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REVIEW 3 major objections 4 minor 295 references

Galactic OB stars demand more convective-core mixing than standard stellar models assume.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-08-04 05:03 UTC pith:FQK2RIXN

load-bearing objection A careful, reproducible Bayesian calibration of overshooting in 12–40 Msun stars that yields a constant α_ov ≈ 0.33 and larger He cores — worth serious referee time, though the background-model systematic likely exceeds the quoted statistical error. the 3 major comments →

arxiv 2608.02540 v1 pith:FQK2RIXN submitted 2026-08-03 astro-ph.SR

You're Gonna Need a Bigger Core: Calibrating Massive Star Models against Galactic OB-type Stars

Thibault Lechien , Selma E. de Mink , Stephen Justham , Abel de Burgos , Ruggero Valli , Sergio Sim\'on-D\'iaz This is my paper
classification astro-ph.SR
keywords massive starsconvective overshootingstellar evolutionHertzsprung–Russell diagramterminal-age main sequencehelium core massGalactic OB starsBayesian inference
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 tries to establish how much extra mixing occurs just beyond the convective core of massive stars during their main-sequence lifetime. By comparing a synthetic population of stellar evolution tracks to the observed distribution of more than 900 Galactic OB-type stars in the Hertzsprung–Russell diagram, the authors find that a constant convective-boundary mixing parameter of α_ov = 0.33 ± 0.02 (or an exponential-overshoot equivalent f_ov = 0.028 ± 0.003) best describes stars from 12 to 40 solar masses. This is appreciably larger than the overshooting lengths used in several widely adopted model grids. If the finding is right, massive-star helium cores are 10–40% more massive than those grids predict, which shifts the predicted end of the main sequence, the timing of mass transfer in binaries, and the ionizing output of stellar populations. The paper combines its high-mass constraint with lower-mass calibrations to propose a mass-dependent overshooting recipe across 1.2 to 40 solar masses.

Core claim

The paper's central claim is that the terminal-age main sequence of Galactic OB stars, located directly from the data as a drop in number density in the HR diagram, cannot be reproduced by commonly used overshooting prescriptions. Forward-modeling the population with a grid of main-sequence tracks, the inference favors a constant overshooting length of α_ov = 0.33 ± 0.02 over the 12–40 solar-mass range, with an exponential-diffusion equivalent of f_ov = 0.028 ± 0.003. The data provide no support for the rising overshooting-with-mass trend seen at lower masses; they are consistent with either a constant or a mildly decreasing prescription. A consequence is that the helium-core mass at the end

What carries the argument

The machinery is a forward model of a stellar population: a grid of main-sequence tracks computed for many initial masses and overshooting lengths, a Salpeter initial mass function with continuous star formation sampled into a synthetic HR diagram, and a two-component likelihood (main sequence plus uniform background) evaluated with nested sampling. The parameter being constrained, the convective-boundary mixing length α_ov (or f_ov), controls how far mixing extends beyond the formal convective core; moving it changes where tracks leave the main sequence and hence where the predicted density drop lands.

Load-bearing premise

The inference assumes that the observed HR-diagram density drop is produced by single-star main-sequence evolution diluted by a uniform background, so if selection effects or binary merger products preferentially populate that boundary, the fitted overshooting length is biased.

What would settle it

Measure the average convective-core overshoot of a dozen 12–40 solar-mass stars asteroseismically or via apsidal-motion constraints; if the mean lies clearly below about 0.25 with small scatter, the central calibration of α_ov ≈ 0.33 fails.

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

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If this is right

  • If the calibration is right, commonly used model grids under-predict the helium-core mass of a 12–40 solar-mass star by 10–40%.
  • The data-driven terminal-age main sequence is systematically cooler than the TAMS assumed in many existing models, shifting inferred ages and masses of OB stars.
  • Because core growth sets the timing of binary mass transfer, predictions for post-main-sequence binary products and compact remnants will change.
  • The proposed mass-dependent recipe from 1.2 to 40 solar masses offers population and spectral synthesis codes a single consistent overshooting prescription across the whole mass range.
  • The public set of calibrated main-sequence tracks allows other studies to adopt the calibration directly.

Where Pith is reading between the lines

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

  • If the ~33% background fraction includes many binary-interaction products near the main-sequence boundary, the fitted overshoot may partly absorb population complexity rather than pure single-star mixing; comparing binary-rich and binary-poor subsamples would separate these effects.
  • Applying the same forward-modeling to similarly complete OB-star samples in lower-metallicity galaxies would test whether the inferred overshooting length depends on metallicity, which the current calibration cannot constrain.
  • Because larger cores shorten the main-sequence lifetime and change the initial-to-final core-mass mapping, the calibration may shift predicted black-hole mass distributions and gravitational-wave merger rates from population synthesis.
  • The intermediate branch of the proposed mass-dependent recipe (4–12 solar masses) is a linear interpolation rather than a directly measured constraint, so asteroseismic or binary targets in that gap could confirm or break the prescription.

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

3 major / 4 minor

Summary. The paper calibrates convective boundary mixing in massive stars by forward-modeling the HR-diagram distribution of the IACOB sample (604 stars with Gaia-based luminosities) with MESA evolution tracks and a Bayesian mixture likelihood. The central result is that a constant overshooting parameter in the 12–40 Msun range is preferred, with alpha_ov = 0.33 ± 0.02 (step) or f_ov = 0.028 ± 0.003 (exponential), and that this differs from extrapolations of low-mass calibrations. The authors also derive a model-dependent TAMS location, explore mass-dependent overshooting prescriptions, compare with prior theoretical and empirical constraints, and provide calibrated tracks and a combined prescription for 1.2–40 Msun (Eqs. 3–4). Robustness experiments include alternative winds, rotation, MLT++, exponential overshooting, and distance cuts.

Significance. If the calibration holds, this is a valuable population-level constraint in a mass range where direct constraints are scarce, with clear implications for population synthesis, binary evolution, and compact-object predictions. The paper’s strengths include a transparent forward-modeling framework, careful nested-sampling inference, model-comparison experiments with Bayes factors, public MESA grids and inlists on Zenodo, and explicit discussion of caveats. However, the headline uncertainty (0.02) is purely statistical and does not include model systematics that, on the paper’s own numbers, can be several times larger.

major comments (3)
  1. [§3.2, Table B.2] The claim that the calibration is “robust to moderate changes in the adopted stellar-physics assumptions” is not supported by the wind-systematic results. The default Pauli+25 grid gives alpha_ov = 0.332 ± 0.024, while the Dutch (Vink/de Jager) grid gives alpha_ov = 0.228 ± 0.013. The difference of ~0.10 is roughly five to eight times the reported statistical uncertainty, and it directly affects the recommended high-mass branch of Eqs. (3) and (4) and the helium-core mass comparison in Fig. 7. The authors need either to justify why the Pauli+25 wind scheme is the appropriate physical choice for these stars or to quote a combined systematic uncertainty that incorporates the Dutch-grid result. As written, the abstract’s “alpha_ov = 0.33 ± 0.02” understates the model dependence of the central value.
  2. [§4.5, Eq. (2), Appendix B.4] The uniform-background contamination model is a load-bearing assumption. With pi_bg ≈ 0.33, roughly one third of the sample is assigned to a component whose only role is to absorb stars not described by single-star main-sequence evolution. The observed density drop that pins alpha_ov is assumed to be the TAMS, but if real contaminants—binary products, merger remnants, post-MS objects, or selection effects—are concentrated in the cool, luminous region, the fit will compensate by shifting the effective TAMS and biasing alpha_ov upward. The sentence “this may lead to a bias in the inferred overshooting length” is acknowledged but not quantified. A necessary robustness test is to replace the uniform background with alternative templates (e.g., empirical post-MS distributions, two-component backgrounds, or contamination localized near the upper TAMS) and report the resulting shift in alpha_ov
  3. [§3.3, Figure 3] The “data-driven” TAMS is not an independent empirical constraint: it is the boundary of the same MESA models whose overshooting parameter is fitted to the data. This does not invalidate the calibration, since the likelihood does not use a pre-defined TAMS, but the comparison with Castro+14 and de Burgos+25 should be framed as consistency between a model output and previous empirical boundaries. If the paper intends the TAMS location to be used as a constraint by other studies, this circularity should be stated explicitly. The current wording in Section 1 (“Establish a location of the TAMS using a physics-informed, data-driven method”) risks overstating its independence.
minor comments (4)
  1. [§2.1] Typo: “could by caused by selection effects” should read “could be caused by selection effects.”
  2. [Eq. (3)] The low-mass branch is difficult to read as typeset; the expression “11.36 0.02013 / (1+e^{-5.5(M-1.47)}) - 0.00373” appears to be a logistic plus offset. Please format it unambiguously and verify that the plotted curve matches Eq. (3).
  3. [§3.1, Table B.3] The statement that constant and decreasing prescriptions receive “comparable support” is accurate, but the text in Section 3.1 says the data “favor a decrease” before the model-comparison caveat; consider rewording to avoid implying a trend that the evidence does not decisively support.
  4. [Appendix B.4] The corner plot in Fig. B.1 reports alpha_edge, but the paper does not discuss the implications of alpha_edge ≈ 0.15 for stars above 40 Msun. Since those stars are included in the mass-dependent grids and could affect the high-mass tail, a sentence explaining why this parameter is not relevant to the main conclusions would be helpful.

Circularity Check

0 steps flagged

No significant circularity: the paper is an explicit calibration, and the derived TAMS and core masses are model outputs of the fitted overshoot parameter, not independent predictions.

full rationale

The paper is openly a calibration study: the overshooting parameter is a free parameter of forward MESA models and is inferred from the observed IACOB HR diagram through the mixture likelihood in Eqs. (1)-(2). The reported TAMS location and helium-core masses are deterministic outputs of the best-fit tracks, not quantities that were fed into the inference as constraints. There is therefore no equation-level identity or statistically forced 'prediction' between the fitted parameter and the headline results. The main caveat that could superficially resemble circularity is the uniform-background component (π_bg ≈ 33%, Section B.4), but the authors explicitly flag it as a potential bias: 'As these are likely not uniformly distributed, this may lead to a bias in the inferred overshooting length' (Section 4.5). This is a model systematic and an acknowledged limitation, not a circular reduction of the derivation to its inputs. Self-citations to the IACOB project and de Burgos et al. (2025) provide the dataset and a previous TAMS estimate used for comparison, but the inference does not load-bearingly depend on those citations. The central numerical result is a fitted calibration; the quoted ±0.02 uncertainty is statistical, and the background-model bias is a correctness concern rather than a circularity.

Axiom & Free-Parameter Ledger

5 free parameters · 6 axioms · 0 invented entities

The inference is only as good as the population prior, contamination model, and stellar input physics: one fitted parameter α_ov carries most of the calibrating weight, and several domain assumptions are load-bearing. No new physical entities are introduced; the background component is a statistical nuisance, not an invented physical object.

free parameters (5)
  • α_ov (step overshoot, 12–40 M_sun) = 0.332 ± 0.024 (reported as 0.33 ± 0.02)
    The central fitted parameter; sets the TAMS temperature and therefore the HR-diagram density drop.
  • f_ov (exponential overshoot, 12–40 M_sun) = 0.0279 ± 0.003
    Alternative overshoot scheme fitted with the 'Exp' grid.
  • π_bg (background fraction) = 0.331 ± 0.038
    Mixture weight in Eq. (2); about one third of the sample is assigned to the non-main-sequence background.
  • α_edge (overshoot for M > 40 M_sun) = 0.151 (+0.098/−0.088)
    Separate nuisance parameter preventing the scarce highest-mass stars from biasing the 12–40 M_sun result.
  • Mass-dependence slopes (linear/log-linear/exponential/quadratic) = e.g. log M linear: 0.881 − 0.423 log10(M)
    Fitted in model-comparison runs (Table B.2); decreasing slopes prefer a downward trend, but Bayes factors do not strongly favor them over constant.
axioms (6)
  • domain assumption Population prior: Salpeter IMF (slope −2.35) and continuous star formation history.
    Used in Eq. (1) as p(M,t|θ); the relative weighting of model points across the HR diagram directly affects the best-fit α_ov.
  • domain assumption Uniform background component absorbs all non-single-star-main-sequence contaminants.
    Eq. (2) with L_bg = 1/A_HR; Section 4.5 acknowledges this may bias α_ov.
  • domain assumption Effective overshooting length is constant over the main sequence and identical for all stars of a given mass.
    Section 4.5; simulations find time- and star-dependent overshooting, so the inferred value is a lifetime-averaged effective parameter.
  • domain assumption Default wind mass-loss prescription of Pauli et al. (2025) is used for the main grid.
    Section 2.2 / Appendix A; if the Dutch scheme is used instead, best-fit α_ov drops to 0.228 ± 0.013 (Section 3.2).
  • domain assumption MESA input physics (Cox MLT with α_MLT=1.82, Ledoux criterion with α_sc=1.0, 23-isotope network) is adequate for main-sequence massive stars.
    Appendix A lists these choices; they are standard but not derived in the paper.
  • domain assumption IACOB sample after cuts (d<2.5 kpc, log L/L_sun > 4.5) is representative enough for population inference.
    Section 2.1; the luminosity cut is motivated by slow-rotator selection effects but residual selection bias remains possible.

pith-pipeline@v1.3.0-daily-deepseek · 21596 in / 15554 out tokens · 164646 ms · 2026-08-04T05:03:44.909816+00:00 · methodology

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Cite this review

Pith. "Pith review of You're Gonna Need a Bigger Core: Calibrating Massive Star Models against Galactic OB-type Stars." pith.science (2026). https://pith.science/paper/FQK2RIXN

@misc{pith2026260802540,
  author       = {Pith},
  title        = {Pith review of: You're Gonna Need a Bigger Core: Calibrating Massive Star Models against Galactic OB-type Stars},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/FQK2RIXN}},
  note         = {Machine review of arXiv:2608.02540}
}
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read the original abstract

The evolution of massive stars above 8 M$_\odot$ depends critically on the amount of mixing above the convective core during the main sequence. However, current models typically extrapolate results from lower-mass stars, where constraints from asteroseismology and eclipsing binary systems are more readily available. A new opportunity to study the evolution of massive stars and their distribution in the Hertzsprung--Russell diagram arises by combining the IACOB spectroscopic sample of over 900 Galactic OB-type stars with Gaia distances. We use this homogeneously analyzed sample to place population-level constraints on main-sequence evolution. We analyze the data by forward modeling stellar evolution tracks with MESA and applying Bayesian inference. This enables us to 1) determine a physically-motivated, data-driven location of the terminal-age main sequence, 2) constrain convective boundary mixing and resulting core masses, and 3) provide a set of massive star models calibrated against modern data. We explore how boundary mixing depends on mass and find that it is well described by a constant overshooting parameter in the mass range of 12 to 40 M$_\odot$, with $\alpha_{\mathrm{ov}} = 0.33 \pm 0.02$, or $f_{\mathrm{ov}} = 0.028 \pm 0.003$ in the step and exponential overshooting schemes respectively. We find evidence against a continuation of the trend to increase with mass that is found at lower masses. Instead, the data does not exclude a decreasing trend at the high mass end. We find that the resulting helium core masses are 10 to 40% larger than other commonly used overshooting prescriptions. Combining our findings with existing observational constraints for low- and intermediate-mass stars, we propose a new mass-dependent overshooting prescription for a wide range of masses. Our calibration and model set are particularly useful for population and spectral synthesis applications.

Figures

Figures reproduced from arXiv: 2608.02540 by Abel de Burgos, Ruggero Valli, Selma E. de Mink, Sergio Sim\'on-D\'iaz, Stephen Justham, Thibault Lechien.

Figure 1
Figure 1. Figure 1: The observed density distribution in the IACOB sample [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Varying the overshooting length and comparing a synthetic population of stars to the observed data in the HR diagram finds [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of the location of our proposed TAMS in the [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: A comparison of a wide range of observationally derived constraints on overshooting (from asteroseismology, eclipsing [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of our best-fit overshooting value with (a) predictions from convection simulations and (b) other common [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Comparison of the location of our physically-motivated, [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Comparison of the helium core mass at the TAMS of our [PITH_FULL_IMAGE:figures/full_fig_p007_7.png] view at source ↗

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Reference graph

Works this paper leans on

295 extracted references · 56 canonical work pages · 12 internal anchors

  1. [1]

    Webbink, R. F. , editor =. Stellar Evolution and Binaries , booktitle =

  2. [2]

    Abbott, B. P. and Abbott, R. and Abbott, T. D. and Abernathy, M. R. and Acernese, F. and Ackley, K. and Adams, C. and Adams, T. and Addesso, P. and Adhikari, R. X. and Adya, V. B. and Affeldt, C. and Agathos, M. and Agatsuma, K. and Aggarwal, N. and Aguiar, O. D. and Aiello, L. and Ain, A. and Ajith, P. and Allen, B. and Allocca, A. and Altin, P. A. and A...

    2041

  3. [3]

    and Abbott, T

    Abbott, R. and Abbott, T. D. and Acernese, F. and Ackley, K. and Adams, C. and Adhikari, N. and Adhikari, R. X. and Adya, V. B. and Affeldt, C. and Agarwal, D. and Agathos, M. and Agatsuma, K. and Aggarwal, N. and Aguiar, O. D. and Aiello, L. and Ain, A. and Ajith, P. and Akcay, S. and Akutsu, T. and Albanesi, S. and Allocca, A. and Altin, P. A. and Amato...

  4. [4]

    Energy Optimization in Binary Star Systems: Explanation for Equal Mass Members in Close Orbits , shorttitle =

    Adams, Fred C and Batygin, Konstantin and Bloch, Anthony M , year = 2020, month = may, journal =. Energy Optimization in Binary Star Systems: Explanation for Equal Mass Members in Close Orbits , shorttitle =. doi:10.1093/mnras/staa850 , urldate =

    work page doi:10.1093/mnras/staa850 2020

  5. [5]

    Aerts, Conny and Mathis, St. Angular. Annual Review of Astronomy and Astrophysics , volume =. doi:10.1146/annurev-astro-091918-104359 , urldate =

    doi:10.1146/annurev-astro-091918-104359

  6. [6]

    and Molenberghs, G

    Aerts, C. and Molenberghs, G. and Michielsen, M. and Pedersen, M. G. and Bj. Forward. The Astrophysical Journal Supplement Series , volume =. doi:10.3847/1538-4365/aaccfb , urldate =

    doi:10.3847/1538-4365/aaccfb

  7. [7]

    Reviews of Modern Physics , volume =

    Probing the Interior Physics of Stars through Asteroseismology , author =. Reviews of Modern Physics , volume =. doi:10.1103/RevModPhys.93.015001 , urldate =

    doi:10.1103/revmodphys.93.015001

  8. [8]

    and Briquet, M

    Aerts, C. and Briquet, M. and Degroote, P. and Thoul, A. and. Seismic Modelling of the. Astronomy and Astrophysics , volume =. doi:10.1051/0004-6361/201117629 , urldate =

    doi:10.1051/0004-6361/201117629

  9. [9]

    Agrawal, Poojan and Hurley, Jarrod and Stevenson, Simon and Rodriguez, Carl L. and Sz. Modelling Stellar Evolution in Mass-Transferring Binaries and Gravitational-Wave Progenitors with. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1093/mnras/stad2334 , urldate =

    doi:10.1093/mnras/stad2334

  10. [10]

    and Kupka, F

    Ahlborn, F. and Kupka, F. and Weiss, A. and Flaskamp, M. , year = 2022, month = nov, journal =. Stellar Evolution Models with Overshooting Based on 3-Equation Non-Local Theories. doi:10.1051/0004-6361/202243126 , urldate =

    work page doi:10.1051/0004-6361/202243126 2022

  11. [11]

    and Carter, Joshua A

    Albrecht, Simon and Winn, Joshua N. and Carter, Joshua A. and Snellen, Ignas A. G. and. The Astrophysical Journal , volume =. doi:10.1088/0004-637X/726/2/68 , urldate =

    work page doi:10.1088/0004-637x/726/2/68

  12. [12]

    and Pedersen, May G

    Anders, Evan H. and Pedersen, May G. , year = 2023, month = apr, journal =. Convective. doi:10.3390/galaxies11020056 , urldate =

    doi:10.3390/galaxies11020056 2023

  13. [13]

    and Jermyn, Adam S

    Anders, Evan H. and Jermyn, Adam S. and Lecoanet, Daniel and Brown, Benjamin P. , year = 2022, month = feb, journal =. Stellar. doi:10.3847/1538-4357/ac408d , urldate =

    doi:10.3847/1538-4357/ac408d 2022

  14. [14]

    The Astrophysical Journal , volume =

    New Strong Evidence for the Importance of Convective Overshooting in Intermediate-Mass Stars , author =. The Astrophysical Journal , volume =. doi:10.1086/185858 , urldate =

    work page doi:10.1086/185858

  15. [15]

    Andrae, Ren. Robust. The Astrophysical Journal Supplement Series , volume =. doi:10.3847/1538-4365/acd53e , urldate =

    doi:10.3847/1538-4365/acd53e

  16. [16]

    and Leidi, G

    Andrassy, R. and Leidi, G. and Higl, J. and Edelmann, P. V. F. and Schneider, F. R. N. and R. Towards a Self-Consistent Model of the Convective Core Boundary in Upper Main Sequence Stars. Astronomy and Astrophysics , volume =. doi:10.1051/0004-6361/202347407 , urldate =

    work page doi:10.1051/0004-6361/202347407

  17. [17]

    and Bavera, Simone S

    Andrews, Jeff J. and Bavera, Simone S. and Briel, Max and Chattaraj, Abhishek and Dotter, Aaron and Fragos, Tassos and. arXiv , keywords =:2411.02376 , publisher =

    Pith/arXiv arXiv

  18. [18]

    Convective Boundary Mixing in Low- and Intermediate-Mass Stars --

    Angelou, George C and Bellinger, Earl P and Hekker, Saskia and Mints, Alexey and Elsworth, Yvonne and Basu, Sarbani and Weiss, Achim , year = 2020, month = apr, journal =. Convective Boundary Mixing in Low- and Intermediate-Mass Stars --. doi:10.1093/mnras/staa390 , urldate =

    doi:10.1093/mnras/staa390 2020

  19. [19]

    nphysa , volume =

    A Compilation of Charged-Particle Induced Thermonuclear Reaction Rates , author =. nphysa , volume =

  20. [20]

    doi:10.48550/arXiv.2510.21385 , urldate =

    Gaia and Massive Stars in 2025 , author =. doi:10.48550/arXiv.2510.21385 , urldate =. arXiv , keywords =:2510.21385 , primaryclass =

    doi:10.48550/arxiv.2510.21385 2025

  21. [21]

    Apell. The. doi:10.48550/arXiv.1010.5680 , urldate =. arXiv , keywords =:1010.5680 , primaryclass =

    Pith/arXiv arXiv doi:10.48550/arxiv.1010.5680

  22. [22]

    Apellaniz, J Ma. The

  23. [23]

    Monthly Notices of the Royal Astronomical Society , volume =

    The Mass Range of Hot Subdwarf. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1093/mnras/stad3891 , urldate =

    doi:10.1093/mnras/stad3891

  24. [24]

    Jacques and Scott, Pat , year = 2009, month = sep, journal =

    Asplund, Martin and Grevesse, Nicolas and Sauval, A. Jacques and Scott, Pat , year = 2009, month = sep, journal =. The. doi:10.1146/annurev.astro.46.060407.145222 , urldate =

    arXiv 2009

  25. [25]

    and Amarsi, A

    Asplund, M. and Amarsi, A. M. and Grevesse, N. , year = 2021, month = sep, journal =. The Chemical Make-up of the. doi:10.1051/0004-6361/202140445 , urldate =

    doi:10.1051/0004-6361/202140445 2021

  26. [26]

    From stellar light to astrophysical insight: automating variable star research with machine learning

    Audenaert, Jeroen , year = 2025, month = jul, publisher =. From Stellar Light to Astrophysical Insight: Automating Variable Star Research with Machine Learning , shorttitle =. doi:10.48550/arXiv.2507.03093 , urldate =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2507.03093 2025

  27. [28]

    The Astronomical Journal , volume =

    Estimating. The Astronomical Journal , volume =. doi:10.3847/1538-3881/abd806 , urldate =

    doi:10.3847/1538-3881/abd806

  28. [29]

    VizieR Online Data Catalog , volume =

  29. [30]

    Learning the Stellar Structure Equations via Self-supervised Physics-Informed Neural Networks

    Ballester, Manuel and. Learning the. doi:10.48550/arXiv.2604.06255 , urldate =. arXiv , keywords =:2604.06255 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2604.06255

  30. [31]

    Bao, Yuchen and Li, Zhenwei and Ge, Hongwei and Chen, Xuefei and Han, Zhanwen , year = 2025, month = jul, journal =. A. doi:10.3847/1538-4357/addfd8 , urldate =

    doi:10.3847/1538-4357/addfd8 2025

  31. [32]

    Monthly Notices of the Royal Astronomical Society , volume =

    A Study of Convective Core Overshooting as a Function of Stellar Mass Based on Two-Dimensional Hydrodynamical Simulations , author =. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1093/mnras/stad009 , urldate =

    doi:10.1093/mnras/stad009

  32. [33]

    and Mandel, Ilya and Neijssel, Coenraad J

    Barrett, Jim W. and Mandel, Ilya and Neijssel, Coenraad J. and Stevenson, Simon and. Exploring the. Proceedings of the International Astronomical Union , volume =. doi:10.1017/S1743921317000059 , urldate =

    work page doi:10.1017/s1743921317000059

  33. [34]

    Astronomy & Astrophysics , volume =

    The Impact of Mass-Transfer Physics on the Observable Properties of Field Binary Black Hole Populations , author =. Astronomy & Astrophysics , volume =. doi:10.1051/0004-6361/202039804 , urldate =

    doi:10.1051/0004-6361/202039804

  34. [35]

    Belczynski, Krzysztof and Kalogera, Vassiliki and Bulik, Tomasz , year = 2002, month = jun, journal =. A. doi:10.1086/340304 , urldate =

    doi:10.1086/340304 2002

  35. [36]

    and Angelou, George C

    Bellinger, Earl P. and Angelou, George C. and Hekker, Saskia and Basu, Sarbani and Ball, Warrick H. and Guggenberger, Elisabeth , year = 2016, month = oct, journal =. Fundamental. doi:10.3847/0004-637X/830/1/31 , urldate =

    doi:10.3847/0004-637x/830/1/31 2016

  36. [37]

    Bellinger, Earl Patrick and. The. The Astrophysical Journal Letters , volume =. doi:10.3847/2041-8213/ad4990 , urldate =

    doi:10.3847/2041-8213/ad4990 2041

  37. [38]

    Berlanas, S. R. and Mahy, L. and Herrero, A. and Apell. Gaia-. doi:10.48550/arXiv.2501.16508 , urldate =. arXiv , keywords =:2501.16508 , primaryclass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2501.16508

  38. [40]

    Bestenlehner, J. M. and Crowther, Paul A. and Bronner, V. A. and. Binarity at. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1093/mnras/staf900 , urldate =

    doi:10.1093/mnras/staf900

  39. [41]

    Astronomy and Astrophysics , volume =

    A Self-Consistent Solution for an Accretion Disc Structure around a Rapidly Rotating Non-Magnetized Star , author =. Astronomy and Astrophysics , volume =

  40. [42]

    New Predictions for Radiation-Driven, Steady-State Mass-Loss and Wind-Momentum from Hot, Massive Stars

    Bj. New Predictions for Radiation-Driven, Steady-State Mass-Loss and Wind-Momentum from Hot, Massive Stars. Astronomy and Astrophysics , volume =. doi:10.1051/0004-6361/202141948 , urldate =

    doi:10.1051/0004-6361/202141948

  41. [43]

    and Richards, Mercedes T

    Blondin, John M. and Richards, Mercedes T. and Malinowski, Michael L. , year = 1995, month = jun, journal =. Hydrodynamic. doi:10.1086/175753 , urldate =

    work page doi:10.1086/175753 1995

  42. [44]

    and Saumon, Didier and Starrett, Charles E

    Blouin, Simon and Shaffer, Nathaniel R. and Saumon, Didier and Starrett, Charles E. , year = 2020, month = aug, journal =. New. doi:10.3847/1538-4357/ab9e75 , keywords =

    doi:10.3847/1538-4357/ab9e75 2020

  43. [45]

    , year = 1971, month = jul, journal =

    Bodenheimer, P. , year = 1971, month = jul, journal =. Rapidly Rotating Stars. doi:10.1086/151014 , adsnote =

    work page doi:10.1086/151014 1971

  44. [46]

    Binarity at Low Metallicity (BLOeM) -- Multiplicity properties of Oe and Be stars

    Bodensteiner, J. and Shenar, T. and Sana, H. and Britavskiy, N. and Crowther, P. A. and Langer, N. and Lennon, D. J. and Mahy, L. and Patrick, L. R. and Villase. Binarity at. doi:10.48550/arXiv.2502.02641 , urldate =. arXiv , keywords =:2502.02641 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2502.02641

  45. [47]

    and Shenar, T

    Bodensteiner, J. and Shenar, T. and Sana, H. , year = 2020, month = sep, journal =. Investigating the Lack of Main-Sequence Companions to Massive. doi:10.1051/0004-6361/202037640 , urldate =

    doi:10.1051/0004-6361/202037640 2020

  46. [48]

    and Shenar, T

    Bodensteiner, J. and Shenar, T. and Mahy, L. and Fabry, M. and Marchant, P. and. Is. Astronomy & Astrophysics , volume =. doi:10.1051/0004-6361/202038682 , urldate =

    doi:10.1051/0004-6361/202038682

  47. [49]

    Constraining Accretion Efficiency in Massive Binary Stars with

    Bouffanais, Yann and Mapelli, Michela and Santoliquido, Filippo and Giacobbo, Nicola and Iorio, Giuliano and Costa, Guglielmo , year = 2021, month = jun, journal =. Constraining Accretion Efficiency in Massive Binary Stars with. doi:10.1093/mnras/stab1589 , urldate =

    work page doi:10.1093/mnras/stab1589 2021

  48. [50]

    and Harmanec, P

    Bozic, H. and Harmanec, P. and Horn, J. and Koubsky, P. and Scholz, G. and McDavid, D. and Hubert, A. -M. and Hubert, H. , year = 1995, month = dec, journal =. Toward a Consistent Model of the

    1995

  49. [51]

    Braun, Teresa A. M. , year = 2026, month = feb, address =. Application of Non-Local Convection Theories to Stellar Evolution:

    2026

  50. [52]

    , author =

    Effects of Accretion onto Massive Main Sequence Stars. , author =. Astronomy and Astrophysics , volume =

  51. [53]

    Braun, T. A. M. and Ahlborn, F. and Weiss, A. , year = 2024, month = sep, journal =. Testing a Non-Local 1-Equation Turbulent Convection Model:. doi:10.1051/0004-6361/202450511 , urldate =

    work page doi:10.1051/0004-6361/202450511 2024

  52. [54]

    Braun, T. A. M. and Ahlborn, F. and Kupka, F. and Weiss, A. , year = 2026, month = may, journal =. Testing the 3-Equation. doi:10.1051/0004-6361/202557615 , urldate =

    work page doi:10.1051/0004-6361/202557615 2026

  53. [55]

    Evolution of

    Br. Evolution of. The Astrophysical Journal , volume =. doi:10.3847/1538-4357/ae5b76 , urldate =. arXiv , keywords =:2512.13838 , primaryclass =

    Pith/arXiv arXiv

  54. [58]

    and Aerts, C

    Briquet, M. and Aerts, C. and Baglin, A. and Nieva, M. F. and Degroote, P. and Przybilla, N. and Noels, A. and Schiller, F. and Vu. An Asteroseismic Study of the. Astronomy and Astrophysics , volume =. doi:10.1051/0004-6361/201015690 , urldate =

    doi:10.1051/0004-6361/201015690

  55. [59]

    and Neiner, C

    Briquet, M. and Neiner, C. and Aerts, C. and Morel, T. and Mathis, S. and Reese, D. R. and Lehmann, H. and Costero, R. and Echevarria, J. and Handler, G. and Kambe, E. and Hirata, R. and Masuda, S. and Wright, D. and Yang, S. and Pintado, O. and Mkrtichian, D. and Lee, B. C. and Han, I. and Bruch, A. and De Cat, P. and Uytterhoeven, K. and Lefever, K. and...

    arXiv 2012

  56. [60]

    and Berger, Edo and Stevenson, Simon and Justham, Stephen and Mandel, Ilya and Chru

    Broekgaarden, Floor S. and Berger, Edo and Stevenson, Simon and Justham, Stephen and Mandel, Ilya and Chru. Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations -. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1093/mnras/stac1677 , urldate =

    doi:10.1093/mnras/stac1677

  57. [61]

    and De Mink, S

    Brott, I. and De Mink, S. E. and Cantiello, M. and Langer, N. and De Koter, A. and Evans, C. J. and Hunter, I. and Trundle, C. and Vink, J. S. , year = 2011, month = jun, journal =. Rotating Massive Main-Sequence Stars:. doi:10.1051/0004-6361/201016113 , urldate =

    doi:10.1051/0004-6361/201016113 2011

  58. [62]

    and Evans, C

    Brott, I. and Evans, C. J. and Hunter, I. and De Koter, A. and Langer, N. and Dufton, P. L. and Cantiello, M. and Trundle, C. and Lennon, D. J. and De Mink, S. E. and Yoon, S.-C. and Anders, P. , year = 2011, month = jun, journal =. Rotating Massive Main-Sequence Stars:. doi:10.1051/0004-6361/201016114 , urldate =

    doi:10.1051/0004-6361/201016114 2011

  59. [63]

    Brown, J. C. and Cassinelli, J. P. and Maheswaran, M. , year = 2008, month = dec, journal =. Magnetically. doi:10.1086/592558 , urldate =

    work page doi:10.1086/592558 2008

  60. [64]

    Monthly Notices of the Royal Astronomical Society , volume =

    Stellar Population Synthesis at the Resolution of 2003 , author =. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1046/j.1365-8711.2003.06897.x , urldate =

    arXiv 2003

  61. [65]

    Collaborative

    Buchner, Johannes , year = 2019, month = oct, journal =. Collaborative. doi:10.1088/1538-3873/aae7fc , urldate =. arXiv , keywords =:1707.04476 , primaryclass =

    Pith/arXiv arXiv 2019

  62. [66]

    Buchner, Johannes , year = 2023, month = jan, journal =. Nested. doi:10.1214/23-SS144 , urldate =. arXiv , keywords =:2101.09675 , primaryclass =

    Pith/arXiv arXiv 2023

  63. [67]

    A Statistical Test for

    Buchner, Johannes , year = 2016, month = jan, journal =. A Statistical Test for. doi:10.1007/s11222-014-9512-y , urldate =. arXiv , keywords =:1407.5459 , primaryclass =

    Pith/arXiv arXiv 2016

  64. [68]

    doi:10.48550/arXiv.2101.09604 , urldate =

    Buchner, Johannes , year = 2021, month = apr, number =. doi:10.48550/arXiv.2101.09604 , urldate =. arXiv , keywords =:2101.09604 , primaryclass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2101.09604 2021

  65. [69]

    and Aerts, C

    Buysschaert, B. and Aerts, C. and Bowman, D. M. and Johnston, C. and Van Reeth, T. and Pedersen, M. G. and Mathis, S. and Neiner, C. , year = 2018, month = aug, journal =. Forward Seismic Modeling of the Pulsating Magnetic. doi:10.1051/0004-6361/201832642 , urldate =

    doi:10.1051/0004-6361/201832642 2018

  66. [70]

    and Eldridge, Jan J

    Byrne, Conor M. and Eldridge, Jan J. and Stanway, Elizabeth R. , year = 2025, month = feb, journal =. Bpass Stellar Evolution Models Incorporating. doi:10.1093/mnras/staf178 , urldate =

    doi:10.1093/mnras/staf178 2025

  67. [71]

    The Dependence of Theoretical Synthetic Spectra on

    Byrne, C M and Stanway, E R and Eldridge, J J and McSwiney, L and Townsend, O T , year = 2022, month = jun, journal =. The Dependence of Theoretical Synthetic Spectra on. doi:10.1093/mnras/stac807 , urldate =

    doi:10.1093/mnras/stac807 2022

  68. [72]

    Astronomy and Astrophysics , volume =

    Binary Star Progenitors of Long Gamma-Ray Bursts , author =. Astronomy and Astrophysics , volume =. doi:10.1051/0004-6361:20077115 , urldate =

    doi:10.1051/0004-6361:20077115

  69. [73]

    Carciofi, A. C. and Bjorkman, J. E. , year = 2008, month = sep, journal =. Non-. doi:10.1086/589875 , urldate =

    doi:10.1086/589875 2008

  70. [74]

    Cassinelli, J. P. and Cohen, D. H. and Macfarlane, J. J. and Drew, J. E. and. The Astrophysical Journal , volume =. doi:10.1086/175135 , urldate =

    work page doi:10.1086/175135

  71. [75]

    Cassinelli, J. P. and Cohen, D. H. and Macfarlane, J. J. and Drew, J. E. and. The Astrophysical Journal , volume =. doi:10.1086/177023 , urldate =

    work page doi:10.1086/177023

  72. [76]

    Cassinelli, J. P. and Brown, J. C. and Maheswaran, M. and Miller, N. A. and Telfer, D. C. , year = 2002, month = oct, journal =. A. doi:10.1086/342654 , urldate =

    work page doi:10.1086/342654 2002

  73. [77]

    and Potekhin, A

    Cassisi, S. and Potekhin, A. Y. and Pietrinferni, A. and Catelan, M. and Salaris, M. , year = 2007, month = jun, journal =. Updated. doi:10.1086/516819 , keywords =

    doi:10.1086/516819 2007

  74. [78]

    and Najarro, F

    Castellanos, R. and Najarro, F. and Garcia, M. and Negueruela, I. and Patrick, L. R. and Ritchie, B. and Guarcello, M. G. and Shenar, T. and Evans, C. and Prinja, R. and Fenech, D. , year = 2026, month = feb, number =. First Spectroscopic Identification of the Main Sequence in. doi:10.48550/arXiv.2602.24218 , urldate =. arXiv , keywords =:2602.24218 , pri...

    work page doi:10.48550/arxiv.2602.24218 2026

  75. [79]

    and Fossati, L

    Castro, N. and Fossati, L. and Langer, N. and. The Spectroscopic. Astronomy & Astrophysics , volume =. doi:10.1051/0004-6361/201425028 , urldate =

    doi:10.1051/0004-6361/201425028

  76. [80]

    and Oey, M

    Castro, N. and Oey, M. S. and Fossati, L. and Langer, N. , year = 2018, month = nov, journal =. The. doi:10.3847/1538-4357/aae6d0 , urldate =

    doi:10.3847/1538-4357/aae6d0 2018

  77. [81]

    and Williams, Benjamin F

    Choi, Yumi and Gilbert, Karoline M. and Williams, Benjamin F. and Weisz, Daniel R. and Skillman, Evan D. and Dalcanton, Julianne J. and McQuinn, Kristen B. W. and Dolphin, Andrew E. and Pastorelli, Giada and Boyer, Martha L. and Gordon, Karl D. and Girardi, L. The. The Astronomical Journal , volume =. doi:10.3847/1538-3881/adc384 , urldate =

    work page doi:10.3847/1538-3881/adc384

  78. [82]

    , year = 2016, month = jun, journal =

    Choi, Jieun and Dotter, Aaron and Conroy, Charlie and Cantiello, Matteo and Paxton, Bill and Johnson, Benjamin D. , year = 2016, month = jun, journal =. Mesa. doi:10.3847/0004-637X/823/2/102 , urldate =

    doi:10.3847/0004-637x/823/2/102 2016

  79. [83]

    Drew and

    Chojnowski, S. Drew and. The. The Astrophysical Journal , volume =. doi:10.3847/1538-4357/aad964 , urldate =. arXiv , keywords =:1806.06843 , primaryclass =

    Pith/arXiv arXiv

  80. [84]

    Chemical

    Chru. Chemical. Annalen der Physik , volume =. doi:10.1002/andp.202200170 , urldate =

    doi:10.1002/andp.202200170

Showing first 80 references.