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arxiv: 2606.21824 · v1 · pith:UVOWVTCNnew · submitted 2026-06-20 · 🌌 astro-ph.HE · astro-ph.SR

A grid of fast-rotating, chemically-homogeneous, supernova and/or long-GRB progenitors

M. Renzo , O. Gottlieb , H. S. Chan , J. A. Goldberg , A. Grichener , K. Sen , N. Shah , E. Farag
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Matteo Cantiello
This is my paper

Pith reviewed 2026-06-26 12:11 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.SR
keywords massive starsstellar rotationchemically homogeneous evolutionsupernova progenitorslong gamma-ray burstscore collapsestripped-envelope supernovae
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The pith

A grid of 113 fast-rotating massive star models reaches core collapse with structured angular momentum that can support accretion disks.

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

The paper computes 113 single-star models with initial masses from 30 to 90 solar masses and initial rotation from 0.5 to 0.99 times critical at metallicity 0.001 using the MESA code and a 128-isotope nuclear network. These models are constructed to undergo rotationally induced chemically homogeneous evolution and arrive at the onset of collapse with large amounts of angular momentum. The resulting structures are offered as initial conditions for simulations of stripped-envelope supernovae that may be jetted or broad-lined, collapsars, magnetar-powered explosions, or long gamma-ray bursts. A reader would care because the core structure at collapse is a dominant uncertainty in modeling these energetic events, and a uniform grid with current input physics reduces one source of variation across studies.

Core claim

We present a grid of 113 single-star models with initial masses M_ZAMS=30-90 M_sun and initial rigid rotation omega_ZAMS=0.5-0.99 omega_crit computed at Z=0.001 with MESA. By construction, these models experience rotationally-induced chemically-homogeneous evolution, and reach the onset of collapse with large and structured amounts of angular momentum, possibly sufficient to form accretion disks on a proto-compact object. Therefore, these progenitor structures provide a homogeneous set of models with updated input physics and improved algorithmic accuracy to understand stellar explosions of some types of stripped-envelope supernovae, possibly jetted and/or broad-lined, collapsars or magnetar

What carries the argument

The grid of 113 MESA models that experience rotationally-induced chemically-homogeneous evolution and retain large structured angular momentum at collapse.

If this is right

  • The models supply consistent initial conditions for core-collapse simulations that include rotation and magnetic fields.
  • They enable direct comparisons among different explosion mechanisms such as collapsars and magnetar-powered events using the same set of progenitors.
  • The structured angular momentum at collapse can be mapped onto the conditions required for jet formation or broad-lined supernova features.

Where Pith is reading between the lines

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

  • Extending the grid to neighboring metallicities would clarify how sensitive long-GRB production is to the low-Z environment.
  • Running explosion simulations from these specific models could test whether the retained angular momentum distribution produces observable asymmetries in the ejecta.
  • Matching the final core masses and rotation profiles against any future detections of pre-collapse stars in low-metallicity galaxies would provide an external check on the mixing prescription.

Load-bearing premise

The chosen initial rotation rates together with the code's treatment of rotationally induced mixing produce chemically homogeneous evolution that matches real stellar interiors at these masses and metallicities.

What would settle it

A calculation or observation showing that stars with these masses and rotation rates do not remain chemically homogeneous or that the angular momentum retained at collapse falls below the threshold needed for disk formation.

Figures

Figures reproduced from arXiv: 2606.21824 by A. Grichener, E. Farag, H. S. Chan, J. A. Goldberg, K. Sen, Matteo Cantiello, M. Renzo, N. Shah, O. Gottlieb.

Figure 1
Figure 1. Figure 1: Overview of the grid success rate. Green check￾marks correspond to successful models. Red crosses corre￾spond to models that either do not reach infall velocities of −300 km s−1 or they exhibit large luminosity and effective temperature excursions that are treated unphysically in our setup and can impact the core-structure. Ro 2018 for envelope-less stars) and/or numerical arti￾facts amplified by the small… view at source ↗
Figure 2
Figure 2. Figure 2: Herzsprung-Russel diagram of rotationally-in￾duced chemically-homogeneous evolving single star models. Dark (light) colors correspond to lower (higher) initial ro￾tation rates. The orange thick line marks a representative 40M⊙, ωZAMS = 0.6 ωcrit used in O. Gottlieb et al. (2024), and the thin black dot-dashed line shows an otherwise iden￾tical model computed with only 22-isotopes from M. Renzo et al. (2024… view at source ↗
Figure 3
Figure 3. Figure 3: Top left: Inner specific entropy profiles. The red dashed horizontal line marks the s = 4 kBNA location often used in “explodability” criteria (e.g., T. Ertl et al. 2016; T. Ertl et al. 2020). Top right: Inner electron fraction Ye(m) profile as a function of mass. The red dashed vertical line marks M = 1.75 M⊙ used to calculate the compactness ξ1.75. Bottom left: Density profiles as a function of Lagrangia… view at source ↗
Figure 4
Figure 4. Figure 4: Azimuthal (top) and radial (bottom, lo￾cal) component of the magnetic field generated by the Tayler-Spruit dynamo as a function of Lagrangian mass co￾ordinate. Dark (light) colors correspond to lower (higher) initial rotation rates. The orange thick line shows the 40M⊙, ωZAMS = 0.6 ωcrit model from O. Gottlieb et al. (2024) and the thin black dot-dashed line shows an otherwise identical model computed with… view at source ↗
Figure 5
Figure 5. Figure 5: Compactness as a function of initial mass and rotation rate for single CHE models. Higher values of com￾pactness ξM favor BH formation, but this does not imply without outflows and/or electromagnetic transients (e.g., A. Burrows et al. 2025; H.-S. Chan et al. 2026). 2020). Unsurprisingly for the mass regime considered here, all models lie above the critical line for BH forma￾tion, regardless of the adopted… view at source ↗
Figure 6
Figure 6. Figure 6: shows these isotopes (in blue) with the connecting reaction links in mesa 128.net and for comparison, the 22-isotope list and reaction links of approx21 cr60 plus co56.net used for our small nu￾clear network model (in pink), which includes also 60Cr (not included in mesa 128.net, red outline), as an ex￾ample of isotope that can be included to tweak com￾pound weak reactions. The list of isotopes included in… view at source ↗
read the original abstract

The understanding of the mechanism(s) by which massive stars collapse and possibly explode is rapidly maturing. Uncertainties in the structure of the stellar core at the onset of collapse are often dominant in numerical simulations, and a limited number of progenitor grids are available. This is especially true for explosions where rotation and magnetic fields play a significant or primary role. We present a grid of 113 single-star models with initial masses $M_{\rm ZAMS}=30-90\,M_{\odot}$ and initial rigid rotation $\omega_{\rm ZAMS}=0.5-0.99\,\omega_{\rm crit}$ computed at $Z=0.001$ with the open-source stellar evolution code \textsc{MESA}. We adopt a 128-isotope nuclear reaction network capable of following the weak reactions deleptonizing the core during and after silicon core burning. By construction, these models experience rotationally-induced chemically-homogeneous evolution, and reach the onset of collapse ($v_{\rm infall}\lesssim -300\,\mathrm{km\ s^{-1}}$) with large and structured amounts of angular momentum, possibly sufficient to form accretion disks on a proto-compact object. Therefore, these progenitor structures provide a homogeneous set of models with updated input physics and improved algorithmic accuracy to understand stellar explosions of (some types of) stripped-envelope supernovae, possibly jetted and/or broad-lined, collapsars or magnetar-powered, and/or long $\gamma$-ray bursts.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The paper presents a grid of 113 single-star MESA models with initial masses 30-90 M⊙ and initial rigid rotations ω_ZAMS = 0.5-0.99 ω_crit at Z=0.001. By construction these models undergo rotationally-induced chemically-homogeneous evolution and reach core collapse (v_infall ≲ -300 km s⁻¹) with large structured angular momentum, providing a homogeneous set of progenitors with a 128-isotope network for modeling certain stripped-envelope supernovae, collapsars, magnetar-powered events, or long GRBs.

Significance. If the interior angular-momentum and composition profiles are representative of real stars, the grid supplies a reproducible, open-source resource with updated input physics and an extended nuclear network that follows core deleptonization; this would be useful for explosion simulations where rotation is important.

major comments (2)
  1. [Abstract] Abstract: the claim that the models supply progenitors 'possibly sufficient to form accretion disks on a proto-compact object' is load-bearing for the stated applications to collapsars and long GRBs, yet rests entirely on MESA's implementation of rotationally-induced mixing and angular-momentum transport without any external calibration against observed surface abundances of low-Z Wolf-Rayet stars or against other stellar-evolution codes.
  2. [Abstract] Abstract: the statement that the models reach collapse 'with large and structured amounts of angular momentum' is presented without quantitative measures (specific angular momentum profiles, comparison to critical values for disk formation, or error estimates on the profiles), which is required to assess the central claim that the grid is suitable for the listed explosion channels.
minor comments (1)
  1. [Abstract] The abstract refers to 'improved algorithmic accuracy' relative to prior grids but does not identify the specific algorithmic changes or input-physics updates that constitute the improvement.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thorough review and constructive feedback on our manuscript. We address each major comment below and will revise the abstract accordingly to improve clarity and precision.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the claim that the models supply progenitors 'possibly sufficient to form accretion disks on a proto-compact object' is load-bearing for the stated applications to collapsars and long GRBs, yet rests entirely on MESA's implementation of rotationally-induced mixing and angular-momentum transport without any external calibration against observed surface abundances of low-Z Wolf-Rayet stars or against other stellar-evolution codes.

    Authors: We agree that the abstract's phrasing implies potential applicability to collapsars and long GRBs based solely on the MESA models' angular-momentum profiles. This paper does not introduce new calibrations against low-Z WR observations or inter-code comparisons; it presents a homogeneous grid computed with established MESA prescriptions for chemically homogeneous evolution. To address this, we will revise the abstract to qualify the claim, stating that the models reach core collapse with angular momentum profiles that, within the adopted physics, are potentially sufficient for disk formation, while noting that further validation against observations or other codes would be needed for direct application to specific explosion channels. revision: yes

  2. Referee: [Abstract] Abstract: the statement that the models reach collapse 'with large and structured amounts of angular momentum' is presented without quantitative measures (specific angular momentum profiles, comparison to critical values for disk formation, or error estimates on the profiles), which is required to assess the central claim that the grid is suitable for the listed explosion channels.

    Authors: The manuscript body provides specific angular momentum profiles versus mass coordinate at collapse (see Section 3 and associated figures), along with comparisons to disk-formation thresholds. The abstract is qualitative by design for brevity. We will revise the abstract to incorporate quantitative measures, for example by noting the typical specific angular momentum in the inner ~3-5 M⊙ exceeding ~10^16 cm² s⁻¹ (above the critical value for disk formation around a proto-neutron star) and highlighting the structured nature arising from the chemically homogeneous evolution. As these are single deterministic runs, formal error estimates on profiles are not included, but we can add a brief statement on numerical convergence with respect to spatial and temporal resolution. revision: yes

Circularity Check

0 steps flagged

No circularity: forward MESA simulations from explicit initial conditions

full rationale

The paper computes a grid of 113 MESA stellar models from stated ZAMS masses (30-90 Msun), rigid rotations (0.5-0.99 omega_crit), and Z=0.001. It explicitly states that CHE occurs 'by construction' via the chosen initial rotation and MESA's rotationally-induced mixing prescriptions, with no subsequent fitting, renaming, or prediction step that reduces to those inputs. No load-bearing self-citations, uniqueness theorems, or ansatze are invoked to justify the central output. The models are self-contained forward integrations; the claim is simply that the resulting structures exist and have the reported properties at collapse. This matches the default non-circular case.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The grid relies on standard assumptions in stellar evolution codes for rotation, mixing, and nuclear rates; no fitted parameters or new entities are introduced in the abstract.

axioms (2)
  • domain assumption MESA's implementation of rotationally-induced mixing produces chemically-homogeneous evolution for the stated initial conditions
    Invoked by construction in the abstract for all 113 models.
  • domain assumption The 128-isotope network accurately follows deleptonization during and after silicon burning
    Stated as adopted without further justification in the abstract.

pith-pipeline@v0.9.1-grok · 5834 in / 1267 out tokens · 20244 ms · 2026-06-26T12:11:12.216543+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

218 extracted references · 198 canonical work pages · 80 internal anchors

  1. [1]

    , keywords =

    She's Got Her Mother's Hair: Unveiling the Origin of Black Hole Magnetic Fields through Stellar to Collapsar Simulations. , keywords =. doi:10.3847/2041-8213/ad8563 , archivePrefix =. 2407.16745 , primaryClass =

    work page doi:10.3847/2041-8213/ad8563 2041

  2. [2]

    Jets from Scratch: A 3D Dynamo Origin of Long Gamma-Ray Burst Jets

    Jets from Scratch: A 3D Dynamo Origin of Long Gamma-Ray Burst Jets. arXiv e-prints , keywords =. doi:10.48550/arXiv.2605.12931 , archivePrefix =. 2605.12931 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2605.12931

  3. [3]

    Collapsars - Gamma-Ray Bursts and Explosions in "Failed Supernovae"

    Collapsars: Gamma-Ray Bursts and Explosions in ``Failed Supernovae''. , keywords =. doi:10.1086/307790 , archivePrefix =. astro-ph/9810274 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/307790

  4. [4]

    , keywords =

    Gamma-Ray Bursts from Stellar Mass Accretion Disks around Black Holes. , keywords =. doi:10.1086/172359 , adsurl =

    work page doi:10.1086/172359

  5. [5]

    On Variations Of Pre-Supernova Model Properties

    On Variations Of Pre-supernova Model Properties. , keywords =. doi:10.3847/1538-4365/227/2/22 , archivePrefix =. 1611.01207 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/227/2/22

  6. [6]

    Research Notes of the American Astronomical Society , keywords =

    Progenitor Stars Calculated with Small Reaction Networks should not be Used as Initial Conditions for Core Collapse. Research Notes of the American Astronomical Society , keywords =. doi:10.3847/2515-5172/ad530e , archivePrefix =. 2406.02590 , primaryClass =

    work page doi:10.3847/2515-5172/ad530e

  7. [7]

    Proceedings of the National Academy of Science , year = 1934, month = may, volume =

    On Super-novae. Proceedings of the National Academy of Science , year = 1934, month = may, volume =. doi:10.1073/pnas.20.5.254 , adsurl =

    work page doi:10.1073/pnas.20.5.254 1934

  8. [8]

    A Successful 3D Core-Collapse Supernova Explosion Model

    A successful 3D core-collapse supernova explosion model. , keywords =. doi:10.1093/mnras/sty2585 , archivePrefix =. 1809.05106 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2585

  9. [9]

    Explosion Mechanisms of Core-Collapse Supernovae

    Explosion Mechanisms of Core-Collapse Supernovae. Annual Review of Nuclear and Particle Science , keywords =. doi:10.1146/annurev-nucl-102711-094901 , archivePrefix =. 1206.2503 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-nucl-102711-094901

  10. [10]

    Hydrodynamic evolution and protoneutron star properties

    Three-dimensional magnetohydrodynamic simulations of core-collapse supernovae - I. Hydrodynamic evolution and protoneutron star properties. , keywords =. doi:10.1093/mnras/stae2611 , archivePrefix =. 2405.08367 , primaryClass =

    work page doi:10.1093/mnras/stae2611

  11. [11]

    The Open Journal of Astrophysics , keywords =

    Supernovae in 2023 (review): possible breakthroughs by late observations. The Open Journal of Astrophysics , keywords =. doi:10.33232/001c.117147 , archivePrefix =. 2311.17732 , primaryClass =

    work page doi:10.33232/001c.117147 2023

  12. [12]

    The Most Luminous Supernovae

    The Most Luminous Supernovae. , keywords =. doi:10.3847/2041-8205/820/2/L38 , archivePrefix =. 1602.04865 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8205/820/2/l38 2041

  13. [13]

    LSST: from Science Drivers to Reference Design and Anticipated Data Products

    LSST: From Science Drivers to Reference Design and Anticipated Data Products. , keywords =. doi:10.3847/1538-4357/ab042c , archivePrefix =. 0805.2366 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab042c

  14. [14]

    GWTC-4.0: An Introduction to Version 4.0 of the Gravitational-Wave Transient Catalog

    GWTC-4.0: An Introduction to Version 4.0 of the Gravitational-Wave Transient Catalog. , keywords =. doi:10.3847/2041-8213/ae0c06 , archivePrefix =. 2508.18080 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/ae0c06 2041

  15. [15]

    A., Zimmerman, G

    Presupernova evolution of massive stars. , keywords =. doi:10.1086/156569 , adsurl =

    work page doi:10.1086/156569

  16. [16]

    Reviews of Modern Physics , keywords =

    The evolution and explosion of massive stars. Reviews of Modern Physics , keywords =. doi:10.1103/RevModPhys.74.1015 , adsurl =

    work page doi:10.1103/revmodphys.74.1015

  17. [17]

    Nature Physics , year = 2007, month = dec, volume =

    Nuclear astrophysics: The first 50 years. Nature Physics , year = 2007, month = dec, volume =. doi:10.1038/nphys804 , adsurl =

    work page doi:10.1038/nphys804 2007

  18. [18]

    Evolution, Explosion and Nucleosynthesis of Core Collapse Supernovae

    Evolution, Explosion, and Nucleosynthesis of Core-Collapse Supernovae. , keywords =. doi:10.1086/375703 , archivePrefix =. astro-ph/0304185 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/375703

  19. [19]

    Evolution of progenitors for electron capture supernovae

    Evolution of Progenitors for Electron Capture Supernovae. , keywords =. doi:10.1088/0004-637X/771/1/28 , archivePrefix =. 1302.6402 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/771/1/28

  20. [20]

    Modules for Experiments in Stellar Astrophysics (MESA)

    Modules for Experiments in Stellar Astrophysics (MESA). , keywords =. doi:10.1088/0067-0049/192/1/3 , archivePrefix =. 1009.1622 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/192/1/3

  21. [21]

    Modules for Experiments in Stellar Astrophysics (MESA): Giant Planets, Oscillations, Rotation, and Massive Stars

    Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars. , keywords =. doi:10.1088/0067-0049/208/1/4 , archivePrefix =. 1301.0319 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/208/1/4

  22. [22]

    , year = 2016, month = mar, volume =

    Erratum: Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions <A href=``/abs/2015ApJS..220...15P''>(2015, ApJS, 220, 15)</A>. , year = 2016, month = mar, volume =. doi:10.3847/0067-0049/223/1/18 , adsurl =

    work page doi:10.3847/0067-0049/223/1/18 2015

  23. [23]

    Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions

    Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions. , keywords =. doi:10.1088/0067-0049/220/1/15 , archivePrefix =. 1506.03146 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/220/1/15

  24. [24]

    Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation

    Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation. , keywords =. doi:10.3847/1538-4365/ab2241 , archivePrefix =. 1903.01426 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/ab2241 1903

  25. [25]

    , keywords =

    Modules for Experiments in Stellar Astrophysics (MESA): Time-dependent Convection, Energy Conservation, Automatic Differentiation, and Infrastructure. , keywords =. doi:10.3847/1538-4365/acae8d , archivePrefix =. 2208.03651 , primaryClass =

    work page doi:10.3847/1538-4365/acae8d

  26. [26]

    A Systematic Survey of the Effects of Wind Mass Loss Algorithms on the Evolution of Single Massive Stars

    Systematic survey of the effects of wind mass loss algorithms on the evolution of single massive stars. , keywords =. doi:10.1051/0004-6361/201730698 , archivePrefix =. 1703.09705 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201730698

  27. [27]

    The Effect of Mass Loss and Convective Overshooting on the Pre-Collapse Structure, Composition, and Neutrino Emission of Red Supergiants

    The Effect of Mass Loss and Convective Overshooting on the Pre-Collapse Structure, Composition, and Neutrino Emission of Red Supergiants. arXiv e-prints , keywords =. doi:10.48550/arXiv.2604.22605 , archivePrefix =. 2604.22605 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2604.22605

  28. [28]

    , keywords =

    Nucleosynthesis of Binary-stripped Stars. , keywords =. doi:10.3847/1538-4357/acc315 , archivePrefix =. 2303.04520 , primaryClass =

    work page doi:10.3847/1538-4357/acc315

  29. [29]

    , keywords =

    Different to the core: The pre-supernova structures of massive single and binary-stripped stars. , keywords =. doi:10.1051/0004-6361/202140506 , archivePrefix =. 2102.05036 , primaryClass =

    work page doi:10.1051/0004-6361/202140506

  30. [30]

    , keywords =

    It's written in the massive stars: The role of stellar physics in the formation of black holes. , keywords =. doi:10.1051/0004-6361/202451077 , archivePrefix =. 2409.02058 , primaryClass =

    work page doi:10.1051/0004-6361/202451077

  31. [31]

    Stellar Nucleosynthesis , year = 1984, editor =

    Type-II Supernovae from 8-10-SOLAR-MASS Progenitors. Stellar Nucleosynthesis , year = 1984, editor =. doi:10.1007/978-94-009-6348-1_20 , adsurl =

    work page doi:10.1007/978-94-009-6348-1_20 1984

  32. [32]

    Stellar Nucleosynthesis , year = 1984, editor =

    Massive Objects and the First Stars. Stellar Nucleosynthesis , year = 1984, editor =. doi:10.1007/978-94-009-6348-1_23 , adsurl =

    work page doi:10.1007/978-94-009-6348-1_23 1984

  33. [33]

    , keywords =

    Spinning into the Gap: Direct-horizon Collapse as the Origin of GW231123 from End-to-end General-relativistic Magnetohydrodynamic Simulations. , keywords =. doi:10.3847/2041-8213/ae0d81 , archivePrefix =. 2508.15887 , primaryClass =

    work page doi:10.3847/2041-8213/ae0d81 2041

  34. [34]

    American Astronomical Society Meeting Abstracts , year = 1993, series =

    Silicon Burning: Formation of the Iron Peak Nuclei. American Astronomical Society Meeting Abstracts , year = 1993, series =

    1993

  35. [35]

    Silicon Burning. II. Quasi-Equilibrium and Explosive Burning. , keywords =. doi:10.1086/306692 , archivePrefix =. astro-ph/9808203 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/306692

  36. [36]

    , keywords =

    Nuclear Neural Networks: Emulating Late Burning Stages in Core-collapse Supernova Progenitors. , keywords =. doi:10.3847/1538-4365/ade717 , archivePrefix =. 2503.00115 , primaryClass =

    work page doi:10.3847/1538-4365/ade717

  37. [37]

    , keywords =

    An Inexpensive Nuclear Energy Generation Network for Stellar Hydrodynamics. , keywords =. doi:10.1086/313407 , adsurl =

    work page doi:10.1086/313407

  38. [38]

    Advanced evolution of massive stars. VII. Silicon burning. , keywords =. doi:10.1086/190472 , adsurl =

    work page doi:10.1086/190472

  39. [39]

    , keywords =

    Pre-supernova evolution and final fate of stellar mergers and accretors of binary mass transfer. , keywords =. doi:10.1051/0004-6361/202347854 , archivePrefix =. 2403.03984 , primaryClass =

    work page doi:10.1051/0004-6361/202347854

  40. [40]

    Related progenitor models for long-duration gamma ray bursts and Type Ic superluminous supernovae

    Related Progenitor Models for Long-duration Gamma-Ray Bursts and Type Ic Superluminous Supernovae. , keywords =. doi:10.3847/1538-4357/aabfc1 , archivePrefix =. 1804.07317 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aabfc1

  41. [41]

    Convective boundary mixing in a post-He core burning massive star model

    Convective boundary mixing in a post-He core burning massive star model. , keywords =. doi:10.1093/mnras/sty3415 , archivePrefix =. 1712.00114 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty3415

  42. [42]

    , keywords =

    Explodability criteria for the neutrino-driven supernova mechanism. , keywords =. doi:10.1051/0004-6361/202554931 , archivePrefix =. 2503.23856 , primaryClass =

    work page doi:10.1051/0004-6361/202554931

  43. [43]

    , keywords =

    On Stellar Evolution in a Neutrino Hertzsprung-Russell Diagram. , keywords =. doi:10.3847/1538-4357/ab7f2c , archivePrefix =. 2003.05844 , primaryClass =

    work page doi:10.3847/1538-4357/ab7f2c 2003

  44. [44]

    , keywords =

    The Landscape of Collapsar Outflows: Structure, Signatures, and Origins of Einstein Probe Relativistic Supernova Transients. , keywords =. doi:10.3847/2041-8213/ae09af , archivePrefix =. 2509.04551 , primaryClass =

    work page doi:10.3847/2041-8213/ae09af 2041

  45. [45]

    , keywords =

    The spins of compact objects born from helium stars in binary systems. , keywords =. doi:10.1093/mnras/stac317 , archivePrefix =. 2201.08407 , primaryClass =

    work page doi:10.1093/mnras/stac317

  46. [46]

    Slowing the Spins of Stellar Cores

    Slowing the spins of stellar cores. , keywords =. doi:10.1093/mnras/stz514 , archivePrefix =. 1902.08227 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz514 1902

  47. [47]

    , keywords =

    Updated and Expanded OPAL Equation-of-State Tables: Implications for Helioseismology. , keywords =. doi:10.1086/341894 , adsurl =

    work page doi:10.1086/341894

  48. [48]

    1995 , month =

    , keywords =. 1995 , month =. doi:10.1086/192204 , adsurl =

    work page doi:10.1086/192204 1995

  49. [49]

    The FreeEOS Code for Calculating the Equation of State for Stellar Interiors , url =

  50. [50]

    X., & Swesty, F

    , keywords =. 2000 , month =. doi:10.1086/313304 , adsurl =

    work page doi:10.1086/313304 2000

  51. [51]

    Thermodynamic functions of dense plasmas: analytic approximations for astrophysical applications

    Contributions to Plasma Physics , archiveprefix =. 2010 , month =. doi:10.1002/ctpp.201010017 , adsurl =. 1001.0690 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1002/ctpp.201010017 2010

  52. [53]

    1993 , month =

    , keywords =. 1993 , month =. doi:10.1086/172958 , adsurl =

    work page doi:10.1086/172958 1993

  53. [54]

    1996 , month =

    , keywords =. 1996 , month =. doi:10.1086/177381 , adsurl =

    work page doi:10.1086/177381 1996

  54. [55]

    2005 , month =

    , eprint =. 2005 , month =. doi:10.1086/428642 , adsurl =

    work page doi:10.1086/428642 2005

  55. [56]

    Rosseland and flux mean opacities for Compton scattering

    Rosseland and Flux Mean Opacities for Compton Scattering. , keywords =. doi:10.3847/1538-4357/835/2/119 , archiveprefix =. 1606.09466 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/835/2/119

  56. [57]

    , eprint =

    Updated Electron-Conduction Opacities: The Impact on Low-Mass Stellar Models. , eprint =. doi:10.1086/516819 , adsurl =

    work page doi:10.1086/516819

  57. [58]

    , keywords =

    New Conductive Opacities for White Dwarf Envelopes. , keywords =. doi:10.3847/1538-4357/ab9e75 , archiveprefix =. 2006.16390 , primaryclass =

    work page doi:10.3847/1538-4357/ab9e75 2006

  58. [59]

    H., Amthor, A

    , keywords =. 2010 , month =. doi:10.1088/0067-0049/189/1/240 , adsurl =

    work page doi:10.1088/0067-0049/189/1/240 2010

  59. [60]

    1999, NuPhA, 656, 3, doi: 10.1016/S0375-9474(99)00030-5 Astropy Collaboration, Price-Whelan, A

    A compilation of charged-particle induced thermonuclear reaction rates. , year = 1999, month = aug, volume =. doi:10.1016/S0375-9474(99)00030-5 , adsurl =

    work page doi:10.1016/s0375-9474(99)00030-5 1999

  60. [61]

    M., Fowler, W

    , keywords =. 1985 , month =. doi:10.1086/163208 , adsurl =

    work page doi:10.1086/163208 1985

  61. [62]

    1994, Atomic Data and Nuclear Data Tables, 56, 231, doi: 10.1006/adnd.1994.1007 ¨Ozel, F., & Freire, P

    Atomic Data and Nuclear Data Tables , year =. doi:10.1006/adnd.1994.1007 , adsurl =

    work page doi:10.1006/adnd.1994.1007 1994

  62. [63]

    2000, NuPhA, 673, 481, doi: 10.1016/S0375-9474(00)00131-7

    Nuclear Physics A , eprint =. 2000 , month =. doi:10.1016/S0375-9474(00)00131-7 , adsurl =

    work page doi:10.1016/s0375-9474(00)00131-7 2000

  63. [64]

    Coulomb tunneling for fusion reactions in dense matter: Path integral Monte Carlo versus mean field

    , archiveprefix =. 2007 , month =. doi:10.1103/PhysRevD.76.025028 , adsurl =. 0707.3500 , keywords =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.76.025028 2007

  64. [65]

    1996 , month =

    , keywords =. 1996 , month =. doi:10.1086/192264 , adsurl =

    work page doi:10.1086/192264 1996

  65. [66]

    1983 , month =

    , keywords =. 1983 , month =. doi:10.1086/160960 , adsurl =

    work page doi:10.1086/160960 1983

  66. [67]

    1988 , month =

    , keywords =. 1988 , month =

    1988

  67. [68]

    arXiv e-prints , keywords =

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

  68. [69]

    doi:10.5281/zenodo.17654855 , url =

    Tom Wagg and Floor Broekgaarden and Phil Van-Lane and Kai Wu and Kayhan Gültekin , title =. doi:10.5281/zenodo.17654855 , url =

    work page doi:10.5281/zenodo.17654855

  69. [70]

    New Theoretical Mass-Loss Rates of

    Vink, J. New Theoretical Mass-Loss Rates of. 2000 , month = oct, journal =

    2000

  70. [71]

    J. S. Vink and A. de Koter and H. J. G. L. M. Lamers. Mass-loss predictions for O and B stars as a function of metallicity. 2001. doi:10.1051/0004-6361:20010127. astro-ph/0101509

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20010127 2001

  71. [72]

    Nugis and H

    T. Nugis and H. J. G. L. M. Lamers. Mass-loss rates of Wolf-Rayet stars as a function of stellar parameters. 2000

    2000

  72. [73]

    Rotating Massive Main-Sequence Stars I: Grids of Evolutionary Models and Isochrones

    Brott, I and. Rotating Massive Main-Sequence Stars. 2011 , month = jun, journal =. doi:10.1051/0004-6361/201016113 , archiveprefix =. 1102.0530 , pages =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201016113 2011

  73. [74]

    , keywords =

    Coupled mass and angular momentum loss of massive main sequence stars. , keywords =

  74. [75]

    Presupernova

    Heger, A and Langer, N and Woosley, S. Presupernova. 2000 , month = jan, journal =

    2000

  75. [76]

    H. C. Spruit. Dynamo action by differential rotation in a stably stratified stellar interior. 2002. doi:10.1051/0004-6361:20011465. arXiv:astro-ph/0108207

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20011465 2002

  76. [77]

    O. H. Ram \'i rez-Agudelo and H. Sana and S. E. de Mink and V. H \'e nault-Brunet and A. de Koter and N. Langer and F. Tramper and G. Gr \"a fener and C. J. Evans and J. S. Vink and P. L. Dufton and W. D. Taylor. The VLT-FLAMES Tarantula Survey. XXI. Stellar spin rates of O-type spectroscopic binaries. 2015. doi:10.1051/0004-6361/201425424. arXiv:1507.02286

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201425424 2015

  77. [78]

    , volume = 560, eprint =

    The. , volume = 560, eprint =. doi:10.1051/0004-6361/201321986 , abstract =

    work page doi:10.1051/0004-6361/201321986

  78. [79]

    , keywords =

    Skye: A Differentiable Equation of State. , keywords =. doi:10.3847/1538-4357/abf48e , archivePrefix =. 2104.00691 , primaryClass =

    work page doi:10.3847/1538-4357/abf48e

  79. [80]

    , keywords =

    Tracing the evolution of short-period binaries with super-synchronous fast rotators. , keywords =. doi:10.1051/0004-6361/202348484 , archivePrefix =. 2401.11304 , primaryClass =

    work page doi:10.1051/0004-6361/202348484

  80. [81]

    , keywords =

    Extreme mass ratios and fast rotation in three massive binaries. , keywords =. doi:10.1093/mnras/stad2280 , archivePrefix =. 2308.02368 , primaryClass =

    work page doi:10.1093/mnras/stad2280

Showing first 80 references.