [PITH_FULL_IMAGE:figures/full_fig_p010_3.png] view at source ↗

**Figure 4.** Figure 4: Similar to Figure 3, but for the simulated distributions of Galactic single Be stars in the [PITH_FULL_IMAGE:figures/full_fig_p011_4.png] view at source ↗

**Figure 5.** Figure 5: Tangential velocity distributions for simulated Galactic single Be stars. The black histogram shows [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗

read the original abstract

Be stars are rapid rotators generally produced by binary interactions. The single Be stars in the observations pose challenges to the Be star formation theory. In this paper, we propose a new pathway for the formation of single Be stars, in which the Be star is taken as the ejected companion star from a Type Ia supernova (SN Ia) explosion. Recent numerical simulations suggest that explosive oxygen burning, initiated via the convective Urca process in certain helium (He) stars near the Chandrasekhar mass limit, can set off a SN Ia. Based on this proposition, we further demonstrate that about $0.4\%$ of He star + main-sequence (MS) star binaries may evolve into single Be stars, where the MS star is spun up due to the mass accretion from the He star, and then the He star explodes as a SN Ia. We employ detailed binary evolutionary simulations and find the parameter space that would produce single Be stars via the SN Ia channel. Around $22\%$ of Be stars from the SN Ia progenitor channel exhibit peculiar tangential velocities exceeding $24\ \rm km/s$, classifying them as runaway stars. This suggests that the SN Ia channel plays a meaningful role in forming single Be stars, particularly within the runaway star population.

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.

Desk Editor's Note private letter to a colleague

The paper maps a new binary channel where single Be stars form as ejected companions from SN Ia explosions in He+MS systems, but the claimed fractions rest on an external and still-uncertain explosion mechanism.

read the letter

The core idea is straightforward: in some helium-star plus main-sequence binaries, the helium star transfers mass, spins up the companion to Be-star rotation, then explodes as a Type Ia supernova and leaves the spun-up star as a single runaway. They use detailed binary evolution calculations to identify the initial parameter space that produces this outcome and report that roughly 0.4 percent of such binaries follow the channel, with about 22 percent of the resulting Be stars showing tangential velocities above 24 km/s. That specific pathway is not in the earlier literature they cite, so the suggestion itself is new. The modeling work appears careful in tracing the mass-transfer and spin-up phases, and the runaway fraction is a concrete, testable output. The central numbers, however, are produced by assuming that the helium stars reach near-Chandrasekhar mass and then explode through the convective Urca process after mass transfer. That trigger is taken from separate recent simulations rather than derived or tested inside this work. If the explosion does not occur under the actual post-transfer compositions and conditions, the channel contributes nothing. The abstract gives no error bars on the fractions, no direct comparison to observed Be-star velocities or binary fractions, and no exploration of how sensitive the results are to the assumed supernova physics. The paper is therefore a clean theoretical proposal rather than a fully validated one. It is aimed at researchers working on Be-star formation channels and runaway populations. The binary modeling is solid enough that a serious referee should see it, even though the supernova assumption will need extra scrutiny and probably additional runs or observational checks before the fractions can be taken as firm.

Referee Report

2 major / 2 minor

Summary. The manuscript proposes a new formation channel for single Be stars in which a main-sequence star accretes mass from a helium-star companion, is spun up to Be-star rotation rates, and is subsequently ejected as a single runaway star following a Type Ia supernova explosion of the helium star. The explosion is assumed to be triggered by explosive oxygen burning initiated via the convective Urca process in helium stars near the Chandrasekhar limit. Detailed binary evolutionary simulations are used to identify the initial parameter space that produces this outcome, yielding the result that ~0.4% of He+MS binaries evolve into single Be stars and that ~22% of the resulting Be stars have peculiar tangential velocities exceeding 24 km/s.

Significance. If the external assumption that certain helium stars explode as SN Ia via the Urca process holds and the binary simulations accurately capture mass-transfer and spin-up physics, the channel would provide a concrete mechanism for producing isolated rapid rotators, particularly among the runaway population. The use of detailed binary evolutionary simulations to map the relevant initial-parameter space is a methodological strength that allows quantitative estimates of the channel's contribution.

major comments (2)

[Abstract] Abstract: the reported 0.4% fraction of He+MS binaries that produce single Be stars and the 22% high-velocity subset are presented as direct outcomes of the simulations, yet no error bars, sensitivity ranges, or tables of explored initial conditions (masses, periods, mass-transfer efficiencies) are supplied. Without these, it is impossible to judge whether the fractions are robust or depend on specific choices in the evolutionary code.
[Introduction] Introduction and mechanism description: the entire pathway rests on the premise that helium stars that have accreted or lost mass can reach conditions for convective-Urca-triggered oxygen burning and explode as SN Ia. The manuscript treats this as an external input from recent simulations and does not quantify what fraction of the post-mass-transfer helium stars in the computed grids actually satisfy the required mass, composition, and thermal conditions, nor does it propagate uncertainties in explosion energy or kick velocity into the final runaway statistics.

minor comments (2)

[Methods] A dedicated table or figure summarizing the initial binary-parameter grid, the fraction of systems that reach the SN Ia stage, and the resulting Be-star properties would greatly improve clarity and reproducibility.
[Results] The choice of the 24 km/s threshold for classifying runaways should be justified with reference to the local velocity dispersion or observational selection criteria used in Be-star surveys.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. We address each major comment below, indicating where revisions will be made to improve clarity and robustness.

read point-by-point responses

Referee: [Abstract] Abstract: the reported 0.4% fraction of He+MS binaries that produce single Be stars and the 22% high-velocity subset are presented as direct outcomes of the simulations, yet no error bars, sensitivity ranges, or tables of explored initial conditions (masses, periods, mass-transfer efficiencies) are supplied. Without these, it is impossible to judge whether the fractions are robust or depend on specific choices in the evolutionary code.

Authors: The reported fractions are direct results from our grid of detailed binary evolutionary simulations that map the initial parameter space of He+MS binaries leading to the described outcome. We agree that additional documentation of the grid would strengthen the presentation. In the revised manuscript we will add a table (or appendix section) summarizing the explored ranges of initial masses, orbital periods, and mass-transfer efficiencies, along with the number of models computed and the resulting fractions. We will also include a brief discussion of sensitivity to key assumptions such as mass-transfer efficiency, making clear that the quoted values apply to our fiducial setup. revision: yes
Referee: [Introduction] Introduction and mechanism description: the entire pathway rests on the premise that helium stars that have accreted or lost mass can reach conditions for convective-Urca-triggered oxygen burning and explode as SN Ia. The manuscript treats this as an external input from recent simulations and does not quantify what fraction of the post-mass-transfer helium stars in the computed grids actually satisfy the required mass, composition, and thermal conditions, nor does it propagate uncertainties in explosion energy or kick velocity into the final runaway statistics.

Authors: Our study takes the convective-Urca-triggered SN Ia explosion in suitable helium stars as an external premise drawn from recent dedicated simulations, and focuses on identifying the binary evolutionary pathways that produce a spun-up MS companion prior to the explosion. We did not perform a post-processing count of the exact fraction of post-mass-transfer helium stars meeting every detailed thermal and compositional criterion, as that would require coupling our binary models to full stellar-structure explosion calculations. In the revision we will expand the introduction and add a dedicated discussion paragraph that (i) restates the assumptions and cites the specific conditions from the literature, and (ii) examines how plausible ranges in explosion energy and kick velocity (drawn from existing SN Ia studies) would affect the reported 22% runaway fraction, thereby propagating the main uncertainty into the final statistics. revision: partial

Circularity Check

0 steps flagged

No significant circularity; central fractions are simulation outputs under external SN Ia assumption

full rationale

The paper's derivation chain consists of binary population synthesis and detailed evolutionary tracks that map initial He+MS binary parameters through mass transfer, spin-up of the MS star, and assumed SN Ia disruption to produce single Be stars and their velocity distribution. The 0.4% fraction and 22% high-velocity subset are direct outputs of these calculations once the external premise (He stars near Chandrasekhar limit exploding via convective Urca oxygen burning) is adopted from cited numerical simulations. No equation or result is defined in terms of itself, no fitted parameter is relabeled as a prediction, and the SN Ia mechanism is treated as an imported input rather than derived or self-cited within the load-bearing steps. The derivation therefore remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the assumption that certain helium stars near the Chandrasekhar limit can explode as Type Ia supernovae via explosive oxygen burning triggered by the convective Urca process, plus the binary population synthesis framework used to compute the 0.4% yield.

axioms (1)

domain assumption Explosive oxygen burning, initiated via the convective Urca process in certain helium stars near the Chandrasekhar mass limit, can set off a SN Ia
Invoked in the abstract as the basis for the SN Ia channel; drawn from recent numerical simulations.

pith-pipeline@v0.9.0 · 5543 in / 1332 out tokens · 48283 ms · 2026-05-09T20:49:19.495305+00:00 · methodology

discussion (0)

Reference graph

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