The Stellar Winds Atlas II: Black Hole Formation at Solar Metallicity

Alex C. Gormaz-Matamala; Amedeo Romagnolo; Avishai Gilkis; Daniel Pauli; Floor S. Broekgaarden; Konstantinos Antoniadis; Laya Binu; Lucas M. de S\'a; Lumen Boco; Michela Mapelli

REVIEW 3 major objections 5 minor 299 references

The Stellar Winds Atlas II: Black Hole Formation at Solar Metallicity

T0 review · 3 major / 5 minor · reviewed 2026-08-01 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read At solar metallicity, a single fork decides how massive a black hole a dying star leaves behind: collapse as a cool supergiant and keep a heavy remnant, or be stripped into a Wolf-Rayet star and lose most of its mass to thick winds.

desk verdict A systematic and useful wind-era map of BH mass predictions at Z_sun; the supergiant-branch peak is an upper limit, and the framing should stop selling it as the prediction. read the letter →

arxiv 2607.26147 v1 pith:4CIWZ7GR submitted 2026-07-28 astro-ph.SR astro-ph.GA

Amedeo Romagnolo , Floor S. Broekgaarden , Alex C. Gormaz-Matamala , Lucas M. de Sá , Daniel Pauli , Avishai Gilkis , Lumen Boco , Michela Mapelli

show 2 more authors

Konstantinos Antoniadis Laya Binu

This is my paper

classification astro-ph.SRastro-ph.GA

keywords blackholeformationstellarwindsWolf-Rayetstarscoolsupergiantmasslosssolarmetallicitymassivestarevolutionmass-lossprescriptionsHumphreys-Davidsonlimit

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

At solar metallicity, the mass of the black hole a massive star leaves behind is set less by how strong its winds are in detail than by which of two evolutionary paths it takes. The paper argues the decisive fork is whether the star loses its hydrogen envelope and becomes a Wolf-Rayet star before core collapse. Stars that enter the Wolf-Rayet stage have their final mass dictated by thick, optically thick winds, which erase nearly all memory of earlier mass loss. Stars that instead collapse while still cool supergiants retain their envelopes and form substantially heavier black holes, producing a peak around 30 solar masses near an initial mass of 40 solar masses. The result maps the wide spread in existing theoretical predictions onto two controllable bottlenecks — envelope stripping efficiency and Wolf-Rayet mass-loss rates — and this is what makes the problem tractable.

What carries the argument

The load-bearing object is the evolutionary bifurcation defined by the paper: whether a star collapses as a cool supergiant or first becomes a Wolf-Rayet star. The immediate switch controlling it is the effective-temperature threshold at which cool supergiant winds are initiated; moving this threshold by 0.5 kK can change a 40-solar-mass star's remnant mass by about 5 solar masses. For stars that pass the switch and enter the Wolf-Rayet stage, the optically thick wind prescription (especially for hydrogen-free Wolf-Rayet stars) takes over and dictates the final mass. The paper also uses the timing of the transition to optically thick winds as a diagnostic, linking it to the Humphreys-Davidso

What would settle it

A census of solar-metallicity black holes: if no isolated black holes appear in the roughly 20–30 solar mass range, the supergiant branch is suppressed. Separately, the Wolf-Rayet/OB ratio at luminosities around log(L/Lsun) ~ 6.3–6.5 can falsify timing predictions; for example, models that predict no OB stars above about 45–65 solar masses are in tension with the observed 110-solar-mass OB star Cyg OB2 #12.

Watch

Extended reading notes

Core claim

The paper's central discovery is a bifurcation in black-hole remnant mass at solar metallicity. Across 14 wind prescriptions in a common 1D stellar evolution setup, final remnant mass converges to two branches: the Wolf-Rayet branch, where optically thick winds dominate and remove most of the mass, and the cool-supergiant branch, where the envelope is retained and the remnant is much heavier. The paper shows this bifurcation is universal: it appears in every model, and the choice of cool-supergiant mass loss — specifically the effective temperature at which those winds switch on — controls which branch a star takes. A 40-solar-mass star collapses into a 28.6-solar-mass black hole if cool sup

Load-bearing premise

The paper assumes every star collapses directly to a black hole, conserving all its pre-collapse mass except 1% lost to neutrinos; the authors themselves note this likely overestimates remnant masses for stars that retain a loosely bound hydrogen envelope, and partial envelope ejection during core collapse could shrink the heavy supergiant branch.

Editorial extensions

If this is right

If the bifurcation is correct, the final black hole mass at solar metallicity reduces to two bottlenecks: envelope stripping efficiency (whether the star becomes a Wolf-Rayet star) and Wolf-Rayet mass-loss rates.
Stars collapsing as cool supergiants produce a black hole mass peak near 30 solar masses around an initial mass of 40 solar masses, so an observational census of isolated solar-metallicity black holes in the 20–30 solar mass range can test this branch.
Stars that enter the Wolf-Rayet phase yield similar final black hole masses regardless of their prior mass-loss history, meaning model disagreements trace to thick-wind prescriptions rather than main-sequence winds.
The timing of the transition to optically thick winds determines whether stars respect the Humphreys-Davidson limit, and the observed Wolf-Rayet/OB star ratio in the Milky Way is a direct model-independent probe of that timing.
If hydrogen-free Wolf-Rayet winds are weak, very massive solar-metallicity stars can enter the pair-instability pulsation regime; the absence of isolated black holes above roughly 30 solar masses would be evidence that such massive remnants require binary or dynamical formation.

Reading between the lines

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

If the bifurcation is universal, the same two bottlenecks may organize black hole mass predictions at lower metallicity, meaning calibrating envelope stripping and Wolf-Rayet winds at solar metallicity would sharpen predictions for high-redshift gravitational-wave merger rates.
The extreme sensitivity to a 0.5 kK shift in the cool-supergiant wind threshold suggests that direct empirical constraints on yellow supergiant winds, not just red supergiants, would be unusually high-leverage for black hole mass predictions.
The supergiant branch implies a distinctive dichotomy in remnant masses — heavy supergiant-collapse remnants versus lighter Wolf-Rayet remnants — that could be searched for in astrometric and X-ray binary black hole populations.
The paper deliberately leaves luminous blue variable eruptions unmodeled; if those eruptions are what enforce the Humphreys-Davidson limit by stripping envelopes, the supergiant branch would be suppressed, so the bifurcation may partly be an artifact of missing eruptive mass loss.

Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

The two things to know: this is a genuinely systematic grid—14 wind prescriptions, one MESA framework, side-by-side transition criteria, and a clean sensitivity test (Fig. 2) that isolates the cool-supergiant threshold as the control knob for the 40-solar-mass peak. The bifurcation idea (supergiant vs. WR pathway) is not brand-new in every piece, but the head-to-head comparison within a common code, plus the new KABS and Warm_Gamma combinations, makes it a reference-grade atlas. The paper is honest about the direct-collapse assumption, explicitly calling it an upper limit and citing Nadezhin and Lovegrove & Woosley in footnote 4.

The soft spot is exactly there. The supergiant branch produces its ~30 M_sun BHs at M_ZAMS~40 because essentially the entire pre-collapse mass is dumped into the remnant. If neutrino-driven shock ejection removes a chunk of the loosely bound H envelope—the same mechanism the paper itself flags—the heavy branch comes down toward the CO-core mass, and the contrast between the two branches shrinks. The authors acknowledge this in the text, but the abstract and the Supergiant Pathway bullet present the peak as the prediction rather than a ceiling. That framing needs fixing. The 'universally controlled' claim is also broader than the parameter space actually explored, though the Fig. 2 experiment supports the weaker version: within this grid, the T_eff,trans of cool supergiant winds is the dominant switch. The WR/OB comparison rests on small, incomplete samples; the authors say as much, but the conclusion section leans on it more than the data warrant.

Credit where due: the code and MESA inlists are on GitHub, the model grid is internally consistent, and the comparison with previous literature (Fig. 17) is useful precisely because it makes the divergences interpretable. This is the kind of paper that deserves a serious referee—not for the absolute BH masses, but for the map of how wind prescriptions and transition criteria move the result. I would send it to review with a request to soften the claims in the abstract and conclusions, and to give the envelope-ejection caveat a prominent, quantitative treatment rather than a footnote.

For a reading group, this is a good case study in how to do a systematic model survey and how not to overstate an upper limit. I would cite it for the atlas value, not for the peak.

Referee Report

3 major / 5 minor

Summary. This paper constructs a 'Wind Atlas' for solar-metallicity massive stars by running 14 wind prescriptions in a common 1D MESA framework over M_ZAMS = 20–300 Msun, then uses the StarEstate population-synthesis code to compare synthetic VMS populations with Galactic OB/WR samples. The central claim is that the final BH mass is set by a bifurcation: stars that lose enough envelope to become Wolf-Rayet stars end up with masses set by their thick winds, whereas stars that collapse as cool supergiants retain much of their envelope and form more massive BHs, producing a peak near M_ZAMS ~ 40 Msun in models with weak YSG winds. The paper argues that the cool-supergiant wind threshold (T_eff,trans) controls this bifurcation and identifies envelope stripping and WR mass-loss rates as the two key bottlenecks. It tests this framework against Cygnus X-1, the HD limit, and the Galactic WR/OB ratio.

Significance. If the central bifurcation claim holds, the paper provides a valuable organizing principle for a notoriously divergent literature: rather than focusing on the overall strength of winds, modelers should focus on envelope stripping efficiency and WR mass-loss rates. The study is unusually systematic, with 14 models in a common code, a controlled sensitivity test in Fig. 2, and open MESA inlists and population-synthesis code. The comparisons to Cygnus X-1, the HD limit, and observed OB/WR populations are genuine external checks, not fits to the target result. The main weakness is the direct-collapse assumption for supergiant remnants, which the paper itself flags as an upper limit; because the ~40 Msun peak is the flagship prediction, this assumption needs quantitative treatment before the bifurcation claim can be considered robust.

major comments (3)

[Sec. 2.1; Fig. 1; Sec. 3.1.2] The direct-collapse assumption is load-bearing for the supergiant pathway. The text sets M_BH = M_pre-collapse - 1% neutrino mass for all progenitors, and note 4 concedes that neutrino mass loss can shock-eject loosely bound RSG envelopes (Nadezhin 1980; Lovegrove & Woosley 2013; Fernández et al. 2018). The 28.6 Msun BH at M_ZAMS = 40 Msun in FEScRSG/MScRSG is essentially the whole pre-collapse mass. If even a modest fraction of the H-rich envelope is ejected during collapse, the supergiant-branch remnants drop toward the CO-core mass, the prominent peak in Fig. 1 is strongly suppressed or shifted, and the contrast with the WR branch shrinks. Please add a quantitative sensitivity study (e.g., using a simple neutrino-mass-loss envelope-ejection prescription or reporting the CO-core mass as a lower bound for each track) and revise the abstract/conclusions so that the supergiant peak is pre
[Sec. 3.1.3; Fig. 2] The claim that the cool-supergiant wind threshold 'universally controls' the BH mass bifurcation is based on a single 40 Msun FESc track. The sharp drop from 28.6 to 15.7 Msun between T_eff,trans = 4.0 and 5.0 kK is convincing for that case, but the text in Sec. 3.1.2 says the transition condition to optically thick winds is 'nearly irrelevant' in the 20–50 Msun range, while Fig. 1 shows nontrivial model-to-model scatter there. To support 'universally', please show at least a small grid in (M_ZAMS, T_eff,trans) or explicitly restrict the claim to stars near the bifurcation boundary.
[Sec. 3.3; Fig. 4] The WR/OB population comparison is presented as a decisive test, but it depends on post-processed RLOF checks, the assumed binary fraction and period distribution, and the effective-single fraction (27–53% across models). This is a useful plausibility argument, but it is not a quantitative model-selection statistic. Please either add error bars or explicitly state that the comparison is qualitative; this would also make the text in Sec. 3.3 less vulnerable to over-interpretation.

minor comments (5)

[Sec. 3.2.1] The text says the Z=0.019 version of MScV01 predicts a near-ZAMS transition at M_ZAMS >= 65 Msun 'due to weaker mass loss'. Higher Z should increase V01 rates; please clarify whether this is a scaling artifact or a typo.
[Sec. 2.2; Fig. 4] The effective-single fractions and binary interaction criteria are model-dependent; please state the uncertainties in the synthetic population more explicitly in the text, not only in the figure caption.
[Appendix C] When applying the direct-collapse minus 1% formula to literature final masses, the comparison is not apples-to-apples because those studies include different explosion prescriptions. Please note this explicitly in the caption or text.
[Sec. 4.2] The statement that the bifurcation is dominated by winds 'rather than mass transfer events in binaries' (citing Shenar et al. 2020) is stronger than the cited work may support; a softer phrasing would be safer.
[General] The paper relies heavily on the companion 'Atlas I' for the KABS model and calibration details. Since this manuscript may be read independently, please include a short self-contained description of the KABS transition and wind-switch rules in the text or a table footnote.

Circularity Check

0 steps flagged · score 2.0 of 10

No real circularity: the BH-mass bifurcation is computed from externally defined wind grids; the only self-citation is to Atlas I/StarEstate and is not load-bearing.

full rationale

Walking the derivation chain, I find no step where a predicted quantity is equivalent to an input by construction. The 14 wind schemes are externally defined (V01, dJ88, NL00, B20, SV20, GM23, K24, P25, A24, etc.), and the grid is evolved in MESA; the WR/supergiant bifurcation and the ~40 Msun peak are read off the resulting M_BH(M_ZAMS) curves, not imposed as a target. The only non-external inputs from the authors' own prior work are the KABS model (Atlas I; 'originally developed in Atlas I') and the StarEstate population-synthesis code; these are transparently cited and do not smuggle in the conclusion, because the same qualitative supergiant branch is produced by FEScRSG and MScRSG, which are constructed from literature recipes. The direct-collapse prescription (Sec. 2.1: 'we use an upper limit to the BH mass and assume that all stars face direct BH collapse, conserving the totality of their pre-core collapse mass minus 1% being ejected as neutrinos') is an explicitly acknowledged upper limit that inflates the supergiant-branch peak; this is a substantive physical caveat and the paper flags the RSG-envelope-ejection risk in the same section and in footnote 4, but an assumption labeled as an assumption is not circular. No fitted parameter is renamed as a prediction, no author-uniqueness theorem is invoked, and the WR/OB and Cygnus X-1 comparisons are independent tests. Minor self-citation (Atlas I, StarEstate, Romagnolo et al. 2024) is present but not load-bearing, hence score 2 rather than 0.

Assumptions & free parameters 3 free parameters · 8 assumptions · 0 invented entities

No numbers are fitted to the target result; the paper is a comparison grid. The listed parameters and axioms are the model choices whose variation would most affect the bifurcation claim.

free parameters (3)

Cool supergiant wind onset temperature (T_eff, trans) = 4-10 kK (depends on model; see Fig 2)
Chosen per model: FESc uses 10 kK, RSG-only variants use 4 kK. The sensitivity run in Sec 3.1.3 shows a 0.5 kK change around 4.5-5 kK shifts the 40 Msun BH mass from ~24 to ~16 Msun, so the location of this threshold controls whether the supergiant branch exists.
Neutrino mass-loss fraction at collapse = 1%
Normalizes all reported BH masses under the direct-collapse upper limit (Sec 2.1).
Initial rotation Omega_init/Omega_crit = 0.4 (0.6 in FESchighrot)
Set to a round value from the literature; the 0.6 variant shows negligible effect on final BH mass, so this parameter is not central.

assumptions (8)

domain assumption All stars collapse directly to a BH, conserving pre-collapse mass minus 1% (Sec 2.1).
Load-bearing for the supergiant branch masses; the paper flags it as an upper limit.
ad hoc to paper WR stars form as soon as the star develops optically thick winds (Sec 2.1).
Defines the WR onset for all 14 models; different criteria (Gamma_e, eta, Xsurf) are compared, but the assumption that thick winds = WR is a simplification.
ad hoc to paper Cool supergiant winds are turned on at T_eff <= 10 kK (FESc) or <= 4 kK (RSG-only models).
The central bifurcation is controlled by this threshold; the paper varies it only in one sensitivity test (Fig 2).
domain assumption Fixed mixing prescription: Ledoux + exponential overshoot f_ov=0.05, no semiconvection (Sec 2.1).
Envelope stripping and WR formation depend on mixing; not varied across the grid.
domain assumption Initial rotation at 0.4 of critical velocity (Sec 2.1).
Rotation drives surface enrichment and mass loss; only one variant tested.
domain assumption Pair-instability supernovae (PPSN/PSN) are ignored (Sec 2.1).
Affects the upper-mass regime; the paper notes only the artificially-underestimated H-free WR wind model enters PPSN.
domain assumption Wind prescriptions from the literature (V01, dJ88, NL00, B20, SV20, GM23, A24, K24, P25, V17) are reliable within their claimed ranges.
The grid's outcome is a direct consequence of these external rates; no re-calibration is attempted.
domain assumption Population synthesis parameters (binary fraction 75%, Sana+12 period/eccentricity distributions, Frankel+18 metallicity relation) describe the Milky Way VMS population (Sec 2.2).
Underlies the WR/OB ratio comparison in Fig 4.

how reviews work

0 comments

Cite this review

Pith. "Pith review of The Stellar Winds Atlas II: Black Hole Formation at Solar Metallicity." pith.science (2026). https://pith.science/paper/4CIWZ7GR

@misc{pith2026260726147,
  author       = {Pith},
  title        = {Pith review of: The Stellar Winds Atlas II: Black Hole Formation at Solar Metallicity},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/4CIWZ7GR}},
  note         = {Machine review of arXiv:2607.26147}
}

abstract

Stellar winds are a primary source of uncertainty in predicting the masses of black holes (BHs) from massive stars. At solar metallicity, theoretical models lead to widely divergent results due to differing wind prescriptions. A key obstacle remains the lack of systematic investigations across a common parameter space. To address this, we construct a ``Wind Atlas'' using detailed 1D MESA stellar evolution models and population synthesis techniques to estimate the Galactic population of solar metallicity BH progenitors. We systematically investigate 14 distinct wind models, ranging from the most traditional and widespread prescriptions to the most recent. By evaluating stellar evolution across this extensive grid, we show that the final BH mass is dictated by a fundamental bifurcation: whether a star collapses as a cool supergiant or is first stripped of its envelope to become a Wolf-Rayet (WR) star. If a star enters the WR stage, its strong thick winds dominate, making the final mass sensitive to the WR wind prescription while largely erasing the memory of its prior mass-loss history. Conversely, stars that face core collapse as supergiants form significantly more massive BHs, producing a mass peak around an initial mass of 40 $M_\odot$. Rather than simply reproducing these divergent outcomes, our comprehensive evaluation demonstrates that this bifurcation is universally controlled by the highly uncertain mass loss during the cool supergiant phase. This framework strongly constrains the problem of BH mass prediction by identifying two key bottlenecks for future studies: envelope stripping efficiency and WR mass-loss rates. Our atlas provides a clear baseline for interpreting current theoretical discrepancies and testing wind models against observational constraints, such as the Galactic WR/OB population ratio.

Figures

Figures reproduced from arXiv: 2607.26147 by the authors.

**Figure 1.** — 𝑀BH as a function of 𝑀ZAMS for our models. The mass range of Cygnus X-1 BH (Ramachandran et al. 2025) in grey. The left figure represents a zoomed-in plot within 𝑀ZAMS = 55 𝑀⊙. The production of massive BHs at 𝑀ZAMS ≲ 50 𝑀⊙ is only achievable with weak mass loss during the cool supergiant regime (FEScRSG, MScRSG, KABS models). Only models that considerably underestimate H-free WR mass-loss rates (FEScnoHpoor) can … view at source ↗

**Figure 2.** shows the evolution of a FESc 40 𝑀⊙ star under different𝑇eff,trans values. If cool supergiant winds are restricted to RSGs (𝑇eff,trans ∼ 4 kK), the time spent in this phase (Δ𝑡cool) is negligible, and the star collapses into a massive BH of 28.6 𝑀⊙. Increasing the threshold by just 0.5 kK to 4.5 kK initiates a brief cool supergiant phase (0.026 Myr) that is sufficient to lower 𝑀BH by nearly 5 𝑀⊙. Once 𝑇eff,trans is … view at source ↗

**Figure 3.** shows these transition ages, normalized by the stellar lifetime, as a function of 𝑀ZAMS, as well as the 𝑀ZAMS range at which selected models present a transition beyond the HD limit (log 𝐿 ≥ 5.5 and 10−5 × 𝑅 × √ 𝐿 ≥ 1), where we distinguish on whether the stars remain for an amount of time in their LBV phase (𝑡LBV), which we stress remains unmodeled in our analysis, that is more or less than 5% of their total lifeti… view at source ↗

Figures from the paper (13 more)

**Figure 4.** Figure 4: — Comparison between empirical Galactic observations and our synthetic populations of 𝑀ZAMS ≥ 50 M⊙ VMSs scaled to 10% of the Galactic thin disk mass. The synthetic datasets account for both single stars and binary components that successfully avoid mass transfer throu…

**Figure 5.** Figure 5: shows the HR evolution of each track, while Figure 6 displays the contribution of each mass loss scheme for a specific model, both in terms of the cumulative time a star spends in each wind phase, and in terms of the cumulative mass that was lost due to specific mass-…

**Figure 6.** Figure 6: — Cumulative time and mass loss from each wind scheme for a 𝑀ZAMS = 20 𝑀⊙ star at 𝑍⊙, according to each proposed evolutionary model. On the top plot, we cut the cumulative time plot to enhance the visualization of the whole evolution. Despite the relatively short time …

**Figure 7.** Figure 7: shows the HR evolution of a 40 𝑀⊙ star following our evolutionary models [PITH_FULL_IMAGE:figures/full_fig_p011_7.png]

**Figure 8.** Figure 8: — Cumulative time and mass loss from each wind scheme for a 𝑀ZAMS = 40 𝑀⊙ star at 𝑍⊙, according to each proposed evolutionary model [PITH_FULL_IMAGE:figures/full_fig_p011_8.png]

**Figure 9.** Figure 9: — Cumulative time and mass loss from each wind scheme for a 𝑀ZAMS = 75 𝑀⊙ star at 𝑍⊙, according to each proposed evolutionary model. The major contributors are the optically thin and thick winds. 1 R 1 0 R 1 0 0 R 1 0 0 0 R 5.50 5.25 5.00 4.75 4.50 4.25 4.00 3.75 log(T…

**Figure 10.** Figure 10: — HR diagram for 𝑀ZAMS = 75 𝑀⊙ stars at 𝑍⊙. Black dots represent TAMS positions, with the respective surface-H abundances. There is considerable evolutionary variability as a function of different mass-loss rates for optically thin and H-free WR winds. with roughly 1…

**Figure 11.** Figure 11: — [PITH_FULL_IMAGE:figures/full_fig_p013_11.png]

**Figure 12.** Figure 12: — HR diagram for 𝑀ZAMS = 300 𝑀⊙ stars at 𝑍⊙. The colors representing each model remain the same as in [PITH_FULL_IMAGE:figures/full_fig_p013_12.png]

**Figure 14.** Figure 14: — The main evolutionary channels for BH progenitors. 𝑀BH is determined by a key bifurcation: stars that collapse as cool supergiants form higher-mass BHs, while those that evolve as WR stars lose more mass and form lower-mass remnants. The full single black line repre…

**Figure 15.** Figure 15: — HR evolution of a 75 𝑀⊙ star at 𝑍⊙ following the FESc model and the FEScV01. The colorbar represents the evolution of Γe. Black lines are plotted under the stellar tracks’ scatter points to increase contrast. The red ravioli represent where Γe increases past the 0.5…

**Figure 16.** Figure 16: — Fraction of 𝑀ZAMS lost with a specific wind scheme as a function of 𝑀ZAMS. The gray color is the remnant mass fraction, with the dashed white and dash-dotted aqua lines respectively the final core and envelope mass fractions. Top left: FESc model. Top center: MSc. T…

**Figure 17.** Figure 17: — Same as [PITH_FULL_IMAGE:figures/full_fig_p020_17.png]

Discussion (0). Sign in to comment.

Reference graph

Works this paper leans on

299 extracted references · 21 canonical work pages

[1]

The -slow regime

Analytical solutions for radiation-driven winds in massive stars - II. The -slow regime. MNRAS , keywords =. doi:10.1093/mnras/stab995 , archivePrefix =. 2104.03263 , primaryClass =

arXiv
[2]

, keywords =

Unveiling the Cygnus OB2 stellar population with Chandra. , keywords =. doi:10.1051/0004-6361:20066101 , archivePrefix =. astro-ph/0610352 , primaryClass =

arXiv
[3]

ApJ , keywords =

The Impact of Realistic Red Supergiant Mass Loss on Stellar Evolution. ApJ , keywords =. doi:10.3847/1538-4357/ac2574 , archivePrefix =. 2109.03239 , primaryClass =

arXiv
[4]

MNRAS , keywords =

Correction to: 'A new mass-loss rate prescription for red supergiants'. MNRAS , keywords =. doi:10.1093/mnras/stad1818 , adsurl =

work page doi:10.1093/mnras/stad1818
[5]

ApJ , keywords =

Evolution of Galaxy Star Formation and Metallicity: Impact on Double Compact Object Mergers. ApJ , keywords =. doi:10.3847/1538-4357/abd3a0 , archivePrefix =. 2012.02800 , primaryClass =

arXiv 2012
[6]

arXiv e-prints , keywords =

Metal-poor single Wolf-Rayet stars: the interplay of optically thick winds and rotation. arXiv e-prints , keywords =. doi:10.48550/arXiv.2507.00137 , archivePrefix =. 2507.00137 , primaryClass =

work page doi:10.48550/arxiv.2507.00137
[7]

arXiv e-prints , keywords =

Can current models predict the local black hole merger rate?. arXiv e-prints , keywords =. doi:10.48550/arXiv.2606.02725 , archivePrefix =. 2606.02725 , primaryClass =

arXiv doi:10.48550/arxiv.2606.02725
[8]

Nature , year=

Identification of Cygnus X-1 with HDE 226868 , author=. Nature , year=

Show all 299 references

[9]

A&A , keywords =

Lower mass loss rates in O-type stars: Spectral signatures of dense clumps in the wind of two Galactic O4 stars. A&A , keywords =. doi:10.1051/0004-6361:20042531 , archivePrefix =. astro-ph/0412346 , primaryClass =

arXiv
[10]

10.1051/0004-6361/201220798

Massive stars at low metallicity - Evolution and surface abundances of O dwarfs in the SMC⋆⋆⋆ , DOI= "10.1051/0004-6361/201220798", url= "https://doi.org/10.1051/0004-6361/201220798", journal =

doi
[11]

Branchesi, Marica and Maggiore, Michele and Alonso, David and Badger, Charles and Banerjee, Biswajit and Beirnaert, Freija and Belgacem, Enis and Bhagwat, Swetha and Boileau, Guillaume and Borhanian, Ssohrab and Brown, Daniel David and Leong Chan, Man and Cusin, Giulia and Dan...

2023
[12]

Evolution of Massive Main-sequence Stars in Rapid Population Synthesis. I. Framework and Implementation. , keywords =. doi:10.3847/1538-4357/ae5b76 , archivePrefix =. 2512.13838 , primaryClass =

arXiv
[13]

, keywords =

Explosions of pulsating red supergiants: A natural pathway for the diversity of Type II-P/L supernovae. , keywords =. doi:10.1051/0004-6361/202554642 , archivePrefix =. 2508.11077 , primaryClass =
[14]

, keywords =

A Scenario for a Large Number of Low-Mass Black Holes in the Galaxy. , keywords =. doi:10.1086/173844 , adsurl =

doi
[15]

arXiv e-prints , keywords =

Cosmic Explorer: A Submission to the NSF MPSAC ngGW Subcommittee. arXiv e-prints , keywords =. doi:10.48550/arXiv.2306.13745 , archivePrefix =. 2306.13745 , primaryClass =

doi arXiv
[16]

, keywords =

Circumbinary exoplanets and brown dwarfs with the Laser Interferometer Space Antenna. , keywords =. doi:10.1051/0004-6361/201936729 , archivePrefix =. 1910.05414 , primaryClass =

1910 arXiv
[17]

Determination of a new mass-loss rate prescription for red supergiants

ALMA detection of CO rotational line emission in red supergiant stars of the massive young star cluster RSGC1. Determination of a new mass-loss rate prescription for red supergiants. A&A , keywords =. doi:10.1051/0004-6361/202244635 , archivePrefix =. 2303.09385 , primaryClass =

arXiv
[18]

, keywords =

Merging black holes in young star clusters. , keywords =. doi:10.1093/mnras/stz1453 , archivePrefix =. 1901.00863 , primaryClass =

1901 arXiv
[19]

, keywords =

Binary black holes in the pair instability mass gap. , keywords =. doi:10.1093/mnras/staa1997 , archivePrefix =. 1911.01434 , primaryClass =

1911 arXiv
[20]

Double Compact Objects. I. The Significance of the Common Envelope on Merger Rates. ApJ , keywords =. doi:10.1088/0004-637X/759/1/52 , archivePrefix =. 1202.4901 , primaryClass =

arXiv
[21]

Double Compact Objects. II. Cosmological Merger Rates. ApJ , keywords =. doi:10.1088/0004-637X/779/1/72 , archivePrefix =. 1308.1546 , primaryClass =

arXiv
[22]

Science , keywords =

An observed population of intermediate-mass helium stars that have been stripped in binaries. Science , keywords =. doi:10.1126/science.ade4970 , archivePrefix =. 2307.00061 , primaryClass =

arXiv
[23]

, keywords =

The Science of the Einstein Telescope. , keywords =. doi:10.1088/1475-7516/2026/03/081 , archivePrefix =. 2503.12263 , primaryClass =

2026 arXiv
[24]

, keywords =

Mass ejection in failed supernovae: variation with stellar progenitor. , keywords =. doi:10.1093/mnras/sty306 , archivePrefix =. 1710.01735 , primaryClass =

arXiv
[25]

, keywords =

Merging black hole binaries: the effects of progenitor's metallicity, mass-loss rate and Eddington factor. , keywords =. doi:10.1093/mnras/stx2933 , archivePrefix =. 1711.03556 , primaryClass =

arXiv
[26]

MNRAS , keywords =

The excess of cool supergiants from contemporary stellar evolution models defies the metallicity-independent Humphreys-Davidson limit. MNRAS , keywords =. doi:10.1093/mnras/stab383 , archivePrefix =. 2102.03102 , primaryClass =

arXiv
[27]

2024 , eprint=

Gaia BH1 and BH2 -- Evolutionary Models with Overshooting of the Black Hole Progenitors within the Present-Day Binary Separation , author=. 2024 , eprint=

2024
[28]

, keywords =

The landscape of binary core-collapse supernova progenitors and the late emergence of Wolf Rayet winds. , keywords =. doi:10.1093/mnras/staf884 , archivePrefix =. 2503.01993 , primaryClass =

arXiv
[29]

2026 , eprint=

Hot blue progenitors of stellar-mass black holes , author=. 2026 , eprint=

2026
[30]

, keywords =

The wind speeds, dust content, and mass-loss rates of evolved AGB and RSG stars at varying metallicity. , keywords =. doi:10.1093/mnras/stw2708 , archivePrefix =. 1610.05761 , primaryClass =

arXiv
[31]

Modelling for interferometric observations , volume=

The effect of winds on atmospheric layers of red supergiants: I. Modelling for interferometric observations , volume=. 2023 , month=jan, pages=. doi:10.1051/0004-6361/202244503 , journal=

2023 doi
[32]

Modelling VLTI/GRAVITY and MATISSE observations of AH Sco, KW Sgr, V602 Car, CK Car, and V460 Car

The effect of winds on atmospheric layers of red supergiants II. Modelling VLTI/GRAVITY and MATISSE observations of AH Sco, KW Sgr, V602 Car, CK Car, and V460 Car. A&A , keywords =. doi:10.1051/0004-6361/202348047 , archivePrefix =. 2312.12521 , primaryClass =

arXiv
[33]

A\ keywords =

Spectral models for binary products: Unifying subdwarfs and Wolf-Rayet stars as a sequence of stripped-envelope stars. A\ keywords =. doi:10.1051/0004-6361/201732274 , archivePrefix =. 1802.03018 , primaryClass =

arXiv
[34]

ApJ , keywords =

Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds. ApJ , keywords =. doi:10.3847/1538-4357/ace5a3 , archivePrefix =. 2307.00074 , primaryClass =

arXiv
[35]

, keywords =

Wind-envelope interaction as the origin of the slow cyclic brightness variations of luminous blue variables. , keywords =. doi:10.1051/0004-6361/202038298 , archivePrefix =. 2012.00023 , primaryClass =

2012 arXiv
[36]

Dynamic model atmospheres of AGB stars. III. Effects of frequency-dependent radiative transfer. , keywords =. doi:10.1051/0004-6361:20021757 , adsurl =

doi
[37]

Mechanisms, models and measurements

Mass loss of stars on the asymptotic giant branch. Mechanisms, models and measurements. , keywords =. doi:10.1007/s00159-017-0106-5 , adsurl =

doi
[38]

PASJ , keywords =

Core-Halo Structure of a Chemically Homogeneous Massive Star and Bending of the Zero-Age Main Sequence. PASJ , keywords =. doi:10.1093/pasj/51.4.417 , archivePrefix =. astro-ph/9907154 , primaryClass =

arXiv
[39]

ApJl , keywords =

Ultraluminous X-Ray Sources in External Galaxies. ApJl , keywords =. doi:10.1086/320343 , archivePrefix =. astro-ph/0104333 , primaryClass =

arXiv
[40]

A&A , keywords =

Massive donors in interacting binaries: effect of metallicity. A&A , keywords =. doi:10.1051/0004-6361/202037694 , archivePrefix =. 2004.00628 , primaryClass =

2004 arXiv
[41]

10.1051/0004-6361/202038707

It has to be cool: Supergiant progenitors of binary black hole mergers from common-envelope evolution , DOI= "10.1051/0004-6361/202038707", url= "https://doi.org/10.1051/0004-6361/202038707", journal =

doi
[42]

A&A , keywords =

Partial-envelope stripping and nuclear-timescale mass transfer from evolved supergiants at low metallicity. A&A , keywords =. doi:10.1051/0004-6361/202142701 , archivePrefix =. 2111.10271 , primaryClass =

arXiv
[43]

, keywords =

Comfort zones of stars: A limit on orbital tightening via stable mass transfer shapes the properties of binary black hole mergers. , keywords =. doi:10.1051/0004-6361/202555500 , archivePrefix =. 2505.08860 , primaryClass =
[44]

A&A , keywords =

Semiconvective diffusion and energy transport. A&A , keywords =
[45]

, keywords =

The surface temperature of C/O-rich Wolf-Rayet stars. , keywords =
[46]

, keywords =

Mass-dependent mass loss rates of Wolf-Rayet stars. , keywords =
[47]

Luminous Blue Variables: Massive Stars in Transition , year = 1997, editor =

The Eddington Limit in Rotating Massive Stars. Luminous Blue Variables: Massive Stars in Transition , year = 1997, editor =

1997
[48]

A&A , keywords =

Coupled mass and angular momentum loss of massive main sequence stars. A&A , keywords =
[49]

ARAA , keywords =

Presupernova Evolution of Massive Single and Binary Stars. ARAA , keywords =. doi:10.1146/annurev-astro-081811-125534 , archivePrefix =. 1206.5443 , primaryClass =

arXiv
[50]

10.1051/0004-6361/201937300

The expansion of stripped-envelope stars: Consequences for supernovae and gravitational-wave progenitors , DOI= "10.1051/0004-6361/201937300", url= "https://doi.org/10.1051/0004-6361/201937300", journal =

doi
[51]

, keywords =

Pulsations Change the Structures of Massive Stars before Explosion: Interpreting SN 2023ixf and SN 2024ggi. , keywords =. doi:10.3847/2041-8213/ae3d2e , archivePrefix =. 2508.11088 , primaryClass =
[52]

de Laplace, P.S. , url=. Exposition Du Syst. 1809 , publisher=
[53]

arXiv e-prints , keywords =

From cosmological simulations to binary black hole mergers: The impact of using analytical star formation history models on gravitational-wave source populations. arXiv e-prints , keywords =. doi:10.48550/arXiv.2601.20202 , archivePrefix =. 2601.20202 , primaryClass =

doi
[54]

, keywords =

Very Low Energy Supernovae from Neutrino Mass Loss. , keywords =. doi:10.1088/0004-637X/769/2/109 , archivePrefix =. 1303.5055 , primaryClass =

arXiv
[55]

ApJ , keywords =

Impact of the Rotation and Compactness of Progenitors on the Mass of Black Holes. ApJ , keywords =. doi:10.3847/1538-4357/ab584d , archivePrefix =. 1909.01371 , primaryClass =

1909 arXiv
[56]

Handbook of Gravitational Wave Astronomy

Formation Channels of Single and Binary Stellar-Mass Black Holes. Handbook of Gravitational Wave Astronomy. Edited by C. Bambi , year = 2021, eid =. doi:10.1007/978-981-15-4702-7\_16-1 , adsurl =

2021 doi
[57]

arXiv e-prints , keywords =

The role of accretion efficiency, natal kicks, and angular momentum transport in the formation of the Gaia black holes. arXiv e-prints , keywords =. doi:10.48550/arXiv.2604.12839 , archivePrefix =. 2604.12839 , primaryClass =

doi arXiv
[58]

Turbulent Convection in Stellar Interiors. I. Hydrodynamic Simulation. ApJ , keywords =. doi:10.1086/520318 , archivePrefix =. astro-ph/0611315 , primaryClass =

arXiv
[59]

arXiv e-prints , keywords =

Implications of modern mass-loss rates for massive stars. arXiv e-prints , keywords =. doi:10.48550/arXiv.2507.17052 , archivePrefix =. 2507.17052 , primaryClass =

doi arXiv
[60]

, keywords =

Tight asteroseismic constraints on core overshooting and diffusive mixing in the slowly rotating pulsating B8.3V star KIC 10526294. , keywords =. doi:10.1051/0004-6361/201425290 , archivePrefix =. 1505.06902 , primaryClass =

arXiv
[61]

, keywords =

Sub-inertial Gravity Modes in the B8V Star KIC 7760680 Reveal Moderate Core Overshooting and Low Vertical Diffusive Mixing. , keywords =. doi:10.3847/0004-637X/823/2/130 , archivePrefix =. 1604.02680 , primaryClass =

arXiv
[62]

A&A , keywords =

Predictions of the effect of clumping on the wind properties of O-type stars. A&A , keywords =. doi:10.1051/0004-6361/201014290 , adsurl =

doi
[63]

, keywords =

Some Secondary Indications of Gravitational Collapse. , keywords =. doi:10.1007/BF00638971 , adsurl =

doi
[64]

10.1051/0004-6361/202554162

Spindown of massive single main sequence stars in the Milky Way , DOI= "10.1051/0004-6361/202554162", url= "https://doi.org/10.1051/0004-6361/202554162", journal =

doi
[65]

, keywords =

Population synthesis of Thorne- \.Z ytkow objects: Rejuvenated donors and unexplored progenitors in the common envelope formation channel. , keywords =. doi:10.1051/0004-6361/202451531 , archivePrefix =. 2407.11680 , primaryClass =

arXiv
[66]

A&A , keywords =

The earliest O-type eclipsing binary in the Small Magellanic Cloud, AzV 476: A comprehensive analysis reveals surprisingly low stellar masses. A&A , keywords =. doi:10.1051/0004-6361/202141738 , archivePrefix =. 2201.09148 , primaryClass =

arXiv
[67]

, keywords =

New empirical mass-loss recipe for UV radiation line-driven winds of hot stars across various metallicities. , keywords =. doi:10.1051/0004-6361/202553910 , archivePrefix =. 2504.07073 , primaryClass =

arXiv
[68]

, keywords =

The drastic impact of Eddington-limit induced mass ejections on massive star populations. , keywords =. doi:10.1051/0004-6361/202557766 , archivePrefix =. 2601.08822 , primaryClass =
[69]

Monthly Notices of the Royal Astronomical Society , volume =

Was the nineteenth century giant eruption of Eta Carinae a merger event in a triple system?. Monthly Notices of the Royal Astronomical Society , volume =. 2016 , month =. doi:10.1093/mnras/stv2787 , url =

2016 doi
[70]

ApJl , keywords =

Black Hole Mergers in the Universe. ApJl , keywords =. doi:10.1086/312422 , archivePrefix =. astro-ph/9910061 , primaryClass =

arXiv
[71]

Radiation-driven winds of hot luminous stars. IV. The influence of multi-line effects. A&A , keywords =
[72]

, keywords =

O-star mass-loss and wind momentum rates in the Galaxy and the Magellanic Clouds Observations and theoretical predictions. , keywords =
[73]

Radiation driven winds of hot luminous stars. XIV. Line statistics and radiative driving. A&As , keywords =. doi:10.1051/aas:2000312 , adsurl =

doi
[74]

Atmospheric NLTE-models for the spectroscopic analysis of blue stars with winds. II. Line-blanketed models. A&A , eprint =. doi:10.1051/0004-6361:20042365 , adsurl =

doi
[75]

Astronomy and Astrophysics Review , keywords =

Mass loss from hot massive stars. Astronomy and Astrophysics Review , keywords =. doi:10.1007/s00159-008-0015-8 , archivePrefix =. 0811.0487 , adsurl =

arXiv
[76]

, keywords =

Comprehensive UV and optical spectral analysis of Cygnus X-1: Stellar and wind parameters, abundances, and evolutionary implications. , keywords =. doi:10.1051/0004-6361/202554184 , archivePrefix =. 2504.05885 , primaryClass =

arXiv
[77]

Spectroscopic analysis of OB stars in the SMC Wing

Testing massive star evolution, star formation history, and feedback at low metallicity. Spectroscopic analysis of OB stars in the SMC Wing. , keywords =. doi:10.1051/0004-6361/201935365 , archivePrefix =. 1903.01762 , primaryClass =

1903 arXiv
[78]

10.1051/0004-6361/201731093

Stellar population of the superbubble N206 in the LMC - I. Analysis of the Of-type stars , DOI= "10.1051/0004-6361/201731093", url= "https://doi.org/10.1051/0004-6361/201731093", journal =

doi
[79]

10.1051/0004-6361/201832816

Stellar population of the superbubble N 206 in the LMC - II. Parameters of the OB and WR stars, and the total massive star feedback , DOI= "10.1051/0004-6361/201832816", url= "https://doi.org/10.1051/0004-6361/201832816", journal =

doi
[80]

, keywords =

The mass dependence of the overshooting parameter determined from eclipsing binary data. , keywords =. doi:10.1046/j.1365-8711.2000.04035.x , adsurl =
[81]

A&A , keywords =

Convection and stellar structure. A&A , keywords =
[82]

A&A , keywords =

Integral constraints on convective overshooting. A&A , keywords =
[83]

Modeling the Evolution of Disk Galaxies. II. Yields of Massive Stars. , keywords =. doi:10.1086/305368 , adsurl =

doi
[84]

ApJ , year = 1965, month = nov, volume =

Overshooting from Stellar Convective Cores. ApJ , year = 1965, month = nov, volume =. doi:10.1086/148430 , adsurl =

1965 doi
[85]

Journal for the History of Astronomy , year = 1979, month = jan, volume =

John Michell and Black Holes. Journal for the History of Astronomy , year = 1979, month = jan, volume =. doi:10.1177/002182867901000104 , adsurl =

1979 doi
[86]

, keywords =

Dance to Demise How Massive Stars May Form Dense Circumstellar Shells before Explosion. , keywords =. doi:10.3847/1538-4357/ae129c , archivePrefix =. 2508.04497 , primaryClass =
[87]

ApJ , year = 1973, month = aug, volume =

Convective Overshooting in Stellar Interior Models. ApJ , year = 1973, month = aug, volume =. doi:10.1086/152318 , adsurl =

1973 doi
[88]

10.1051/0004-6361/201527916

Wolf-Rayet stars in the Small Magellanic Cloud - II. Analysis of the binaries , DOI= "10.1051/0004-6361/201527916", url= "https://doi.org/10.1051/0004-6361/201527916", journal =

doi
[89]

Analysis of the binaries , author=

Wolf-Rayet stars in the Small Magellanic Cloud: II. Analysis of the binaries , author=. arXiv: Solar and Stellar Astrophysics , year=
[90]

Astronomy & Astrophysics , year=

The Wolf-Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud , author=. Astronomy & Astrophysics , year=
[91]

Spectroscopy, orbital analysis, formation, and evolution (Corrigendum)

The Wolf-Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud. Spectroscopy, orbital analysis, formation, and evolution (Corrigendum). A&A , keywords =. doi:10.1051/0004-6361/201935684e , adsurl =

doi
[92]

, keywords =

Why binary interaction does not necessarily dominate the formation of Wolf-Rayet stars at low metallicity. , keywords =. doi:10.1051/0004-6361/201936948 , archivePrefix =. 2001.04476 , primaryClass =

2001 arXiv
[93]

The Tarantula Massive Binary Monitoring. V. R 144: a wind-eclipsing binary with a total mass 140 M _. A&A , keywords =. doi:10.1051/0004-6361/202140693 , archivePrefix =. 2104.03323 , primaryClass =

arXiv
[94]

The Tarantula Massive Binary Monitoring. VI. Characterisation of hidden companions in 51 single-lined O-type binaries: A flat mass-ratio distribution and black-hole binary candidates. A&A , keywords =. doi:10.1051/0004-6361/202244245 , archivePrefix =. 2207.07674 , primaryClass =

arXiv
[95]

Nature Astronomy , keywords =

An X-ray-quiet black hole born with a negligible kick in a massive binary within the Large Magellanic Cloud. Nature Astronomy , keywords =. doi:10.1038/s41550-022-01730-y , archivePrefix =. 2207.07675 , primaryClass =

arXiv
[96]

arXiv e-prints , keywords =

Wolf-Rayet stars. arXiv e-prints , keywords =. doi:10.48550/arXiv.2410.04436 , archivePrefix =. 2410.04436 , primaryClass =

doi arXiv
[97]

, keywords =

Evolution of the Convective Core Mass during the Main Sequence. , keywords =. doi:10.3847/1538-4357/adc5fa , archivePrefix =. 2409.00460 , primaryClass =

arXiv
[98]

Astronomy Reports , year = 2013, month = may, volume =

Turbulent entrainment at the boundaries of the convective cores of main-sequence stars. Astronomy Reports , year = 2013, month = may, volume =. doi:10.1134/S1063772913050089 , adsurl =

2013 doi
[99]

Atmospheric NLTE models for the spectroscopic analysis of blue stars with winds. IV. Porosity in physical and velocity space. A&A , keywords =. doi:10.1051/0004-6361/201832993 , archivePrefix =. 1805.11010 , primaryClass =

arXiv
[100]

New predictions for radiation-driven, steady-state mass-loss and wind-momentum from hot, massive stars. I. Method and first results. A&A , keywords =. doi:10.1051/0004-6361/201936580 , archivePrefix =. 1910.06586 , primaryClass =

1910 arXiv
[101]

, keywords =

An on-the-fly line-driven wind iterative mass-loss estimator (LIME) for hot, massive stars of arbitrary chemical compositions. , keywords =. doi:10.1051/0004-6361/202554940 , archivePrefix =. 2504.00936 , primaryClass =
[102]

Three-dimensional radiative transfer in clumped hot star winds. I. Influence of clumping on the resonance line formation. A&A , keywords =. doi:10.1051/0004-6361/201118590 , archivePrefix =. 1202.4787 , primaryClass =

arXiv
[103]

A&A , keywords =

Macroclumping as solution of the discrepancy between H and P v mass loss diagnostics for O-type stars. A&A , keywords =. doi:10.1051/0004-6361/201322390 , archivePrefix =. 1310.0449 , primaryClass =

arXiv
[104]

, keywords =

Radial pulsation runaway in massive red supergiants in late evolutionary stage and implications to hydrogen-rich supernovae. , keywords =. doi:10.1093/mnras/staf1603 , archivePrefix =. 2509.14928 , primaryClass =
[105]

ApJ , keywords =

The MAVERIC Survey: Still No Evidence for Accreting Intermediate-mass Black Holes in Globular Clusters. ApJ , keywords =. doi:10.3847/1538-4357/aac9b9 , archivePrefix =. 1806.00259 , primaryClass =

arXiv
[106]

, keywords =

The initial mass-remnant mass relation for core collapse supernovae. , keywords =. doi:10.1051/0004-6361/202451483 , archivePrefix =. 2501.18689 , primaryClass =

arXiv
[107]

High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , year = 2019, editor =

High-Mass X-ray Binaries: progenitors of double compact objects. High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , year = 2019, editor =. doi:10.1017/S1743921319001315 , archivePrefix =. 1901.06939 , primaryClass =

2019 arXiv
[108]

10.1051/0004-6361:20042555

An empirical formula for the mass-loss rates of dust-enshrouded red supergiants and oxygen-rich Asymptotic Giant Branch stars , DOI= "10.1051/0004-6361:20042555", url= "https://doi.org/10.1051/0004-6361:20042555", journal =

doi
[109]

Galaxies , keywords =

Red Supergiant Mass Loss and Mass-Loss Rates. Galaxies , keywords =. doi:10.3390/galaxies13040072 , archivePrefix =. 2507.15971 , primaryClass =

arXiv
[110]

, year = 1972, month = jan, volume =

Cygnus X-1-a Spectroscopic Binary with a Heavy Companion ?. , year = 1972, month = jan, volume =. doi:10.1038/235037a0 , adsurl =

1972 doi
[111]

A&A , keywords =

Convective penetration in stellar interiors. A&A , keywords =
[112]

A&A , keywords =

Circulation and turbulence in rotating stars. A&A , keywords =
[113]

A&A , keywords =

A comparison between observed Algol-type double stars in the solar neighborhood and evolutionary computations of galactic case A binaries with a B-type primary at birth. A&A , keywords =. doi:10.1051/0004-6361/201630131 , archivePrefix =. 1611.08398 , primaryClass =

arXiv
[114]

arXiv", primaryClass =

Massive double compact object mergers: gravitational wave sources and r-process element production sites. A&A , archivePrefix = "arXiv", primaryClass = "astro-ph.SR", keywords =. doi:10.1051/0004-6361/201322198 , adsnote =

doi
[115]

The role of overshoot in DA white dwarfs, A-type stars, and the Sun

Hydrodynamical models of stellar convection. The role of overshoot in DA white dwarfs, A-type stars, and the Sun. A&A , keywords =
[116]

Effects of convection and radial pulsations on atmospheric structures

Global 3D radiation-hydrodynamics models of AGB stars. Effects of convection and radial pulsations on atmospheric structures. , keywords =. doi:10.1051/0004-6361/201629594 , archivePrefix =. 1702.05433 , primaryClass =

arXiv
[117]

ApJ , keywords =

Stellar evolution at high mass including the effect of a stellar wind. ApJ , keywords =. doi:10.1086/157388 , adsurl =

doi
[118]

A&A , keywords =

Stellar evolution III: the overshooting from convective cores. A&A , keywords =
[119]

Evolution of chemical abundances in massive stars. I. OB stars, Hubble-Sandage variables and Wolf-Rayet stars. Changes at stellar surfaces and galactic enrichment by stellar winds. , keywords =
[120]

A&A , keywords =

Grids of evolutionary models of massive stars with mass loss and overshooting - Properties of Wolf-Rayet stars sensitive to overshooting. A&A , keywords =
[121]

A\ keywords =

Grids of evolutionary models from 0.85 to 120M : observational tests and the mass limits. A\ keywords =
[122]

, keywords =

New models of Wolf-Rayet stars and comparison with data in galaxies. , keywords =
[123]

Stellar evolution with rotation. III. Meridional circulation with MU -gradients and non-stationarity. A&A , keywords =
[124]

Annual Review of Astronomy and Astrophysics , volume =

Maeder, André and Maeynet, Georges , title =. Annual Review of Astronomy and Astrophysics , volume =. 2000 , doi =

2000
[125]

Stellar evolution with rotation and magnetic fields. II. General equations for the transport by Tayler-Spruit dynamo. A&A , keywords =. doi:10.1051/0004-6361:20034583 , archivePrefix =. astro-ph/0404417 , primaryClass =

arXiv
[126]

arXiv e-prints , keywords =

The impact of convective criteria on the properties of massive stars. arXiv e-prints , keywords =. doi:10.48550/arXiv.2310.18139 , archivePrefix =. 2310.18139 , primaryClass =

doi arXiv
[127]

arXiv e-prints , keywords =

Grids of stellar models with rotation VIII: Models from 1.7 to 500 M_ at metallicity Z = 10^ -5. arXiv e-prints , keywords =. doi:10.48550/arXiv.2407.06739 , archivePrefix =. 2407.06739 , primaryClass =

doi arXiv
[128]

MNRAS , keywords =

Very massive stars and pair-instability supernovae: mass-loss framework for low metallicity. MNRAS , keywords =. doi:10.1093/mnras/stad1888 , archivePrefix =. 2306.11785 , primaryClass =

arXiv
[129]

, keywords =

On stars with weak winds: the Galactic case. , keywords =. doi:10.1051/0004-6361:20052927 , archivePrefix =. astro-ph/0507278 , primaryClass =

arXiv
[130]

A&A , keywords =

The most massive stars in the Arches cluster. A&A , keywords =. doi:10.1051/0004-6361:20078469 , archivePrefix =. 0711.0657 , primaryClass =

arXiv
[131]

A&A , keywords =

Spectroscopic evolution of very massive stars at Z = 1/2.5 Z _. A&A , keywords =. doi:10.1051/0004-6361/202243048 , archivePrefix =. 2202.13703 , primaryClass =

arXiv
[132]

A&A , keywords =

Surface chemical composition of single WNh stars. A&A , keywords =. doi:10.1051/0004-6361/202347909 , archivePrefix =. 2310.06539 , primaryClass =

arXiv
[133]

Effect of metallicity on surface abundances of O stars

X-Shooting ULLYSES: Massive stars at low metallicity: V. Effect of metallicity on surface abundances of O stars. , keywords =. doi:10.1051/0004-6361/202449457 , archivePrefix =. 2405.01267 , primaryClass =

arXiv
[134]

New predictions for radiation-driven, steady-state mass-loss and wind-momentum from hot, massive stars. II. A grid of O-type stars in the Galaxy and the Magellanic Clouds. A&A , keywords =. doi:10.1051/0004-6361/202038384 , archivePrefix =. 2008.06066 , primaryClass =

2008 arXiv
[135]

New predictions for radiation-driven, steady-state mass-loss and wind-momentum from hot, massive stars. III. Updated mass-loss rates for stellar evolution. A&A , keywords =. doi:10.1051/0004-6361/202141948 , archivePrefix =. 2203.08218 , primaryClass =

arXiv
[136]

, keywords =

The winds of hot massive first stars. , keywords =. doi:10.1051/0004-6361:20053289 , archivePrefix =. astro-ph/0509171 , primaryClass =

arXiv
[137]

, keywords =

CNO-driven winds of hot first stars. , keywords =. doi:10.1051/0004-6361:200810208 , archivePrefix =. 0810.2973 , primaryClass =

arXiv
[138]

arXiv e-prints , keywords =

New line-driven wind mass-loss rates for OB stars with metallicities down to 0.01\,Z_. arXiv e-prints , keywords =. doi:10.48550/arXiv.2508.21702 , archivePrefix =. 2508.21702 , primaryClass =

doi arXiv
[139]

, keywords =

New mass-loss rates of Magellanic Cloud B supergiants from global wind models. , keywords =. doi:10.1051/0004-6361/202347916 , archivePrefix =. 2311.01257 , primaryClass =

arXiv
[140]

Comoving frame models of hot star winds. II. Reduction of O star wind mass-loss rates in global models. A&A , keywords =. doi:10.1051/0004-6361/201730723 , archivePrefix =. 1706.06194 , primaryClass =

arXiv
[141]

A&A , keywords =

New mass-loss rates of B supergiants from global wind models. A&A , keywords =. doi:10.1051/0004-6361/202039900 , archivePrefix =. 2101.04973 , primaryClass =

arXiv
[142]

A&A , keywords =

Global hot-star wind models for stars from Magellanic Clouds. A&A , keywords =. doi:10.1051/0004-6361/201731969 , archivePrefix =. 1712.03321 , primaryClass =

arXiv
[143]

The evolution and explosion of massive stars , author =. Rev. Mod. Phys. , volume =. 2002 , month =. doi:10.1103/RevModPhys.74.1015 , url =

2002 doi
[144]

arXiv", primaryClass =

Evolution and fate of very massive stars. MNRAS , archivePrefix = "arXiv", primaryClass = "astro-ph.SR", keywords =. doi:10.1093/mnras/stt794 , adsnote =

doi
[145]

MNRAS , keywords =

Grids of stellar models with rotation VII: models from 0.8 to 300 M _ at supersolar metallicity (Z = 0.020). MNRAS , keywords =. doi:10.1093/mnras/stac230 , archivePrefix =. 2201.08645 , primaryClass =

arXiv
[147]

, keywords =

Chemical enrichment by Wolf-Rayet stars: non-solar metallicities. , keywords =. doi:10.1046/j.1365-8711.2003.06420.x , adsurl =

2003
[148]

ApJ , archivePrefix = "arXiv", eprint =

Self-consistent Solutions for Line-driven Winds of Hot Massive Stars: The m-CAK Procedure. ApJ , archivePrefix = "arXiv", eprint =. doi:10.3847/1538-4357/ab05c4 , adsurl =

doi
[149]

ApJ , keywords =

New Hydrodynamic Solutions for Line-driven Winds of Hot Massive Stars Using the Lambert W-function. ApJ , keywords =. doi:10.3847/1538-4357/ac12c9 , archivePrefix =. 2106.15060 , primaryClass =

arXiv
[150]

A&A , keywords =

New self-consistent wind parameters to fit optical spectra of O-type stars observed with the HERMES spectrograph. A&A , keywords =. doi:10.1051/0004-6361/202142383 , archivePrefix =. 2202.08735 , primaryClass =

arXiv
[151]

A&A , keywords =

Evolution of massive stars with new hydrodynamic wind models. A&A , keywords =. doi:10.1051/0004-6361/202243959 , archivePrefix =. 2207.04786 , primaryClass =

arXiv
[152]

A&A , keywords =

Evolution of rotating massive stars with new hydrodynamic wind models. A&A , keywords =. doi:10.1051/0004-6361/202345847 , archivePrefix =. 2303.13058 , primaryClass =
[153]

, keywords =

Evolution of rotating massive stars adopting a newer, self-consistent wind prescription at Small Magellanic Cloud metallicity. , keywords =. doi:10.1051/0004-6361/202449782 , archivePrefix =. 2404.07570 , primaryClass =

arXiv
[154]

, keywords =

Evolution of stars with 60 and 200 M _ : predictions for WNh stars in the Milky Way. , keywords =. 2025 , month = apr, volume =. doi:10.1051/0004-6361/202451565 , archivePrefix =. 2407.14165 , primaryClass =

2025 arXiv
[155]

, keywords =

Revisiting the evolutionary status of massive stars in the central parsec of the Milky Way. , keywords =. doi:10.1051/0004-6361/202556877 , archivePrefix =. 2512.07432 , primaryClass =
[156]

, keywords =

A comparative study of the evolution of a close binary using a standard and an improved technique for computing mass transfer. , keywords =
[157]

, keywords =

Turning on and off mass transfer in cataclysmic binaries. , keywords =
[158]

, keywords =

Tidal evolution in close binary systems. , keywords =
[159]

arXiv e-prints , keywords =

Impact of main-sequence mass loss on the appearance, structure and evolution of Wolf-Rayet stars. arXiv e-prints , keywords =. doi:10.48550/arXiv.2404.14488 , archivePrefix =. 2404.14488 , primaryClass =

doi arXiv
[160]

X-Shooting ULLYSES: Massive stars at low metallicity. XIII. Putting the bi-stability jump to the test in the LMC. arXiv e-prints , keywords =. doi:10.48550/arXiv.2506.09129 , archivePrefix =. 2506.09129 , primaryClass =

doi
[161]

Properties of SMC late-O and B supergiants reveal the metallicity dependence of winds in the Magellanic Clouds

X-Shooting ULLYSES: Massive stars at low metallicity XIV. Properties of SMC late-O and B supergiants reveal the metallicity dependence of winds in the Magellanic Clouds. arXiv e-prints , keywords =
[162]

, keywords =

Testing a Predictive Theoretical Model for the Mass Loss Rates of Cool Stars. , keywords =. doi:10.1088/0004-637X/741/1/54 , archivePrefix =. 1108.4369 , primaryClass =

arXiv
[163]

Stellar evolution of low and intermediate-mass stars. I. Mass loss on the AGB and its consequences for stellar evolution. , keywords =
[164]

Memoires of the Societe Royale des Sciences de Liege , keywords =

Circumstellar absorption lines and mass loss from red giants. Memoires of the Societe Royale des Sciences de Liege , keywords =
[165]

On the absolute scale of mass-loss in red giants. I. Circumstellar absorption lines in the spectrum of the visual companion of alpha ^ 1 Her. A&A , keywords =
[166]

The R136 star cluster dissected with Hubble Space Telescope/STIS. III. The most massive stars and their clumped winds. A&A , keywords =. doi:10.1051/0004-6361/202142742 , archivePrefix =. 2202.11080 , primaryClass =

arXiv
[167]

arXiv e-prints , keywords =

An absence of binary companions to Wolf-Rayet stars in the Small Magellanic Cloud: implications for mass loss and black hole masses at low metallicity. arXiv e-prints , keywords =. doi:10.48550/arXiv.2406.01420 , archivePrefix =. 2406.01420 , primaryClass =

doi arXiv
[168]

, keywords =

On the evolution and fate of super-massive stars. , keywords =. doi:10.1051/0004-6361:20078345 , archivePrefix =. 0710.1181 , primaryClass =

arXiv
[169]

Elusive hot stripped helium stars in the Galaxy. I. Evolutionary stellar models in the gap between subdwarfs and Wolf-Rayet stars. A&A , keywords =. doi:10.1051/0004-6361/202347806 , adsurl =

doi
[170]

Konvektionszonen im Innern der SterneKonvektionszonen im Innern der SterneConvection zones in stellar interiors
[171]

Mit 11 Textabbildungen

Die Wasserstoffkonvektionszone der Sonne. Mit 11 Textabbildungen. ZAP , year = 1953, month = jan, volume =

1953
[172]

U ber die Wasserstoffkonvektionszone in Sternen verschiedener Effektivtemperaturen und Leuchtkr \

\"U ber die Wasserstoffkonvektionszone in Sternen verschiedener Effektivtemperaturen und Leuchtkr \"a fte. Mit 5 Textabbildungen. ZAP , year = 1958, month = jan, volume =

1958
[173]

A&A , keywords =

A model for time-dependent turbulent convection. A&A , keywords =
[174]

u r zeitabh \

Ein Modell f \"u r zeitabh \"a ngige Konvektion in Sternen
[175]

Stellar evolution models with overshooting based on 3-equation non-local theories. I. Physical basis and the computation of the dissipation rate. A&A , keywords =. doi:10.1051/0004-6361/202243125 , archivePrefix =. 2207.12296 , primaryClass =

arXiv
[176]

Bericht \"u ber Untersuchungen zur ausgebildeten Turbulenz

7. Bericht \"u ber Untersuchungen zur ausgebildeten Turbulenz. Zeitschrift Angewandte Mathematik und Mechanik , year = 1925, month = jan, volume =. doi:10.1002/zamm.19250050212 , adsurl =

1925 doi
[177]

Stellar evolution models with overshooting based on 3-equation non-local theories. II. Main-sequence models of A- and B-type stars. A&A , keywords =. doi:10.1051/0004-6361/202243126 , archivePrefix =. 2207.12512 , primaryClass =

arXiv
[178]

Fryer and S

Chris L. Fryer and S. E. Woosley and Dieter H. Hartmann , title =. The Astrophysical Journal , abstract =. 1999 , month =. doi:10.1086/307992 , url =

1999 doi
[179]

, keywords =

Impact of stellar winds on the pair-instability supernova rate. , keywords =. doi:10.1051/0004-6361/202555490 , archivePrefix =. 2505.07959 , primaryClass =

arXiv
[180]

MNRAS , keywords =

The cosmic merger rate density of compact objects: impact of star formation, metallicity, initial mass function, and binary evolution. MNRAS , keywords =. doi:10.1093/mnras/stab280 , archivePrefix =. 2009.03911 , primaryClass =

2009 arXiv
[181]

MNRAS , keywords =

Dependence of gravitational wave transient rates on cosmic star formation and metallicity evolution history. MNRAS , keywords =. doi:10.1093/mnrasl/slz183 , archivePrefix =. 1912.04474 , primaryClass =

1912 arXiv
[182]

, keywords =

The most magnetic stars. , keywords =. doi:10.1093/mnras/stt1910 , archivePrefix =. 1310.2696 , primaryClass =

arXiv
[183]

2025 , eprint=

The collision and merger products of stars do not look alike: A magnetohydrodynamics comparison , author=. 2025 , eprint=

2025
[184]

Monthly Notices of the Royal Astronomical Society , volume =

Petit, V and Wade, G A and Schneider, F R N and Fossati, L and Kamp, K and Neiner, C and David-Uraz, A and Alecian, E and the MiMeS Collaboration , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2019 , month =. doi:10.1093/mnras/stz2469 , url =

2019 doi
[185]

Oxygen- versus iron-dependent cosmic star formation history

Trading oxygen for iron II. Oxygen- versus iron-dependent cosmic star formation history. arXiv e-prints , keywords =. doi:10.48550/arXiv.2511.15782 , archivePrefix =. 2511.15782 , primaryClass =

doi arXiv
[186]

Trading oxygen for iron. I. The [O/Fe]-specific star formation rate relation of galaxies. , keywords =. doi:10.1051/0004-6361/202347602 , archivePrefix =. 2308.00023 , primaryClass =

arXiv
[187]

MNRAS , keywords =

The influence of the distribution of cosmic star formation at different metallicities on the properties of merging double compact objects. MNRAS , keywords =. doi:10.1093/mnras/sty3087 , archivePrefix =. 1811.03565 , primaryClass =

arXiv
[188]

MNRAS , keywords =

Metallicity of stars formed throughout the cosmic history based on the observational properties of star-forming galaxies. MNRAS , keywords =. doi:10.1093/mnras/stz2057 , archivePrefix =. 1907.11243 , primaryClass =

1907 arXiv
[189]

ApJ , keywords =

Observing Intermediate-mass Black Holes and the Upper Stellar-mass gap with LIGO and Virgo. ApJ , keywords =. doi:10.3847/1538-4357/ac3130 , archivePrefix =. 2105.06366 , primaryClass =

arXiv
[190]

arXiv e-prints , keywords =

pastamarkers 2: pasta sauce colormaps for your flavorful results. arXiv e-prints , keywords =. doi:10.48550/arXiv.2503.23126 , archivePrefix =. 2503.23126 , primaryClass =

doi arXiv
[191]

arXiv e-prints , keywords =

pastamarkers: astrophysical data visualization with pasta-like markers. arXiv e-prints , keywords =. doi:10.48550/arXiv.2403.20314 , archivePrefix =. 2403.20314 , primaryClass =

doi arXiv
[192]

Hunter, J. D. , Title =. Computing in Science & Engineering , Volume =
[193]

Harris and K

Charles R. Harris and K. Jarrod Millman and St. Array programming with. 2020 , month = sep, journal =. doi:10.1038/s41586-020-2649-2 , publisher =

2020 doi
[194]

doi:10.5281/zenodo.13819579 , url =

The pandas development team , title =. doi:10.5281/zenodo.13819579 , url =

doi
[195]

, title =

Van Rossum, Guido and Drake, Fred L. , title =. 2009 , isbn =

2009
[196]

arXiv e-prints , keywords =

Streamlining and standardizing software citations with The Software Citation Station. arXiv e-prints , keywords =
[197]

doi:10.5281/zenodo.13225824 , url =

Tom Wagg and Floor Broekgaarden and Kayhan Gültekin , title =. doi:10.5281/zenodo.13225824 , url =

doi
[198]

10.1051/0004-6361/202452573

Evolutionary tracks, ejecta, and ionizing photons from intermediate-mass to very massive stars with PARSEC⋆ , DOI= "10.1051/0004-6361/202452573", url= "https://doi.org/10.1051/0004-6361/202452573", journal =

doi
[199]

MNRAS , keywords =

Formation of GW190521 from stellar evolution: the impact of the hydrogen-rich envelope, dredge-up, and ^ 12 C( , ) ^ 16 O rate on the pair-instability black hole mass gap. MNRAS , keywords =. doi:10.1093/mnras/staa3916 , archivePrefix =. 2010.02242 , primaryClass =

2010 arXiv
[200]

MNRAS , keywords =

Formation of binary black holes similar to GW190521 with a total mass of 150 M _ from Population III binary star evolution. MNRAS , keywords =. doi:10.1093/mnrasl/slaa191 , archivePrefix =. 2009.06922 , primaryClass =

2009 arXiv
[201]

MNRAS , keywords =

Evolution of Wolf-Rayet stars as black hole progenitors. MNRAS , keywords =. doi:10.1093/mnras/stab1548 , archivePrefix =. 2105.12139 , primaryClass =

arXiv
[202]

, keywords =

Stellar wind yields of very massive stars. , keywords =. doi:10.1093/mnras/stad2537 , archivePrefix =. 2308.10941 , primaryClass =

arXiv
[203]

Extragalactic Jets from Every Angle , year = 2015, editor =

The ``Christmas burst'' GRB 101225A revisited. Extragalactic Jets from Every Angle , year = 2015, editor =. doi:10.1017/S1743921315002604 , adsurl =

2015 doi
[204]

Monthly Notices of the Royal Astronomical Society , volume =

Patton, Rachel A and Sukhbold, Tuguldur and Eldridge, J J , title = ". Monthly Notices of the Royal Astronomical Society , volume =. 2022 , month =. doi:10.1093/mnras/stab3797 , url =

2022 doi
[205]

, keywords =

The onset of stellar multiplicity in massive star formation: A search for low-mass companions of massive young stellar objects with L′-band adaptive optics imaging. , keywords =. doi:10.1051/0004-6361/202347548 , archivePrefix =. 2311.06131 , primaryClass =

arXiv
[206]

ApJ , keywords =

Runaway Coalescence at the Onset of Common Envelope Episodes. ApJ , keywords =. doi:10.3847/1538-4357/aacf08 , archivePrefix =. 1803.03261 , primaryClass =

arXiv
[207]

Pulsational Pair-instability Supernovae. I. Pre-collapse Evolution and Pulsational Mass Ejection. ApJ , keywords =. doi:10.3847/1538-4357/ab4fe5 , archivePrefix =. 1901.11136 , primaryClass =

1901 arXiv
[208]

ApJ , keywords =

Stellar Collisions and Ultracompact X-Ray Binary Formation. ApJ , keywords =. doi:10.1086/499938 , archivePrefix =. astro-ph/0509511 , primaryClass =

arXiv
[209]

MNRAS , keywords =

Structure and evolution of high-mass stellar mergers. MNRAS , keywords =. doi:10.1093/mnras/stt1268 , archivePrefix =. 1307.2445 , primaryClass =

arXiv
[210]

A&A , keywords =

Evolution of the stellar-merger red nova V1309 Scorpii: Spectral energy distribution analysis. A&A , keywords =. doi:10.1051/0004-6361/201527700 , archivePrefix =. 1606.09426 , primaryClass =

arXiv
[211]

, keywords =

Investigating cannibalistic millisecond pulsar binaries using MESA: New constraints from pulsar spin and mass evolution. , keywords =. doi:10.1051/0004-6361/202452035 , archivePrefix =. 2408.16048 , primaryClass =

arXiv
[212]

, keywords =

Formation of Black Widows and Redbacks Two Distinct Populations of Eclipsing Binary Millisecond Pulsars. , keywords =. doi:10.1088/0004-637X/775/1/27 , archivePrefix =. 1308.4107 , primaryClass =

arXiv
[213]

, keywords =

Understanding the Evolution of Close Binary Systems with Radio Pulsars. , keywords =. doi:10.1088/2041-8205/786/1/L7 , archivePrefix =. 1402.7338 , primaryClass =

arXiv
[214]

ApJ , keywords =

Stellar Collisions and the Interior Structure of Blue Stragglers. ApJ , keywords =. doi:10.1086/339060 , archivePrefix =. astro-ph/0107388 , primaryClass =

arXiv
[215]

Science , keywords =

Cygnus X-1 contains a 21-solar mass black hole Implications for massive star winds. Science , keywords =. doi:10.1126/science.abb3363 , archivePrefix =. 2102.09091 , primaryClass =
[216]

ApJ , keywords =

Wind Mass-loss Rates of Stripped Stars Inferred from Cygnus X-1. ApJ , keywords =. doi:10.3847/1538-4357/abde4a , archivePrefix =. 2102.09092 , primaryClass =

arXiv
[217]

Binary Systems, their Evolution and Environments , year = 2014, editor =

Black hole X-ray transients: The formation puzzle. Binary Systems, their Evolution and Environments , year = 2014, editor =. doi:10.48550/arXiv.1312.5924 , archivePrefix =. 1312.5924 , primaryClass =

2014 doi arXiv
[218]

, keywords =

The Cosmic Carbon Footprint of Massive Stars Stripped in Binary Systems. , keywords =. doi:10.3847/1538-4357/ac2f44 , archivePrefix =. 2110.04131 , primaryClass =

arXiv
[219]

ApJl , keywords =

Constraints from Gravitational-wave Detections of Binary Black Hole Mergers on the ^ 12 C( , ) ^ 16 O Rate. ApJl , keywords =. doi:10.3847/2041-8213/abbadd , archivePrefix =. 2006.06678 , primaryClass =

arXiv
[220]

A&A , keywords =

The evolution of massive close binaries revised. A&A , keywords =
[221]

Memoires of the Societe Royale des Sciences de Liege , keywords =

On the relationship between Of and WR stars. Memoires of the Societe Royale des Sciences de Liege , keywords =
[222]

ApJ , keywords =

Presupernova Evolution in Massive Interacting Binaries. ApJ , keywords =. doi:10.1086/171341 , adsurl =

doi
[223]

MNRAS , keywords =

Super-Eddington stellar winds driven by near-surface energy deposition. MNRAS , keywords =. doi:10.1093/mnras/stw365 , archivePrefix =. 1509.06370 , primaryClass =

arXiv
[224]

Andrews and Simone S

Tassos Fragos and Jeff J. Andrews and Simone S. Bavera and Christopher P. L. Berry and Scott Coughlin and Aaron Dotter and Prabin Giri and Vicky Kalogera and Aggelos Katsaggelos and Konstantinos Kovlakas and Shamal Lalvani and Devina Misra and Philipp M. Srivastava and Ying Qi...

2023
[225]

The evolution of massive stars and their spectra. I. A non-rotating 60 M _ star from the zero-age main sequence to the pre-supernova stage. A&A , keywords =. doi:10.1051/0004-6361/201322573 , archivePrefix =. 1401.7322 , primaryClass =

arXiv
[226]

Grids of stellar models with rotation. IV. Models from 1.7 to 120 M _ ☉ at a metallicity Z = 0.0004. A&A , keywords =. 2019. doi:10.1051/0004-6361/201833720 , archivePrefix =. 1904.04009 , primaryClass =

2019 arXiv
[227]

ApJ , keywords =

WO-type Wolf-Rayet Stars: The Last Hurrah of Massive Star Evolution. ApJ , keywords =. doi:10.3847/1538-4357/ac66e7 , archivePrefix =. 2204.04258 , primaryClass =

arXiv
[228]

1994", month =

Grids of massive stars with high mass loss rates. V. From 12 to 120 M _ sun \_ at Z=0.001, 0.004, 0.008, 0.020 and 0.040. A&As , year = "1994", month = "Jan", volume =

1994
[229]

Stellar evolution with rotation. V. Changes in all the outputs of massive star models. A&A , keywords =. doi:10.48550/arXiv.astro-ph/0006404 , archivePrefix =. astro-ph/0006404 , primaryClass =

doi arXiv
[230]

Stellar evolution with rotation. X. Wolf-Rayet star populations at solar metallicity. , keywords =. doi:10.1051/0004-6361:20030512 , archivePrefix =. astro-ph/0304069 , primaryClass =

arXiv
[231]

Stellar evolution with rotation. XI. Wolf-Rayet star populations at different metallicities. A&A , keywords =. doi:10.1051/0004-6361:20047106 , archivePrefix =. astro-ph/0408319 , primaryClass =

arXiv
[232]

, keywords =

The early star generations: the dominant effect of rotation on the CNO yields. , keywords =. doi:10.1051/0004-6361:20053070 , archivePrefix =. astro-ph/0510560 , primaryClass =

arXiv
[233]

ApJ , keywords =

Runaway Coalescence of Pre-common-envelope Stellar Binaries. ApJ , keywords =. doi:10.3847/1538-4357/ab822e , archivePrefix =. 1912.05545 , primaryClass =

1912 arXiv
[234]

ApJ , keywords =

Population Synthesis of Black Hole Binaries with Compact Star Companions. ApJ , keywords =. doi:10.3847/1538-4357/ac173e , archivePrefix =. 2107.03565 , primaryClass =

arXiv
[235]

A&A , keywords =

Line-blanketed model atmospheres for WR stars. A&A , keywords =. doi:10.1051/0004-6361:20020269 , adsurl =

doi
[236]

Very massive stars approaching the Eddington limit

Mass loss from late-type WN stars and its Z-dependence. Very massive stars approaching the Eddington limit. A&A , keywords =. doi:10.1051/0004-6361:20066176 , archivePrefix =. 0803.0866 , primaryClass =

arXiv
[237]

Evidence for a -dependence of Wolf-Rayet type mass loss

The Eddington factor as the key to understand the winds of the most massive stars. Evidence for a -dependence of Wolf-Rayet type mass loss. A&A , keywords =. doi:10.1051/0004-6361/201116701 , archivePrefix =. 1106.5361 , primaryClass =

arXiv
[238]

Implications for the radii of Wolf-Rayet stars and luminous blue variables

Stellar envelope inflation near the Eddington limit. Implications for the radii of Wolf-Rayet stars and luminous blue variables. A&A , keywords =. doi:10.1051/0004-6361/201117497 , archivePrefix =. 1112.1910 , primaryClass =

1910 arXiv
[239]

A&A , keywords =

On the optically thick winds of Wolf-Rayet stars. A&A , keywords =. doi:10.1051/0004-6361/201731590 , archivePrefix =. 1710.04543 , primaryClass =

arXiv
[240]

Mass loss, envelope inflation, and a variable upper stellar mass limit

Physics and evolution of the most massive stars in 30 Doradus. Mass loss, envelope inflation, and a variable upper stellar mass limit. A&A , keywords =. doi:10.1051/0004-6361/202040037 , archivePrefix =. 2101.03837 , primaryClass =

arXiv
[241]

, keywords =

Spectral analyses of the Galactic Wolf-Rayet stars: hydrogen-helium abundances and improved stellar parameters for the WN class. , keywords =
[242]

A&A , keywords =

Spectrum formation in clumped stellar winds: consequences for the analyses of Wolf-Rayet spectra. A&A , keywords =
[243]

A&A , keywords =

A temperature correction method for expanding atmospheres. A&A , keywords =. doi:10.1051/0004-6361:20031308 , adsurl =

doi
[244]

Impact of Gaia distances on fundamental stellar parameters

The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters. A&A , keywords =. doi:10.1051/0004-6361/201834850 , archivePrefix =. 1904.04687 , primaryClass =

1904 arXiv
[245]

A&A , keywords =

Empirical mass-loss rates and clumping properties of Galactic early-type O supergiants. A&A , keywords =. doi:10.1051/0004-6361/202140603 , archivePrefix =. 2108.08340 , primaryClass =

arXiv
[246]

10.1051/0004-6361/202348478

Empirical mass-loss rates and clumping properties of O-type stars in the Large Magellanic Cloud , DOI= "10.1051/0004-6361/202348478", url= "https://doi.org/10.1051/0004-6361/202348478", journal =

doi
[247]

arXiv e-prints , keywords =

Stellar winds of O-type stars traced by high ionization fine-structure emission lines with JWST/MIRI. arXiv e-prints , keywords =. doi:10.48550/arXiv.2606.23456 , archivePrefix =. 2606.23456 , primaryClass =

doi arXiv
[248]

Tests using double-lined eclipsing binaries

Does convective core overshooting depend on stellar mass?. Tests using double-lined eclipsing binaries. , keywords =. doi:10.1051/0004-6361:20078024 , adsurl =

doi
[249]

ApJ , keywords =

The Dependence of Convective Core Overshooting on Stellar Mass: Additional Binary Systems and Improved Calibration. ApJ , keywords =. doi:10.3847/1538-4357/aabd35 , archivePrefix =. 1804.03148 , primaryClass =

arXiv
[250]

, keywords =

An asteroseismic study of the Cephei star Ophiuchi: constraints on global stellar parameters and core overshooting. , keywords =. doi:10.1111/j.1365-2966.2007.12142.x , archivePrefix =. 0706.3274 , primaryClass =

2007
[251]

, keywords =

A study of convective core overshooting as a function of stellar mass based on two-dimensional hydrodynamical simulations. , keywords =. doi:10.1093/mnras/stad009 , archivePrefix =. 2301.02604 , primaryClass =

arXiv
[252]

MNRAS , volume =

Baraffe, I and Clarke, J and Morison, A and Vlaykov, D G and Constantino, T and Goffrey, T and Guillet, T and Le Saux, A and Pratt, J , title =. MNRAS , volume =. 2023 , month =. doi:10.1093/mnras/stad009 , url =

2023 doi
[253]

, keywords =

Evolution of massive stars : comparison of cluster sequences and models with mass loss. , keywords =
[254]

A&A , keywords =

The spectroscopic Hertzsprung-Russell diagram of Galactic massive stars. A&A , keywords =. doi:10.1051/0004-6361/201425028 , archivePrefix =. 1410.3499 , primaryClass =

arXiv
[255]

Castro and M

N. Castro and M. S. Oey and L. Fossati and N. Langer , title =. The Astrophysical Journal , abstract =. 2018 , month =. doi:10.3847/1538-4357/aae6d0 , url =

2018 doi
[256]

, keywords =

Dynamical masses across the Hertzsprung-Russell diagram. , keywords =. doi:10.1093/mnras/stae297 , archivePrefix =. 2308.08584 , primaryClass =

arXiv
[257]

, keywords =

On the nature of the galactic early-B hypergiants. , keywords =. doi:10.1051/0004-6361/201117472 , archivePrefix =. 1202.3991 , primaryClass =

arXiv
[258]

Coupling hydrodynamics with comoving frame radiative transfer. I. A unified approach for OB and WR stars. A&A , keywords =. doi:10.1051/0004-6361/201730642 , archivePrefix =. 1704.08698 , primaryClass =

arXiv
[259]

The impact of revised distances from Gaia DR2 and their role as massive black hole progenitors

The Galactic WC and WO stars. The impact of revised distances from Gaia DR2 and their role as massive black hole progenitors. , keywords =. doi:10.1051/0004-6361/201833712 , archivePrefix =. 1807.04293 , primaryClass =

arXiv
[260]

MNRAS , keywords =

On the nature of massive helium star winds and Wolf-Rayet-type mass-loss. MNRAS , keywords =. doi:10.1093/mnras/staa2712 , archivePrefix =. 2009.01849 , primaryClass =

2009 arXiv
[261]

MNRAS , keywords =

Driving classical Wolf-Rayet winds: a - and Z-dependent mass-loss. MNRAS , keywords =. doi:10.1093/mnras/stz3064 , archivePrefix =. 1910.12886 , primaryClass =

1910 arXiv
[262]

An exploratory study for winds launched by the hot iron bump

The temperature dependency of Wolf-Rayet-type mass loss. An exploratory study for winds launched by the hot iron bump. A&A , keywords =. doi:10.1051/0004-6361/202245110 , archivePrefix =. 2301.01785 , primaryClass =

arXiv
[263]

2025 , eprint=

Discovery of a new transitional type of evolved massive stars with hard ionizing flux , author=. 2025 , eprint=

2025
[264]

, keywords =

Near-Eddington mass loss of hydrogen-rich Wolf-Rayet stars: Consequences of continuum acceleration, metallicity, and temperature. , keywords =. doi:10.1051/0004-6361/202554505 , archivePrefix =. 2506.13582 , primaryClass =

arXiv
[265]

The VLT-FLAMES Tarantula Survey . XXIV. Stellar properties of the O-type giants and supergiants in 30 Doradus. , keywords =. doi:10.1051/0004-6361/201628914 , archivePrefix =. 1701.04758 , primaryClass =

arXiv
[266]

, keywords =

An LTE effective temperature scale for red supergiants in the Magellanic clouds. , keywords =. doi:10.1093/mnras/sty399 , archivePrefix =. 1802.03219 , primaryClass =

arXiv
[267]

, keywords =

Evolutionary nature of puffed-up stripped star binaries and their occurrence in stellar populations. , keywords =. doi:10.1051/0004-6361/202349065 , archivePrefix =. 2312.12658 , primaryClass =

arXiv
[268]

A&A , keywords =

Clumping and X-rays in cooler B supergiant stars. A&A , keywords =. doi:10.1051/0004-6361/202346469 , archivePrefix =. 2307.05421 , primaryClass =

arXiv
[269]

10.1051/0004-6361/202450475

X-Shooting ULLYSES: Massive stars at low metallicity - VII. Stellar and wind properties of B supergiants in the Small Magellanic Cloud , DOI= "10.1051/0004-6361/202450475", url= "https://doi.org/10.1051/0004-6361/202450475", journal =

doi
[270]

The Wind Regime of Early-Type B Hypergiants

Coupling hydrodynamics with comoving frame radiative transfer: III. The Wind Regime of Early-Type B Hypergiants. , keywords =. doi:10.1051/0004-6361/202554127 , archivePrefix =. 2504.03537 , primaryClass =

arXiv
[271]

MNRAS , keywords =

Mass loss and the Eddington parameter: a new mass-loss recipe for hot and massive stars. MNRAS , keywords =. doi:10.1093/mnras/staa474 , archivePrefix =. 2002.05168 , primaryClass =

2002 arXiv
[272]

The VLT-FLAMES Tarantula Survey. XVII. Physical and wind properties of massive stars at the top of the main sequence. A&A , keywords =. doi:10.1051/0004-6361/201423643 , archivePrefix =. 1407.1837 , primaryClass =

arXiv
[273]

A&A , keywords =

On the nature of the bi-stability jump in the winds of early-type supergiants. A&A , keywords =
[274]

A&A , eprint =

New theoretical mass-loss rates of O and B stars. A&A , eprint =
[275]

A&A , eprint =

Mass-loss predictions for O and B stars as a function of metallicity. A&A , eprint =. doi:10.1051/0004-6361:20010127 , adsurl =

doi
[276]

, keywords =

On the metallicity dependence of Wolf-Rayet winds. , keywords =. doi:10.1051/0004-6361:20052862 , archivePrefix =. astro-ph/0507352 , primaryClass =

arXiv
[277]

The possibility of Bi-stability braking

The nature of B supergiants: clues from a steep drop in rotation rates at 22 000 K. The possibility of Bi-stability braking. A&A , keywords =. doi:10.1051/0004-6361/201014205 , archivePrefix =. 1003.1280 , primaryClass =

arXiv
[278]

A&A , keywords =

Wind modelling of very massive stars up to 300 solar masses. A&A , keywords =. doi:10.1051/0004-6361/201116614 , archivePrefix =. 1105.0556 , primaryClass =

arXiv
[279]

ApJl , keywords =

The Transition Mass-loss Rate: Calibrating the Role of Line-driven Winds in Massive Star Evolution. ApJl , keywords =. doi:10.1088/2041-8205/751/2/L34 , archivePrefix =. 1205.0394 , primaryClass =

arXiv
[280]

2015 , eprint=

The True origin of Wolf-Rayet stars , author=. 2015 , eprint=

2015
[281]

A&A , keywords =

Winds from stripped low-mass helium stars and Wolf-Rayet stars. A&A , keywords =. doi:10.1051/0004-6361/201731902 , archivePrefix =. 1710.02010 , primaryClass =

arXiv
[282]

MNRAS , keywords =

Maximum black hole mass across cosmic time. MNRAS , keywords =. doi:10.1093/mnras/stab842 , archivePrefix =. 2010.11730 , primaryClass =

2010 arXiv
[283]

MNRAS , keywords =

Metallicity-dependent wind parameter predictions for OB stars. MNRAS , keywords =. doi:10.1093/mnras/stab902 , archivePrefix =. 2103.12736 , primaryClass =

arXiv
[284]

ARAA , keywords =

Theory and Diagnostics of Hot Star Mass Loss. ARAA , keywords =. doi:10.1146/annurev-astro-052920-094949 , archivePrefix =. 2109.08164 , primaryClass =

arXiv
[285]

arXiv e-prints , keywords =

Theory and Diagnostics of Hot Star Mass Loss. arXiv e-prints , keywords =
[286]

X-Shooting ULLYSES: Massive stars at low metallicity. I. Project description. A&A , keywords =. doi:10.1051/0004-6361/202245650 , archivePrefix =. 2305.06376 , primaryClass =

arXiv
[287]

A Universal mass-loss concept for massive stars

Exploring the Red Supergiant wind kink. A Universal mass-loss concept for massive stars. , keywords =. doi:10.1051/0004-6361/202347801 , archivePrefix =. 2309.08657 , primaryClass =

arXiv
[288]

arXiv e-prints , keywords =

The Maximum Black Hole Mass at Solar Metallicity. arXiv e-prints , keywords =. doi:10.48550/arXiv.2407.07204 , archivePrefix =. 2407.07204 , primaryClass =

doi arXiv
[289]

Astronomy & Astrophysics , year=

How common is LBV S Doradus variability at low metallicity? , author=. Astronomy & Astrophysics , year=
[290]

, keywords =

The role of /Z=0 AGB stars on the early chemical enrichment. , keywords =. doi:10.1016/S0375-9474(01)00736-9 , archivePrefix =. astro-ph/0010365 , primaryClass =

arXiv
[291]

10.1051/0004-6361/201732317

The shape of convective core overshooting from gravity-mode period spacings , DOI= "10.1051/0004-6361/201732317", url= "https://doi.org/10.1051/0004-6361/201732317", journal =

doi
[292]

Nature Astronomy , keywords =

Internal mixing of rotating stars inferred from dipole gravity modes. Nature Astronomy , keywords =. doi:10.1038/s41550-021-01351-x , archivePrefix =. 2105.04533 , primaryClass =

arXiv
[293]

Atmosphere and mass-loss properties of O-type giants in the Small Magellanic Cloud

X-Shooting ULLYSES: Massive stars at low metallicity: VI. Atmosphere and mass-loss properties of O-type giants in the Small Magellanic Cloud. , keywords =. doi:10.1051/0004-6361/202451893 , archivePrefix =. 2411.06884 , primaryClass =

arXiv
[294]

Radiation driven winds of hot luminous stars. II. Wind models for O-stars in the Magellanic clouds. A\ keywords =
[295]

, keywords =

Winds from Hot Stars. , keywords =. doi:10.1146/annurev.astro.38.1.613 , adsurl =

doi
[296]

Line-driven Winds, Ionizing Fluxes, and Ultraviolet Spectra of Hot Stars at Extremely Low Metallicity. I. Very Massive O Stars. , keywords =. doi:10.1086/342178 , archivePrefix =. astro-ph/0205210 , primaryClass =

arXiv
[297]

Improvements of the theory and first results

Radiation-driven winds of hot luminous stars. Improvements of the theory and first results. A\ keywords =
[298]

Radiation-driven winds of hot luminous stars. VIII. The bistable wind of the luminous blue variable P Cygni (B1 Ia+). , keywords =
[299]

ApJ , eprint =

The Influence of Rotation in Radiation-driven Wind from Hot Stars: New Solutions and Disk Formation in Be Stars. ApJ , eprint =. doi:10.1086/423776 , adsurl =

doi
[300]

The influence of rotation in radiation driven winds from hot stars. II. CAK topological analysis. A&A , keywords =. doi:10.1051/0004-6361:20040325 , archivePrefix =. astro-ph/0408511 , primaryClass =

arXiv

Pith tools

Reviewed August 1, 2026 · model on record in the stance chip above.

[1] [1]

The -slow regime

Analytical solutions for radiation-driven winds in massive stars - II. The -slow regime. MNRAS , keywords =. doi:10.1093/mnras/stab995 , archivePrefix =. 2104.03263 , primaryClass =

arXiv

[2] [2]

, keywords =

Unveiling the Cygnus OB2 stellar population with Chandra. , keywords =. doi:10.1051/0004-6361:20066101 , archivePrefix =. astro-ph/0610352 , primaryClass =

arXiv

[3] [3]

ApJ , keywords =

The Impact of Realistic Red Supergiant Mass Loss on Stellar Evolution. ApJ , keywords =. doi:10.3847/1538-4357/ac2574 , archivePrefix =. 2109.03239 , primaryClass =

arXiv

[4] [4]

MNRAS , keywords =

Correction to: 'A new mass-loss rate prescription for red supergiants'. MNRAS , keywords =. doi:10.1093/mnras/stad1818 , adsurl =

work page doi:10.1093/mnras/stad1818

[5] [5]

ApJ , keywords =

Evolution of Galaxy Star Formation and Metallicity: Impact on Double Compact Object Mergers. ApJ , keywords =. doi:10.3847/1538-4357/abd3a0 , archivePrefix =. 2012.02800 , primaryClass =

arXiv 2012

[6] [6]

arXiv e-prints , keywords =

Metal-poor single Wolf-Rayet stars: the interplay of optically thick winds and rotation. arXiv e-prints , keywords =. doi:10.48550/arXiv.2507.00137 , archivePrefix =. 2507.00137 , primaryClass =

work page doi:10.48550/arxiv.2507.00137

[7] [7]

arXiv e-prints , keywords =

Can current models predict the local black hole merger rate?. arXiv e-prints , keywords =. doi:10.48550/arXiv.2606.02725 , archivePrefix =. 2606.02725 , primaryClass =

arXiv doi:10.48550/arxiv.2606.02725

[8] [8]

Nature , year=

Identification of Cygnus X-1 with HDE 226868 , author=. Nature , year=