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REVIEW 4 major objections 5 minor 296 references

Fitting the observed end of the main sequence forces a mass-dependent overshoot in massive-star models, and the overabundance of blue supergiants beyond that line appears to require binary mergers.

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2026-08-03 02:34 UTC pith:YA4F3FM7

load-bearing objection Careful, honest calibration study with new mass-dependent overshoot values, but the BSG 'single-star failure' headline rests on a population comparison that ignores the IACOB selection function. the 4 major comments →

arxiv 2607.29650 v1 pith:YA4F3FM7 submitted 2026-07-31 astro-ph.SR astro-ph.GA

The IACOB project XIX. Revisiting massive-star evolution with empirical TAMS constraints: updated models, overshoot calibration, and the population of blue supergiants

Luca Sciarini , Abel de Burgos , Sophie Rosu , Sylvia Ekstr\"om , Sergio Sim\'on-D\'iaz , Cyril Georgy This is my paper
classification astro-ph.SR astro-ph.GA
keywords massive starsconvective overshootterminal-age main sequenceblue supergiantsstellar rotationpopulation synthesisHertzsprung-Russell diagramsingle-star evolution
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper uses the empirically observed location of the terminal-age main sequence (TAMS) in the Hertzsprung-Russell diagram to calibrate convective overshoot in single-star models of 12–40 solar masses. The authors find that a constant overshoot efficiency cannot reproduce observations; the required step-overshoot parameter rises to a peak near 15–20 solar masses and declines toward higher masses. Even with this tuned mixing, synthetic populations put only about 0.1% of stars to the right of the TAMS, while about 15% of observed massive stars sit there. The paper concludes that the blue supergiants beyond the TAMS largely cannot be explained by single-star evolution and are most plausibly products of binary mergers. If right, this gives both a new calibration of core-boundary mixing and a quantitative argument that binaries dominate the post-main-sequence massive-star population.

Core claim

The central claim is that matching the empirical TAMS lines derived from the IACOB sample requires a mass-dependent overshoot efficiency, with slow-rotator calibration values of α_ov between 0.18 and 0.45 that peak at 15–20 M_sun, in contrast to both the standard constant α_ov=0.1 and the monotonically increasing formula of Scott et al. (2021). The calibrated slow-rotating models reproduce the empirical TAMS, but the same models cannot explain the velocity dependence of the TAMS or the dense population of blue supergiants to its right: models cross the Hertzsprung gap in 5–20 kyr, predicting less than 0.1% of stars there versus the observed ~15%. The authors interpret this mismatch as eviden

What carries the argument

The load-bearing object is the empirical TAMS: two fitted lines from the IACOB sample (de Burgos et al. 2025) that mark where the density of stars drops at the end of core hydrogen burning — one for the full sample, log(L/Lsun)=0.47 Teff−5.42, and one for slow rotators, Teff=21.45 kK. The calibration adjusts the step-overshoot parameter α_ov (mixing distance past the convective core in units of pressure scale height) so that the 'MS hook' of each track lands on the empirical line. Synthetic populations are then built from the calibrated tracks to compare predicted and observed HR diagrams.

Load-bearing premise

The empirical TAMS lines are taken as the true end of the main sequence for single stars; if they are biased by binary products among slow rotators or by post-red-supergiant blue loops, every fitted overshoot value would shift.

What would settle it

An asteroseismic measurement of core overshoot in a ~15–20 M_sun star giving α_ov well below 0.4, or a stellar model with rotation-dependent overshoot that reproduces the velocity-split TAMS lines without re-calibration, would each falsify the central calibration.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • If the calibration is correct, standard grids that assume a single overshoot value (like 0.1 or 0.335) misplace the main-sequence width of 12–40 M_sun stars, and the mismatch grows above 25 M_sun where smaller α_ov is needed.
  • The predicted share of blue supergiants beyond the TAMS is ~0.1%, versus ~15% observed; no variation of angular-momentum transport, convective criterion, or post-RSG blue-loop channel closes this gap.
  • The velocity dependence of the empirical TAMS is not reproduced: single-star models place the fast-rotator TAMS at cooler temperatures than observed, implying fast rotators in the sample are largely not single stars.
  • Hydrodynamic-only angular momentum transport with the Björklund et al. (2023) wind prescription reproduces observed spin-down behaviour, removing a prior mismatch attributed to overly strong winds.

Where Pith is reading between the lines

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

  • If confirmed by future asteroseismic probes of core-boundary mixing around 15–20 M_sun, the non-monotonic α_ov trend would argue for a physical transition (e.g., in envelope structure) rather than a simple scaling with mass.
  • The same empirical TAMS lines could calibrate overshoot in binary evolution codes; under the merger interpretation, the pile-up of blue supergiants right of the TAMS constrains the merger rate and post-merger rejuvenation.
  • Magnetic models predict a population of fast, helium-enriched hot subdwarfs; their absence or presence in surveys would directly test the rotational-mixing efficiency assumed here.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 5 minor

Summary. The paper calibrates the overshoot parameter α_ov in GENEC models by requiring their theoretical TAMS to match empirical TAMS lines from de Burgos et al. (2025) for Galactic OB stars in the IACOB sample. Four calibrations are performed (two AMT treatments × TAMS definitions from the full sample and slow rotators) for initial masses 12–40 M_sun at low rotation. The calibrated grids are extended to initial velocities up to 0.6 v_crit, and synthetic populations are generated with SYCLIST under a uniform IMF, constant SFR, and an empirical velocity CDF. The authors find: (1) mass-dependent, non-monotonic α_ov peaking near 15–20 M_sun, larger than the standard 0.1; (2) the models reproduce the slow-rotator TAMS by construction; (3) models cannot reproduce the velocity dependence of the TAMS; (4) single-star populations predict ~0.1% of stars to the right of the TAMS versus ~15% observed, which they attribute to binary interaction products.

Significance. If robust, the empirical TAMS calibration provides new constraints on convective boundary mixing in massive stars and supports a mass-dependent overshoot; the rotational-velocity comparison is a useful test of wind prescriptions. The paper is careful in listing caveats, and the grids/tracks are made available. However, as presented, the strongest conclusions are weakened by (i) the circular use of the calibration as validation, (ii) the absence of a selection function for the IACOB sample in the synthetic-population comparison, and (iii) missing uncertainties on α_ov. The paper is a solid modeling contribution but needs revision before its headline claims are accepted.

major comments (4)
  1. [§3.1, §4.2, §6] The models are calibrated to reproduce the empirical TAMS lines, so statements that the models 'perfectly fit' the TAMS (§3.1, point 2) and that the synthetic density drop at the TAMS 'validates our approach' (§4.2, point 1) are circular. The paper does acknowledge 'by construction' in §3.1, but the abstract and conclusion present the reproduction of the TAMS as a successful empirical test. I recommend reframing: the calibration is a fit, and the independent check is the CDF comparison in §5.2, which actually shows disagreement. The validation language should be removed or explicitly qualified.
  2. [§4.1, §4.2 (point 5)] The headline result that single-star models fail to explain the BSG population (15% observed vs ~0.1% synthetic to the right of the TAMS) assumes that the observed IACOB sample is a fair draw from the underlying population with a uniform IMF and no selection effects. The paper does not model the Teff-dependent target selection of IACOB (e.g., B-type supergiants may be preferentially included over MS O/B stars at the same luminosity). This is load-bearing: the BSG deficit could largely disappear once the selection function is applied. The authors justify the uniform IMF but do not address sample completeness. This missing support prevents the binary-merger inference from being established.
  3. [Table A.1, §3.1] The calibrated α_ov values are quoted without uncertainties. Since they are obtained by matching empirical TAMS lines that themselves have uncertainties (de Burgos et al. 2025), and since the central claim is a non-monotonic mass dependence peaking at 15–20 M_sun, the absence of error bars makes it impossible to judge whether the mass dependence is significant. A simple sensitivity study (e.g., varying the empirical TAMS within its confidence band and recomputing α_ov, or propagating the observational errors) is needed before this result can be used by the community.
  4. [§3.2, §5.4 (caveat 1)] The conclusion that single-star models are 'unsuccessful at explaining the velocity dependence of the TAMS' is obtained under the assumption that α_ov is independent of rotation. This assumption is acknowledged as a caveat, but it is load-bearing: if overshoot and rotation interact, the fast-rotating tracks and the synthetic FR population would change, and the discrepancy with the empirical FR TAMS might be reduced. I ask the authors to either test a rotation-dependent α_ov (or a reasonable ad hoc prescription) or to explicitly state in the abstract that the failure applies only to rotation-independent overshoot. Without this, the claim is overstated.
minor comments (5)
  1. [Eq. (1)] The coefficient 0.47 has units of dex/kK; please write the fit with units or in a dimensionless form to avoid ambiguity.
  2. [§5.1 and §5.4] 'Schwarzchild' should be 'Schwarzschild'.
  3. [§3.3] 'genechydro' should be 'genechydro models' with a space.
  4. [§5.3] The symbols 'eMsp' and 'Msp' are presumably median and mean spectroscopic masses; use \tilde{M} and \bar{M} for clarity.
  5. [§4.1] The phrase 'Malmquist (1922) bias' is usually written as 'Malmquist bias' without the year in parentheses.

Circularity Check

2 steps flagged

Calibration is transparent, but the paper twice presents the TAMS fit itself as validation: the 'perfect' reproduction of the empirical TAMS and the synthetic-population density drop are by-construction restatements of the α_ov fit.

specific steps
  1. self definitional [Abstract; Sect. 2; Sect. 3.1 bullet 2]
    "we systematically calibrate the value of α_ov such that the models TAMS line – defined as in Martinet et al. (2021) with the minimum temperature reached during the MS, that is, the MS hook – exactly fits the empirical TAMS line derived by de Burgos et al. (2025). ... By construction, models perfectly fit the empirical TAMS of the considered sample (FS or SR). ... The calibrated models at slow rotation reproduce the empirical TAMS location."

    The TAMS alignment is the definition of the calibration: α_ov is tuned so that the model MS hook lands on the empirical de Burgos et al. line. Reporting this as a result ('the calibrated models reproduce the empirical TAMS location') is therefore a restatement of the fitting procedure, not an independent test. The paper itself labels the fit 'by construction', but the Abstract nevertheless presents it as a headline finding.

  2. fitted input called prediction [Sect. 4.2, item 1; Sect. 6]
    "For each type of AMT treatment, the population of SR perfectly reproduce the empirical TAMS, being the full sample TAMS for the models computed with the 'FS calibration' or the slow rotators TAMS for those computed with the 'SR calibration'. Indeed, the density of generated stars drastically drops at the empirical TAMS line. This validates our approach in matching the theoretical TAMS to the empirical TAMS."

    The synthetic populations are drawn from the same tracks whose MS hooks were calibrated to sit exactly on the empirical TAMS. The density drop at that line is inherited from the imposed calibration and is preserved through interpolation, inclination projection, and added noise. Calling this a validation of the calibration is circular: the drop is a consequence of the fit, not an independent prediction that confirms it.

full rationale

The paper is unusually transparent: it explicitly says the α_ov calibration makes the models 'perfectly fit' the empirical TAMS and later says the drop of synthetic density at the TAMS 'validates our approach in matching the theoretical TAMS to the empirical TAMS.' Those two statements are by-construction restatements and are flagged above. The mass-dependent α_ov values in Table A.1 are also the fitted parameters themselves, so the statement that a mass-dependent overshoot efficiency is 'required' is mainly describing the calibration output rather than a prediction; however, the paper uses the phrase 'to fit the observational constraints,' so it does not mislabel that as a prediction. The velocity-dependence failure, the rotational-property comparison, and the blue-supergiant deficit (0.1% vs 15%) are not forced by the α_ov fit: they depend on post-MS crossing times, rotation physics, and the synthetic-population construction, which are independent outputs of the models. The empirical TAMS from de Burgos et al. (2025) involves overlapping authorship (de Burgos and Simón-Díaz), but it is an observational, externally falsifiable input rather than a result imported from this paper's own fitting chain, so I do not count it as load-bearing circularity. The main caveat flagged by the skeptic (no IACOB selection function in the synthetic population, uniform IMF, constant SFR) is a completeness/robustness concern, not a circularity reduction, and is therefore not included in the score. Overall: partial circularity in the self-validation of the calibration, but the central physical conclusions retain independent content.

Axiom & Free-Parameter Ledger

1 free parameters · 6 axioms · 0 invented entities

The central claims rest on accepting the empirical TAMS lines from de Burgos et al. (2025) as ground truth, on a mass-only overshoot dependence, and on single-star evolution for the calibrating sample. These are stated clearly in the paper, so the ledger is transparent; only α_ov is fitted, no new entities are invented.

free parameters (1)
  • Calibrated overshoot efficiency α_ov per initial mass, AMT treatment, and calibrating sample = Table A.1: Hydro FS 0.27–0.18; Hydro SR 0.21–0.23; Magnetic FS 0.30–0.20; Magnetic SR 0.22–0.25 across 12–40 M_sun; peak
    Chosen so the theoretical TAMS hook matches the empirical TAMS lines Eq. (1) and Eq. (2); the mass-dependence claim is a property of these fitted values.
axioms (6)
  • domain assumption The empirical TAMS lines of de Burgos et al. (2025) (Eqs. 1 and 2) trace the true end of the main sequence for the IACOB sample.
    Used as calibration target for α_ov in Sect. 2; if biased, all fitted overshoot values and the mass-dependence conclusion shift.
  • ad hoc to paper Overshoot efficiency α_ov depends only on initial mass and is independent of rotation.
    Stated in §5.4 caveat 1; the grids extrapolate SR calibration to all velocities; if false, the velocity-dependence failure could be an artifact.
  • domain assumption The theoretical TAMS is defined as the minimum Teff reached during MS (MS hook) and maps onto the empirical TAMS density-drop definition.
    §5.2 discusses possible inconsistency; CDF comparison shows the mismatch persists even when definitions are aligned.
  • domain assumption Single-star evolution is an adequate baseline for the slow-rotator calibrating sample.
    Paper acknowledges ~70% binarity (§5.4 caveat 3); if SR sample contains binary products, calibration is biased.
  • domain assumption Björklund et al. (2023) winds prescription is more appropriate than Vink et al. (2001) for OB stars.
    Underlies the attribution of the rotational-property success; cited external evidence supports weaker winds, but this is still a modeling input.
  • domain assumption Synthetic populations require uniform IMF and constant SFR (Sect. 4.1).
    Simplifies comparison; authors argue the BSG deficit is robust to IMF choice, but the quantitative 0.1% vs 15% depends on it.

pith-pipeline@v1.3.0-daily-deepseek · 21819 in / 11641 out tokens · 111647 ms · 2026-08-03T02:34:44.044246+00:00 · methodology

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read the original abstract

Massive stars play a fundamental role in the evolution of the Universe. Yet, several physical processes governing their evolution remain poorly constrained. Notably, the main-sequence width is sensitive to the convective boundary mixing efficiency; it becomes necessary to account for binary interactions to explain some observed properties of massive-star populations. We constrain single-star models using recent observations of massive Galactic stars from the IACOB database. We use the latest proposed empirical location of the TAMS to calibrate the convective boundary mixing efficiency, and use this calibration to test single-star evolution by comparing various model predictions to the observed populations of the IACOB sample. We compute several GENEC grids with various overshoot calibrations, angular momentum transport (AMT) treatments, initial masses and velocities. Finally, we generate synthetic populations from the tracks with SYCLIST and perform a direct comparison with the observed population. The calibrated models at slow rotation reproduce the empirical TAMS location. We find that a mass-dependent overshoot efficiency is required to fit the observational constraints. The overall rotational properties of the observed populations are well reproduced with single-star models, independently of the AMT assumptions. Models accounting only for hydrodynamical instabilities are successful at reproducing the rotational properties, unlike previous genec grids, which we attribute to the choice of winds prescription. Although the empirical TAMS of slow rotators is well reproduced, we find that models are unsuccessful at explaining the velocity dependence of the TAMS location observed in the IACOB sample. Finally, we find that single-star models fail at explaining the population of blue supergiants to the right of the TAMS location.

Figures

Figures reproduced from arXiv: 2607.29650 by Abel de Burgos, Cyril Georgy, Luca Sciarini, Sergio Sim\'on-D\'iaz, Sophie Rosu, Sylvia Ekstr\"om.

Figure 1
Figure 1. Figure 1: Calibrated values of αov for stellar models in the mass range Mini = 12−40 M⊙ using constrains from the IACOB sample (de Burgos et al. 2025). Dashed lines: calibrated values for the FS (i.e., Eq. (1)), solid line, for the SR (i.e., Eq. (2)). Magenta lines: hydro models, blue line: magnetic models. Dashed black line, αov from Scott et al. (2021). 3. Stellar tracks 3.1. Convective boundary mixing dependence … view at source ↗
Figure 2
Figure 2. Figure 2: HRD of stellar models in the mass range Mini = 12 − 40 M⊙ compared to observations from the IACOB sample (de Burgos et al. 2025). Upper panels: Hydro models. Lower panels: Magnetic models. Left to right: αov = 0.1, αov calibrated with the FS, αov calibrated with the SR, αov from Scott et al. (2021). Stars with υ sin i below and above 100 km/s are colored in orange and cyan, respectively. Purple-black line:… view at source ↗
Figure 3
Figure 3. Figure 3: HRD of stellar models in the mass range Mini = 12 − 32 M⊙ with various initial rotational velocities compared to observations from de Burgos et al. (2025). Upper panel: Hydro models. Lower panel: Magnetic models. Observed stars are color-coded as in [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Temperature-velocity diagram of stellar models in the mass range Mini = 12 − 40 M⊙ with initial rotational velocities υini/υcrit = 0.1, 0.4, 0.6 compared to observations from de Burgos et al. (2025). Observed stars are color-coded as in [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: HRD of synthetic populations generated with syclist. Upper panels: Hydro models. Lower panels: Magnetic models. Left panels: Full sample αov calibration. Right panels: Slow rotators αov calibration. Generated stars are color-coded as in [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Teff −υ sin i diagram of synthetic populations generated with syclist. Upper panels: Hydro models. Lower panels: Magnetic models. Left panels: Full sample αov calibration. Right panels: Slow rotators αov calibration. Generated stars are color-coded as in [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Observational and theoretical cumulative distributions in four lu￾minosity bins. The blue shaded area corresponds to the empirical TAMS location, i.e. to the Teff where the CDF of the different luminosity bins drop below 15 % (dashed black line). We further notice that the models’ CDF already get close to zero in the region of the empirical TAMS, which is consistent with the observed distribution in the HR… view at source ↗
Figure 8
Figure 8. Figure 8: Evolution in the HRD of stellar models of masses Mini = 20 and 32 M⊙ with different RSG winds prescriptions compared to observations from (de Burgos et al. 2025). Upper panel: Observa￾tions are color-coded by their mass. Lower panel: Models and observa￾tions are color-coded by their mass. Red-black line: SR TAMS, gray￾black line: temperature limit of the sample. Stars outside the luminos￾ity bin log L/L⊙ =… view at source ↗

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Works this paper leans on

296 extracted references · 20 canonical work pages · 7 internal anchors

  1. [1]

    , keywords =

    Observation of Gravitational Waves from a Binary Black Hole Merger. , keywords =. doi:10.1103/PhysRevLett.116.061102 , archivePrefix =. 1602.03837 , primaryClass =

    Pith/arXiv arXiv

  2. [2]

    GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs , author =. Phys. Rev. X , volume =. 2019 , month =. doi:10.1103/PhysRevX.9.031040 , url =

    doi:10.1103/physrevx.9.031040 2019

  3. [3]

    , keywords =

    Clues on the Origin and Evolution of Massive Contact Binaries: Atmosphere Analysis of VFTS 352. , keywords =. doi:10.3847/1538-4357/ab24d4 , archivePrefix =. 1906.01066 , primaryClass =

    Pith/arXiv arXiv 1906

  4. [4]

    Constraining the overcontact phase in massive binary evolution. I. Mixing in V382 Cyg, VFTS 352, and OGLE SMC-SC10 108086. , keywords =. doi:10.1051/0004-6361/202040195 , archivePrefix =. 2104.07621 , primaryClass =

    Pith/arXiv arXiv

  5. [5]

    Science , keywords =

    Asteroseismology of HD 129929: Core Overshooting and Nonrigid Rotation. Science , keywords =. doi:10.1126/science.1084993 , adsurl =

    doi:10.1126/science.1084993

  6. [6]

    , keywords =

    Angular Momentum Transport in Stellar Interiors. , keywords =. doi:10.1146/annurev-astro-091918-104359 , archivePrefix =. 1809.07779 , primaryClass =

    Pith/arXiv arXiv

  7. [7]

    , keywords =

    The fates of massive stars: exploring uncertainties in stellar evolution with METISSE. , keywords =. doi:10.1093/mnras/staa2264 , archivePrefix =. 2005.13177 , primaryClass =

    Pith/arXiv arXiv 2005

  8. [8]

    , keywords =

    Modelling stellar evolution in mass-transferring binaries and gravitational-wave progenitors with METISSE. , keywords =. doi:10.1093/mnras/stad2334 , archivePrefix =. 2303.10187 , primaryClass =

    Pith/arXiv arXiv

  9. [9]

    From 0.2 to 1.5 M _ at seven metallicities from PMS to TAMS

    First grids of low-mass stellar models and isochrones with self-consistent treatment of rotation. From 0.2 to 1.5 M _ at seven metallicities from PMS to TAMS. , keywords =. doi:10.1051/0004-6361/201935160 , archivePrefix =. 1905.08516 , primaryClass =

    Pith/arXiv arXiv 1905

  10. [10]

    arXiv e-prints , keywords =

    POSYDON Version 2: Population Synthesis with Detailed Binary-Evolution Simulations across a Cosmological Range of Metallicities. arXiv e-prints , keywords =

  11. [11]

    , keywords =

    Timescales of Kozai-Lidov oscillations at quadrupole and octupole order in the test particle limit. , keywords =. doi:10.1093/mnras/stv1552 , archivePrefix =. 1504.05957 , primaryClass =

    Pith/arXiv arXiv

  12. [12]

    , keywords =

    Binary Black Hole Mergers from Field Triples: Properties, Rates, and the Impact of Stellar Evolution. , keywords =. doi:10.3847/1538-4357/aa6f5e , archivePrefix =. 1703.06614 , primaryClass =

    Pith/arXiv arXiv

  13. [13]

    , keywords =

    Impact of the Tayler magnetic instability on the surface abundance of boron in massive stars. , keywords =. doi:10.1051/0004-6361/202555163 , archivePrefix =. 2507.04267 , primaryClass =

    Pith/arXiv arXiv

  14. [14]

    , 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 =

    Pith/arXiv arXiv

  15. [15]

    Predicting the distributions of the main observables of Advanced LIGO

    The origin of spin in binary black holes. Predicting the distributions of the main observables of Advanced LIGO. , keywords =. doi:10.1051/0004-6361/201936204 , archivePrefix =. 1906.12257 , primaryClass =

    Pith/arXiv arXiv 1906

  16. [16]

    Nature Astronomy , keywords =

    The formation of merging black holes with masses beyond 30 M _ at solar metallicity. Nature Astronomy , keywords =. doi:10.1038/s41550-023-02018-5 , archivePrefix =. 2212.10924 , primaryClass =

    Pith/arXiv arXiv

  17. [17]

    , keywords =

    A new mass-loss rate prescription for red supergiants. , keywords =. doi:10.1093/mnras/staa255 , archivePrefix =. 2001.07222 , primaryClass =

    Pith/arXiv arXiv 2001

  18. [18]

    , keywords =

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

    Pith/arXiv arXiv

  19. [19]

    , keywords =

    A Comprehensive Study of Binary Compact Objects as Gravitational Wave Sources: Evolutionary Channels, Rates, and Physical Properties. , keywords =. doi:10.1086/340304 , archivePrefix =. astro-ph/0111452 , primaryClass =

    Pith/arXiv arXiv

  20. [20]

    , keywords =

    Compact Object Modeling with the StarTrack Population Synthesis Code. , keywords =. doi:10.1086/521026 , archivePrefix =. astro-ph/0511811 , primaryClass =

    Pith/arXiv arXiv

  21. [21]

    , keywords =

    Compact Binary Merger Rates: Comparison with LIGO/Virgo Upper Limits. , keywords =. doi:10.3847/0004-637X/819/2/108 , archivePrefix =. 1510.04615 , primaryClass =

    Pith/arXiv arXiv

  22. [22]

    , keywords =

    Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes. , keywords =. doi:10.1051/0004-6361/201936528 , archivePrefix =. 1706.07053 , primaryClass =

    Pith/arXiv arXiv

  23. [23]

    , keywords =

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

    Pith/arXiv arXiv

  24. [24]

    Physical properties of the most massive stars in R136

    The R136 star cluster dissected with Hubble Space Telescope/STIS - II. Physical properties of the most massive stars in R136. , keywords =. doi:10.1093/mnras/staa2801 , archivePrefix =. 2009.05136 , primaryClass =

    Pith/arXiv arXiv 2009

  25. [25]

    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. , keywords =. doi:10.1051/0004-6361/202038384 , archivePrefix =. 2008.06066 , primaryClass =

    Pith/arXiv arXiv 2008

  26. [26]

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

    Pith/arXiv arXiv

  27. [27]

    , keywords =

    Binarity at LOw Metallicity (BLOeM): Multiplicity properties of Oe and Be stars. , keywords =. doi:10.1051/0004-6361/202452623 , archivePrefix =. 2502.02641 , primaryClass =

    Pith/arXiv arXiv

  28. [28]

    , keywords =

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

    Pith/arXiv arXiv

  29. [29]

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

    Pith/arXiv arXiv

  30. [31]

    , keywords =

    COSMIC Variance in Binary Population Synthesis. , keywords =. doi:10.3847/1538-4357/ab9d85 , archivePrefix =. 1911.00903 , primaryClass =

    Pith/arXiv arXiv 1911

  31. [32]

    , 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 =

    arXiv 2007

  32. [33]

    The IACOB project. VIII. Searching for empirical signatures of binarity in fast-rotating O-type stars. , keywords =. doi:10.1051/0004-6361/202245145 , archivePrefix =. 2302.01349 , primaryClass =

    Pith/arXiv arXiv

  33. [34]

    , keywords =

    The impact of asteroseismically calibrated internal mixing on nucleosynthetic wind yields of massive stars. , keywords =. doi:10.1051/0004-6361/202449634 , archivePrefix =. 2406.02404 , primaryClass =

    Pith/arXiv arXiv

  34. [35]

    , keywords =

    Mixing due to internal gravity waves can explain the CNO surface abundances of B-type detached eclipsing binaries and single stars. , keywords =. doi:10.1051/0004-6361/202555888 , archivePrefix =. 2507.20785 , primaryClass =

    arXiv

  35. [36]

    , year = 1955, month = jan, volume =

    Apsidal-motion constants for polytropic models. , year = 1955, month = jan, volume =. doi:10.1093/mnras/115.1.101 , adsurl =

    doi:10.1093/mnras/115.1.101 1955

  36. [37]

    Rotating massive main-sequence stars. I. Grids of evolutionary models and isochrones. , keywords =. doi:10.1051/0004-6361/201016113 , archivePrefix =. 1102.0530 , primaryClass =

    Pith/arXiv arXiv

  37. [38]

    Rotating massive main-sequence stars. II. Simulating a population of LMC early B-type stars as a test of rotational mixing. , keywords =. doi:10.1051/0004-6361/201016114 , archivePrefix =. 1102.0766 , primaryClass =

    Pith/arXiv arXiv

  38. [39]

    Massive stellar triples on the edge: A numerical study of the evolution and final outcomes of destabilized massive triples

    Massive stellar triples on the edge: A numerical study of the evolution and final outcomes of destabilized massive triples. arXiv e-prints , keywords =. doi:10.48550/arXiv.2408.11128 , archivePrefix =. 2408.11128 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2408.11128

  39. [40]

    , keywords =

    Massive stellar triples on the edge: A numerical study of the evolution and final outcomes of destabilised massive triples. , keywords =. doi:10.1051/0004-6361/202451900 , archivePrefix =. 2408.11128 , primaryClass =

    Pith/arXiv arXiv

  40. [41]

    Current problems in stellar evolution

    Current problems in stellar evolution. arXiv e-prints , keywords =. doi:10.48550/arXiv.1902.10399 , archivePrefix =. 1902.10399 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1902.10399 1902

  41. [42]

    Reviews of Modern Physics , year = 1957, month = jan, volume =

    Synthesis of the Elements in Stars. Reviews of Modern Physics , year = 1957, month = jan, volume =. doi:10.1103/RevModPhys.29.547 , adsurl =

    doi:10.1103/revmodphys.29.547 1957

  42. [44]

    Nature Astronomy , keywords =

    A calibration point for stellar evolution from massive star asteroseismology. Nature Astronomy , keywords =. doi:10.1038/s41550-023-01978-y , archivePrefix =. 2306.11798 , primaryClass =

    Pith/arXiv arXiv

  43. [45]

    , keywords =

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

    Pith/arXiv arXiv

  44. [46]

    , keywords =

    Effect of horizontal turbulent diffusion on transport by meridional circulation. , keywords =

  45. [47]

    Mesa Isochrones and Stellar Tracks (MIST). I. Solar-scaled Models. , keywords =. doi:10.3847/0004-637X/823/2/102 , archivePrefix =. 1604.08592 , primaryClass =

    Pith/arXiv arXiv

  46. [48]

    , keywords =

    The moment of inertia of main sequence stars. , keywords =

  47. [49]

    , keywords =

    Evolutionary stellar models using Rogers & Iglesias opacities, with particular attention to internal structure constants. , keywords =

  48. [50]

    Studies on stellar rotation. I. The theoretical apsidal motion for evolved rotating stars. , keywords =

  49. [51]

    New grids of stellar models including tidal-evolution constants up to carbon burning. I. From 0.8 to 125 M _ at Z=0.02. , keywords =. doi:10.1051/0004-6361:20040470 , adsurl =

    doi:10.1051/0004-6361:20040470

  50. [52]

    , keywords =

    The apsidal-motion test of stellar structure and evolution: an update. , keywords =. doi:10.1051/0004-6361/201014008 , adsurl =

    work page doi:10.1051/0004-6361/201014008

  51. [53]

    , keywords =

    Gravity and limb-darkening coefficients for the Kepler, CoRoT, Spitzer, uvby, UBVRIJHK, and Sloan photometric systems. , keywords =. doi:10.1051/0004-6361/201116451 , adsurl =

    doi:10.1051/0004-6361/201116451

  52. [54]

    Calculations from 0.40 M _ to 25.0 M _

    An approach to the effects of stellar rotation on the theoretical apsidal motion constants. Calculations from 0.40 M _ to 25.0 M _. , keywords =. doi:10.1051/0004-6361/202449379 , adsurl =

    work page doi:10.1051/0004-6361/202449379

  53. [55]

    , keywords =

    Discs and outflows in the early phases of massive star formation: Influence of magnetic fields and ambipolar diffusion. , keywords =. doi:10.1051/0004-6361/202037479 , archivePrefix =. 2109.10580 , primaryClass =

    Pith/arXiv arXiv

  54. [56]

    Spectroscopic studies of O-type stars. VII. Rotational velocities V sin i and evidence for macroturbulent motions. , year = 1977, month = apr, volume =. doi:10.1086/155173 , adsurl =

    work page doi:10.1086/155173 1977

  55. [57]

    , keywords =

    Evolutionary tracks, ejecta, and ionizing photons from intermediate-mass to very massive stars with PARSEC. , keywords =. doi:10.1051/0004-6361/202452573 , archivePrefix =. 2501.12917 , primaryClass =

    Pith/arXiv arXiv

  56. [59]

    , keywords =

    Physical parameters and wind properties of galactic early B supergiants. , keywords =. doi:10.1051/0004-6361:20053685 , archivePrefix =. astro-ph/0509436 , primaryClass =

    Pith/arXiv arXiv

  57. [60]

    Astronomy & Geophysics , volume =

    Crowther, Paul , title = ". Astronomy & Geophysics , volume =. 2012 , month =. doi:10.1111/j.1468-4004.2012.53430.x , url =

    arXiv 2012

  58. [61]

    , year = 1997, month = jul, volume =

    Eta Carinae: a long period binary?. , year = 1997, month = jul, volume =. doi:10.1016/S1384-1076(97)00008-0 , adsurl =

    work page doi:10.1016/s1384-1076(97)00008-0 1997

  59. [62]

    , keywords =

    The modelling of feedback in star formation simulations. , keywords =. doi:10.1016/j.newar.2015.06.001 , archivePrefix =. 1508.06054 , primaryClass =

    Pith/arXiv arXiv 2015

  60. [63]

    , year = 1997, month = oct, volume =

    Is Eta Carinae a long-period binary?. , year = 1997, month = oct, volume =. doi:10.1016/S1384-1076(97)00028-6 , adsurl =

    work page doi:10.1016/s1384-1076(97)00028-6 1997

  61. [64]

    , keywords =

    Mass transfer in eccentric binary systems using the binary evolution code BINSTAR. , keywords =. doi:10.1051/0004-6361/201220391 , archivePrefix =. 1305.6092 , primaryClass =

    Pith/arXiv arXiv

  62. [65]

    Binary evolution using the theory of osculating orbits. I. Conservative Algol evolution. , keywords =. doi:10.1051/0004-6361/201423730 , archivePrefix =. 1408.4303 , primaryClass =

    Pith/arXiv arXiv

  63. [66]

    The IACOB project. X. Large-scale quantitative spectroscopic analysis of Galactic luminous blue stars. , keywords =. doi:10.1051/0004-6361/202348808 , archivePrefix =. 2312.00241 , primaryClass =

    Pith/arXiv arXiv

  64. [67]

    New clues on the location of the TAMS in the massive star domain

    The IACOB project: XIV. New clues on the location of the TAMS in the massive star domain. , keywords =. doi:10.1051/0004-6361/202453242 , archivePrefix =. 2501.17984 , primaryClass =

    Pith/arXiv arXiv

  65. [68]

    , keywords =

    Seismic constraints on the radial dependence of the internal rotation profiles of six Kepler subgiants and young red giants. , keywords =. doi:10.1051/0004-6361/201322779 , archivePrefix =. 1401.3096 , primaryClass =

    Pith/arXiv arXiv

  66. [69]

    , keywords =

    Mass loss rates in the Hertzsprung-Russell diagram. , keywords =

  67. [70]

    , keywords =

    Massive binaries as the source of abundance anomalies in globular clusters. , keywords =. doi:10.1051/0004-6361/200913205 , archivePrefix =. 0910.1086 , primaryClass =

    Pith/arXiv arXiv

  68. [71]

    , keywords =

    The Rotation Rates of Massive Stars: The Role of Binary Interaction through Tides, Mass Transfer, and Mergers. , keywords =. doi:10.1088/0004-637X/764/2/166 , archivePrefix =. 1211.3742 , primaryClass =

    Pith/arXiv arXiv

  69. [72]

    , keywords =

    Gamma-ray bursts from tidally spun-up Wolf-Rayet stars?. , keywords =. doi:10.1051/0004-6361:200809371 , archivePrefix =. 0804.0014 , primaryClass =

    Pith/arXiv arXiv

  70. [73]

    , year = 1952, month = aug, volume =

    The Brightening of Carinae. , year = 1952, month = aug, volume =. doi:10.1086/126457 , adsurl =

    work page doi:10.1086/126457 1952

  71. [74]

    , keywords =

    The VLT-FLAMES survey of massive stars: stellar parameters and rotational velocities in NGC 3293, NGC 4755 and NGC 6611. , keywords =. doi:10.1051/0004-6361:20065392 , archivePrefix =. astro-ph/0606409 , primaryClass =

    Pith/arXiv arXiv

  72. [75]

    , keywords =

    Stellar triples with chemically homogeneously evolving inner binaries. , keywords =. doi:10.1093/mnras/stad3819 , archivePrefix =. 2307.04793 , primaryClass =

    Pith/arXiv arXiv

  73. [76]

    The VLT-FLAMES Tarantula Survey. X. Evidence for a bimodal distribution of rotational velocities for the single early B-type stars. , keywords =. doi:10.1051/0004-6361/201220273 , archivePrefix =. 1212.2424 , primaryClass =

    Pith/arXiv arXiv

  74. [77]

    Asteroseismology of the Cep star HD 129929. II. Seismic constraints on core overshooting, internal rotation and stellar parameters. , keywords =. doi:10.1051/0004-6361:20034143 , adsurl =

    doi:10.1051/0004-6361:20034143

  75. [78]

    , keywords =

    The two hybrid B-type pulsators: Eridani and 12 Lacertae. , keywords =. doi:10.1111/j.1365-2966.2008.12964.x , archivePrefix =. 0801.2451 , primaryClass =

    arXiv 2008

  76. [79]

    The Observatory , year = 1925, month = mar, volume =

    Circulating currents in rotating stars. The Observatory , year = 1925, month = mar, volume =

    1925

  77. [80]

    , keywords =

    The blue to red supergiant ratio in young clusters at various metallicities. , keywords =. doi:10.1051/0004-6361:20020262 , archivePrefix =. astro-ph/0202478 , primaryClass =

    Pith/arXiv arXiv

  78. [81]

    , keywords =

    The Geneva stellar evolution code. , keywords =. doi:10.1007/s10509-007-9511-y , adsurl =

    doi:10.1007/s10509-007-9511-y

  79. [82]

    , keywords =

    Aproximations to the radii of Roche lobes. , keywords =. doi:10.1086/160960 , adsurl =

    doi:10.1086/160960

  80. [83]

    , keywords =

    Angular momentum transport in stellar interiors constrained by rotational splittings of mixed modes in red giants. , keywords =. doi:10.1051/0004-6361/201219729 , archivePrefix =. 1207.1023 , primaryClass =

    Pith/arXiv arXiv

Showing first 80 references.