pith. sign in

arxiv: 2605.21062 · v1 · pith:ZFYM2VUOnew · submitted 2026-05-20 · 🌌 astro-ph.SR · astro-ph.HE

Neutron star-companion interaction in core collapse supernovae. Population synthesis based on detailed binary evolution models

Andrea Ercolino , Norbert Langer , Avishay Gal-Yam , Abel Schootemeijer , Caroline Mannes , Harim Jin , Ruggero Valli , Selma de Mink
show 1 more author
Luc Dessart
This is my paper

Pith reviewed 2026-05-21 02:09 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.HE
keywords core collapse supernovaebinary stellar evolutionneutron star companionspopulation synthesisperiodic light curveshydrogen-poor supernovaeSN2022jlicompanion inflation
0
0 comments X

The pith

Periodic companion-neutron star interactions occur in more than half of surviving binary systems that produce hydrogen-poor core-collapse supernovae.

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

When the first star in a massive binary explodes, its ejecta strike the companion, which can expand and then orbitally interact with the new neutron star, producing periodic emission. The authors run population synthesis on a large grid of detailed binary evolution calculations to forecast how often this companion-compact object interaction happens and what its observable signatures are. They conclude the periodic version is common in hydrogen-poor supernova progenitors that remain bound but rare in hydrogen-rich ones. This framework reproduces the periods seen in events like SN2022jli and predicts that the inflated companions remain bright enough for years to be detected by current telescopes. If the rates hold, many more such periodic features should appear in both new and archival supernova data.

Core claim

Analyzing a comprehensive grid of detailed binary stellar evolution models with the SN-ORACLE population synthesis code and analytic prescriptions for companion expansion after supernova ejecta impact, the authors find that periodic CCI occurs in more than half of the binary systems that produce a hydrogen-poor core collapse SN and are not disrupted, while the occurrence rate in systems producing hydrogen-rich SNe is small. The resulting period distribution is broad and peaks around 20-50 days, with interactions lasting 0.5-10 years. Specific models in the grid reproduce the observed periods of SN2022jli, SN2015ap, and SN2022esa, and the inflated companions reach J-band magnitudes of 21-23,,

What carries the argument

Population synthesis of a grid of detailed binary evolution models, combined with analytic prescriptions for the expansion of the companion star after supernova ejecta interaction and its subsequent orbital dynamics with the compact object.

If this is right

  • The interactions produce broad period ranges peaking at 20-50 days and lasting 0.5-10 years.
  • Up to 27 percent of hydrogen-poor supernovae could display periodicity in their light curves.
  • The expanded companions increase in luminosity and reach J-band magnitudes of 21-23 for up to 10 years after events like SN2022jli.
  • The effect is far more common for hydrogen-poor than for hydrogen-rich core-collapse supernovae.

Where Pith is reading between the lines

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

  • A systematic search for periodic modulations in existing and future hydrogen-poor supernova light curves could directly measure the surviving binary fraction.
  • The models identify specific binary configurations that match known events, offering targets for multi-wavelength follow-up years after explosion.
  • Different choices for neutron-star birth kicks would change the exact bound fraction but are unlikely to erase the large difference between hydrogen-poor and hydrogen-rich channels.

Load-bearing premise

The analytic prescriptions implemented for the expansion of the companion star following its interaction with the SN ejecta accurately capture the physical response and subsequent orbital interaction with the compact object.

What would settle it

A large observational sample of hydrogen-poor core-collapse supernovae showing a rate of periodic light-curve modulations with 20-50 day periods well below 50 percent among surviving binaries would falsify the predicted occurrence fraction.

Figures

Figures reproduced from arXiv: 2605.21062 by Abel Schootemeijer, Andrea Ercolino, Avishay Gal-Yam, Caroline Mannes, Harim Jin, Luc Dessart, Norbert Langer, Ruggero Valli, Selma de Mink.

Figure 1
Figure 1. Figure 1: Schematic evolution of SN2022jli-like transients in binaries, from the explosion (top), through ejecta-companion interaction (ECI) and compact-object-companion interaction (CCI), to the deflation of the companion (bottom). Characteristic timescales are shown on the left, with t = 0 marking core collapse. quently, SN2022jli provides a unique laboratory for probing and constraining theoretical models of bina… view at source ↗
Figure 2
Figure 2. Figure 2: Fraction of the companions of Type Ibc and Type Ibn super￾nova progenitors at the time of explosion in the reference population model (Sect. 3.1). We distinguish those with no companion (single stars, merger products, or disrupted binaries; white), a degenerate companion (gray), or a non-degenerate companion (blue outline). Non-degenerate companions are further divided into those that remain bound (teal) a… view at source ↗
Figure 3
Figure 3. Figure 3: Population-wide distributions of post-explosion orbital period Ppost−SN, eccentricity epost−SN, and the number of times the NS pene￾trates the envelope of the companion Ninter, for H-poor supernovae un￾dergoing periodic CCI in the reference model. All histograms and 2D plots are normalized to the total number of supernovae exhibiting peri￾odic CCI, except the histogram of Ninter (brown). The histogram of N… view at source ↗
Figure 4
Figure 4. Figure 4: Distribution of the maximum luminosity Lmax (top) of ECI￾inflated non-degenerate companions to all H-poor supernovae in the reference population model. The bottom panel shows the companion’s maximum luminosity relative to the its pre-ECI luminosity. Values are normalized to the total number of H-poor supernovae. Orange and teal filling show systems with unbound and bound companions after explo￾sion, respec… view at source ↗
Figure 5
Figure 5. Figure 5: As [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Fraction of H-poor supernovae with periodic companion–compact-object interaction (CCI) for different popu￾lation models, versus the fraction of binaries in which the primary star explodes and forms a NS that is bound to the companion, fNS,bound, normalized to all systems where the primary undergoes core collapse. Colors indicate the kick prescription (k1–k3), markers the merger criterion (m1–m5), and shade… view at source ↗
Figure 7
Figure 7. Figure 7: Post-supernova orbital period (left) and eccentricity (right) distributions for binary models where periodic CCI is expected. Each line shows the results from a different population model, with those discussed in Sect. 3 shown with thicker lines (see legend) while those with other parameter combinations (see [PITH_FULL_IMAGE:figures/full_fig_p007_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: As [PITH_FULL_IMAGE:figures/full_fig_p008_8.png] view at source ↗
read the original abstract

Most massive stars live in binary systems. When the first supernova (SN) in a binary occurs, the ejecta hit the companion, which may inflate as a consequence, and then interacts with the newly formed compact object. The recent Type Ic SN2022jli shows a periodic modulation in its emission, which is interpreted as evidence for such interaction. We derive predictions for the occurrence rate and observables of SNe exhibiting these companion - compact-object interactions (CCIs). We analyze a comprehensive, state-of-the-art grid of detailed binary stellar evolution models, and implement analytic prescriptions for the expansion of the companion star following its interaction with the SN ejecta. We employ the newly developed population synthesis code SN-ORACLE to derive the distribution functions of the properties of the SNe affected by CCI and their companions, where we use different explodability and neutron star birth kick distributions. We find that periodic CCI is expected to occur in more than half of the binary systems that produce a hydrogen-poor core collapse SN and are not disrupted, while the occurrence rate in systems producing hydrogen-rich SNe is small. We find broad period ranges, peaking around 20-50 days, with the interaction lasting for 0.5-10 years. We identify specific binary evolution models that reproduce the observed period of the light curve undulations of SN2022jli, SN2015ap, and SN2022esa. The inflation of the companion also increases its luminosity and brightness, increasing its detectability with current instruments. For SN2022jli, our best fitting models predict a J-band magnitude of 21-23 for up to 10 years. We find that up to 27% of H-poor SNe could show periodicity in their light curves, while only a few such events have been identified so far. Our results may help find periodic CCI features in future and archival SN observations.

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 / 2 minor

Summary. The manuscript analyzes a comprehensive grid of detailed binary stellar evolution models with the newly developed SN-ORACLE population synthesis code. It implements analytic prescriptions for companion-star expansion after SN ejecta impact and derives occurrence rates, period distributions, and observables for periodic neutron-star–companion interactions (CCI) in core-collapse supernovae, using varied explodability and kick prescriptions. The central claim is that periodic CCI occurs in more than half of non-disrupted hydrogen-poor CCSN binaries (with periods peaking at 20–50 days and durations 0.5–10 yr) while remaining rare for hydrogen-rich events; specific models are identified that reproduce the light-curve periods of SN 2022jli, SN 2015ap, and SN 2022esa.

Significance. If the analytic expansion prescriptions hold, the work supplies concrete, falsifiable predictions for periodic modulations in SN light curves and for the long-term brightness of companions, directly relevant to ongoing and archival searches. Credit is due for the use of state-of-the-art detailed binary grids, the introduction of the SN-ORACLE code, and the explicit matching of individual evolutionary sequences to three observed events. The quantitative rates, however, rest on unvalidated analytic steps whose accuracy controls the headline >50 % fraction.

major comments (2)
  1. [Methods / analytic prescriptions] The section describing the analytic prescriptions for companion expansion and cooling (post-ejecta impact): the >50 % periodic-CCI rate for non-disrupted H-poor systems is obtained by post-processing the binary grid with these prescriptions. No quantitative comparison to hydrodynamical simulations is reported for the mass ratios and orbital separations realized in the grid; an error in the assumed expansion factor or cooling timescale would directly rescale the reported fraction and the H-poor versus H-rich distinction.
  2. [Results / occurrence rates] Results section on occurrence rates and period distributions: no error propagation or sensitivity study is presented for the derived fractions with respect to plausible variations in the explodability prescription, neutron-star kick distribution, or the free parameters of the analytic expansion model. This omission leaves the robustness of the central >50 % claim and the 0.5–10 yr duration range difficult to assess.
minor comments (2)
  1. [Abstract] Abstract: the statement that 'up to 27 % of H-poor SNe could show periodicity' is not immediately reconciled with the >50 % rate among non-disrupted binaries; a short parenthetical on the disrupted fraction would remove ambiguity.
  2. [Figures] Figure showing period distributions: inclusion of the corresponding distribution for H-rich systems would allow immediate visual comparison and strengthen the claimed contrast.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed review of our manuscript. We address each major comment below and describe the revisions we will implement to improve the robustness and clarity of our results.

read point-by-point responses

  1. Referee: [Methods / analytic prescriptions] The section describing the analytic prescriptions for companion expansion and cooling (post-ejecta impact): the >50 % periodic-CCI rate for non-disrupted H-poor systems is obtained by post-processing the binary grid with these prescriptions. No quantitative comparison to hydrodynamical simulations is reported for the mass ratios and orbital separations realized in the grid; an error in the assumed expansion factor or cooling timescale would directly rescale the reported fraction and the H-poor versus H-rich distinction.

    Authors: We acknowledge that the manuscript does not include a direct quantitative comparison of the analytic prescriptions to hydrodynamical simulations specifically for the mass ratios and orbital separations present in our binary grid. The prescriptions are based on analytic models calibrated against existing hydrodynamical studies in the literature. To address this point, we will add a dedicated paragraph in the methods section discussing the validity range of the prescriptions, citing the relevant hydrodynamical benchmarks, and include a sensitivity analysis varying the expansion factor and cooling timescale within plausible uncertainties. This will quantify the effect on the reported occurrence rates. revision: yes

  2. Referee: [Results / occurrence rates] Results section on occurrence rates and period distributions: no error propagation or sensitivity study is presented for the derived fractions with respect to plausible variations in the explodability prescription, neutron-star kick distribution, or the free parameters of the analytic expansion model. This omission leaves the robustness of the central >50 % claim and the 0.5–10 yr duration range difficult to assess.

    Authors: The manuscript already explores results across multiple explodability prescriptions and neutron-star kick distributions, with the >50% fraction for non-disrupted H-poor systems remaining consistent. We agree, however, that a more systematic sensitivity study including variations in the free parameters of the analytic expansion model and basic error propagation would better demonstrate robustness. In the revised version we will add a new subsection or appendix presenting these sensitivity tests, including how the central fraction and duration range respond to changes in the analytic parameters. revision: partial

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper derives CCI occurrence rates (>50% for non-disrupted H-poor CCSN binaries) by post-processing an external grid of detailed binary evolution models with analytic prescriptions for companion expansion after ejecta impact, then feeding results into the new SN-ORACLE population synthesis code along with separate explodability and kick distributions. No step reduces by construction to its own inputs: the rates are forward predictions from the binary grid properties (separations, mass ratios) rather than any fitted parameter, self-definitional loop, or load-bearing self-citation. The H-poor vs. H-rich distinction follows directly from the grid's orbital statistics, which are independent of the CCI classification step. The derivation remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim depends on the accuracy of detailed binary evolution calculations, the validity of analytic post-interaction expansion rules, and the chosen distributions for explodability and neutron-star kicks; these are treated as inputs rather than derived quantities.

free parameters (2)
  • explodability and neutron star birth kick distributions
    Different distributions are employed to generate the final statistics; their specific functional forms and parameters are not derived within the work.
  • analytic prescriptions for companion expansion
    Implemented to model the response to SN ejecta; the functional form and any scaling constants are introduced rather than derived from first principles.
axioms (2)
  • domain assumption Most massive stars live in binary systems.
    Opening statement of the abstract; used to motivate the entire binary-evolution framework.
  • domain assumption The detailed binary stellar evolution models in the grid correctly capture mass transfer, common-envelope phases, and core evolution up to the supernova.
    The population synthesis is built directly on this pre-existing grid.

pith-pipeline@v0.9.0 · 5920 in / 1599 out tokens · 41942 ms · 2026-05-21T02:09:12.099470+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

300 extracted references · 300 canonical work pages · 131 internal anchors

  1. [1]

    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

  2. [2]

    2013, Astrophysical Journal Supplement Series, 208, 4, doi: 10.1088/0067-0049/208/1/4

    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

  3. [3]

    2015, ApJS, 220, 15, doi: 10.1088/0067-0049/220/1/15

    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

  4. [4]

    B., et al

    Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions. , keywords =. doi:10.3847/1538-4365/aaa5a8 , archivePrefix =. 1710.08424 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/aaa5a8

  5. [5]

    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

  6. [6]

    , year = 1955, month = jan, volume =

    The Luminosity Function and Stellar Evolution. , year = 1955, month = jan, volume =. doi:10.1086/145971 , adsurl =

    work page doi:10.1086/145971 1955

  7. [7]

    , keywords =

    SN 1993J: A Type IIb Supernova. , keywords =. doi:10.1086/174319 , adsurl =

    work page doi:10.1086/174319

  8. [8]

    , keywords =

    Luminous Type II Short-Plateau Supernovae 2006Y, 2006ai, and 2016egz: A Transitional Class from Stripped Massive Red Supergiants. , keywords =. doi:10.3847/1538-4357/abf6d6 , archivePrefix =. 2010.15566 , primaryClass =

    work page doi:10.3847/1538-4357/abf6d6 2010

  9. [9]

    Supernova Light Curves Powered by Fallback Accretion

    Supernova Light Curves Powered by Fallback Accretion. , keywords =. doi:10.1088/0004-637X/772/1/30 , archivePrefix =. 1210.7240 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/772/1/30

  10. [10]

    , keywords =

    The progenitor of supernova 1993J: a stripped supergiant in a binary system?. , keywords =. doi:10.1038/364509a0 , adsurl =

    work page doi:10.1038/364509a0

  11. [11]

    Supernovae from massive stars with extended tenuous envelopes

    Supernovae from massive stars with extended tenuous envelopes. , keywords =. doi:10.1051/0004-6361/201732363 , archivePrefix =. 1801.02056 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201732363

  12. [12]

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201220273

  13. [13]

    The chemical make-up of the Sun: A 2020 vision

    The chemical make-up of the Sun: A 2020 vision. , keywords =. doi:10.1051/0004-6361/202140445 , archivePrefix =. 2105.01661 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202140445 2020

  14. [14]

    , keywords =

    Radiative Atomic Rosseland Mean Opacity Tables. , keywords =. doi:10.1086/191659 , adsurl =

    work page doi:10.1086/191659

  15. [15]

    , keywords =

    OPAL Equation-of-State Tables for Astrophysical Applications. , keywords =. doi:10.1086/176705 , adsurl =

    work page doi:10.1086/176705

  16. [16]

    , keywords =

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

    work page doi:10.1086/156569

  17. [17]

    , keywords =

    The JINA REACLIB Database: Its Recent Updates and Impact on Type-I X-ray Bursts. , keywords =. doi:10.1088/0067-0049/189/1/240 , adsurl =

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

  18. [18]

    , keywords =

    Evolution of massive stars in the Large Magellanic Cloud : models with semiconvection. , keywords =

    work page

  19. [19]

    Constraining mixing in massive stars in the Small Magellanic Cloud

    Constraining mixing in massive stars in the Small Magellanic Cloud. , keywords =. doi:10.1051/0004-6361/201935046 , archivePrefix =. 1903.10423 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201935046 1903

  20. [20]

    The Binding Energy Parameter for Common Envelope Evolution

    The binding energy parameter for common envelope evolution. Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/16/8/126 , archivePrefix =. 1605.03668 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1674-4527/16/8/126

  21. [21]

    , keywords =

    Common Envelope Evolution and Double Cores of Planetary Nebulae. , keywords =. doi:10.1086/168974 , adsurl =

    work page doi:10.1086/168974

  22. [22]

    , keywords =

    The origin of subdwarf B stars - I. The formation channels. , keywords =. doi:10.1046/j.1365-8711.2002.05752.x , archivePrefix =. astro-ph/0206130 , primaryClass =

    work page doi:10.1046/j.1365-8711.2002.05752.x 2002

  23. [23]

    , keywords =

    The origin of subdwarf B stars - II. , keywords =. doi:10.1046/j.1365-8711.2003.06451.x , archivePrefix =. astro-ph/0301380 , primaryClass =

    work page doi:10.1046/j.1365-8711.2003.06451.x 2003

  24. [24]

    , keywords =

    Is Betelgeuse the Outcome of a Past Merger?. , keywords =. doi:10.3847/1538-4357/ab91bb , archivePrefix =. 2005.04172 , primaryClass =

    work page doi:10.3847/1538-4357/ab91bb 2005

  25. [25]

    Type Ib and IIb supernova progenitors in interacting binary systems

    Type Ib and IIb Supernova Progenitors in Interacting Binary Systems. , keywords =. doi:10.3847/1538-4357/aa6afe , archivePrefix =. 1701.02089 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa6afe

  26. [26]

    , keywords =

    Common envelopes in massive stars: towards the role of radiation pressure and recombination energy in ejecting red supergiant envelopes. , keywords =. doi:10.1093/mnras/stac049 , archivePrefix =. 2111.00923 , primaryClass =

    work page doi:10.1093/mnras/stac049

  27. [27]

    doi:10.1088/2514-3433/abb6f0 , adsurl =

    Common Envelope Evolution. doi:10.1088/2514-3433/abb6f0 , adsurl =

    work page doi:10.1088/2514-3433/abb6f0

  28. [28]

    On the Energy Equation and Efficiency Parameter of the Common Envelope Evolution

    On the energy equation and efficiency parameter of the common envelope evolution. , keywords =. doi:10.48550/arXiv.astro-ph/0007034 , archivePrefix =. astro-ph/0007034 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0007034

  29. [29]

    Common envelope: enthalpy consideration

    Common Envelope: Enthalpy Consideration. , keywords =. doi:10.1088/2041-8205/731/2/L36 , archivePrefix =. 1103.2790 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/731/2/l36 2041

  30. [30]

    , keywords =

    The role of mass transfer and common envelope evolution in the formation of merging binary black holes. , keywords =. doi:10.1051/0004-6361/202039992 , archivePrefix =. 2103.09243 , primaryClass =

    work page doi:10.1051/0004-6361/202039992

  31. [31]

    , keywords =

    The dependence of convective core overshooting on stellar mass. , keywords =. doi:10.1051/0004-6361/201628779 , adsurl =

    work page doi:10.1051/0004-6361/201628779

  32. [32]

    The spectroscopic Hertzsprung-Russell diagram of Galactic massive stars

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201425028

  33. [33]

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

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

  34. [34]

    , keywords =

    Parametrization of stellar rates of mass loss as functions of the fundamental stellar parameters M, L, and R. , keywords =

    work page

  35. [35]

    , keywords =

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

    work page

  36. [36]

    Mass-loss predictions for O and B stars as a function of metallicity

    Mass-loss predictions for O and B stars as a function of metallicity. , keywords =. doi:10.1051/0004-6361:20010127 , archivePrefix =. astro-ph/0101509 , primaryClass =

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

  37. [37]

    , keywords =

    Mass-loss rates of Wolf-Rayet stars as a function of stellar parameters. , keywords =

    work page

  38. [38]

    Towards a better understanding of the evolution of Wolf-Rayet stars and Type Ib/Ic supernova progenitors

    Towards a better understanding of the evolution of Wolf-Rayet stars and Type Ib/Ic supernova progenitors. , keywords =. doi:10.1093/mnras/stx1496 , archivePrefix =. 1706.04716 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1496

  39. [39]

    , keywords =

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

    work page

  40. [40]

    Presupernova Evolution of Rotating Massive Stars. I. Numerical Method and Evolution of the Internal Stellar Structure. , keywords =. doi:10.1086/308158 , archivePrefix =. astro-ph/9904132 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/308158

  41. [41]

    Formation of contact in massive close binaries

    Formation of contact in massive close binaries. , keywords =. doi:10.1051/0004-6361:20010151 , archivePrefix =. astro-ph/0102244 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20010151

  42. [42]

    The Internal Constitution of the Stars

    work page

  43. [43]

    , year = 1929, month = nov, volume =

    Internal circulation in rotating stars. , year = 1929, month = nov, volume =. doi:10.1093/mnras/90.1.54 , adsurl =

    work page doi:10.1093/mnras/90.1.54 1929

  44. [44]

    , year = 1950, month = jan, volume =

    The importance of rotation in stellar evolution. , year = 1950, month = jan, volume =. doi:10.1093/mnras/110.6.548 , adsurl =

    work page doi:10.1093/mnras/110.6.548 1950

  45. [45]

    , year = 1967, month = nov, volume =

    Differential Rotation in Stars. , year = 1967, month = nov, volume =. doi:10.1086/149360 , adsurl =

    work page doi:10.1086/149360 1967

  46. [46]

    a t station \

    Instabilit \"a t station \"a rer Rotation in Sternen. , year = 1968, month = jan, volume =

    work page 1968

  47. [47]

    , year = 1973, month = jan, volume =

    The adiabatic stability of stars containing magnetic fields-I.Toroidal fields. , year = 1973, month = jan, volume =. doi:10.1093/mnras/161.4.365 , adsurl =

    work page doi:10.1093/mnras/161.4.365 1973

  48. [48]

    IV - The influence of rotation

    The adiabatic stability of stars containing magnetic fields. IV - The influence of rotation. , keywords =. doi:10.1093/mnras/216.2.139 , adsurl =

    work page doi:10.1093/mnras/216.2.139

  49. [49]

    Dynamo action by differential rotation in a stably stratified stellar interior

    Dynamo action by differential rotation in a stably stratified stellar interior. , keywords =. doi:10.1051/0004-6361:20011465 , archivePrefix =. astro-ph/0108207 , primaryClass =

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

  50. [50]

    Comments on Astrophysics and Space Physics , keywords =

    Instabilities of Differential Rotation. Comments on Astrophysics and Space Physics , keywords =

    work page

  51. [51]

    Stellar Instability and Evolution , year = 1974, editor =

    Rotational Instabilities and Stellar Evolution. Stellar Instability and Evolution , year = 1974, editor =

    work page 1974

  52. [52]

    Presupernova Evolution of Differentially Rotating Massive Stars Including Magnetic Fields

    Presupernova Evolution of Differentially Rotating Massive Stars Including Magnetic Fields. , keywords =. doi:10.1086/429868 , archivePrefix =. astro-ph/0409422 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/429868

  53. [53]

    The evolution of rotating stars. II. Calculations with time-dependent redistribution of angular momentum for 7 and 10 M sun stars. , keywords =. doi:10.1086/155904 , adsurl =

    work page doi:10.1086/155904

  54. [54]

    , keywords =

    Evolutionary Models of the Rotating Sun. , keywords =. doi:10.1086/167210 , adsurl =

    work page doi:10.1086/167210

  55. [55]

    , keywords =

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

    work page

  56. [56]

    Single star progenitors of long gamma-ray bursts. I. Model grids and redshift dependent GRB rate. , keywords =. doi:10.1051/0004-6361:20065912 , archivePrefix =. astro-ph/0606637 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20065912

  57. [57]

    The rotation rates of massive stars: the role of binary interaction through tides, mass transfer and mergers

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/764/2/166

  58. [58]

    , keywords =

    Evolution of binary stars and the effect of tides on binary populations. , keywords =. doi:10.1046/j.1365-8711.2002.05038.x , archivePrefix =. astro-ph/0201220 , primaryClass =

    work page doi:10.1046/j.1365-8711.2002.05038.x 2002

  59. [59]

    doi:10.1007/978-3-662-55054-0 , adsurl =

    Supernova Explosions. doi:10.1007/978-3-662-55054-0 , adsurl =

    work page doi:10.1007/978-3-662-55054-0

  60. [60]

    Stripped-envelope stars in different metallicity environments. I. Evolutionary phases, classification, and populations. , keywords =. doi:10.1051/0004-6361/202142895 , archivePrefix =. 2112.06948 , primaryClass =

    work page doi:10.1051/0004-6361/202142895

  61. [61]

    Stripped-envelope stars in different metallicity environments. II. Type I supernovae and compact remnants. , keywords =. doi:10.1051/0004-6361/202243519 , archivePrefix =. 2204.00025 , primaryClass =

    work page doi:10.1051/0004-6361/202243519

  62. [62]

    , year = 1993, month = aug, volume =

    SN 1993J : explosion of a massive cool supergiant with a small envelope nass ?. , year = 1993, month = aug, volume =

    work page 1993

  63. [63]

    , keywords =

    Core-collapse explosions of Wolf-Rayet stars and the connection to Type IIb/Ib/Ic supernovae. , keywords =. doi:10.1111/j.1365-2966.2011.18598.x , archivePrefix =. 1102.5160 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.18598.x 2011

  64. [64]

    Interacting Binary Stars , year = 1985, editor =

    Stellar evolution and binaries. Interacting Binary Stars , year = 1985, editor =

    work page 1985

  65. [65]

    Thresholds for Rapid Mass Transfer in Binary System. I. Polytropic Models. , keywords =. doi:10.1086/165412 , adsurl =

    work page doi:10.1086/165412

  66. [66]

    The spectroscopic Hertzsprung-Russell diagram

    The spectroscopic Hertzsprung-Russell diagram. , keywords =. doi:10.1051/0004-6361/201423374 , archivePrefix =. 1403.2212 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201423374

  67. [67]

    , keywords =

    Thermonuclear and electron-capture supernovae from stripped-envelope stars. , keywords =. doi:10.1051/0004-6361/202243035 , archivePrefix =. 2201.00871 , primaryClass =

    work page doi:10.1051/0004-6361/202243035

  68. [68]

    , keywords =

    Standard models of Wolf-Rayet stars. , keywords =

    work page

  69. [69]

    arXiv e-prints , keywords =

    A model of anisotropic winds from rotating stars for evolutionary calculations. arXiv e-prints , keywords =. doi:10.48550/arXiv.2302.10992 , archivePrefix =. 2302.10992 , primaryClass =

    work page doi:10.48550/arxiv.2302.10992

  70. [70]

    Effects of winds on the leftover hydrogen in massive stars following Roche lobe overflow

    Effects of winds on the leftover hydrogen in massive stars following Roche lobe overflow. , keywords =. doi:10.1093/mnras/stz1134 , archivePrefix =. 1904.09221 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz1134 1904

  71. [71]

    Binary progenitor models of type IIb supernovae

    Binary progenitor models of type IIb supernovae. , keywords =. doi:10.1051/0004-6361/201015410 , archivePrefix =. 1102.1732 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201015410

  72. [72]

    Progenitors of Type IIb Supernovae. I. Evolutionary Pathways and Rates. , keywords =. doi:10.3847/1538-4357/ab4ad7 , archivePrefix =. 1808.07580 , primaryClass =

    work page doi:10.3847/1538-4357/ab4ad7

  73. [73]

    Progenitors of Type IIb Supernovae. II. Observable Properties. , keywords =. doi:10.3847/1538-4357/abb8d5 , archivePrefix =. 2009.06405 , primaryClass =

    work page doi:10.3847/1538-4357/abb8d5 2009

  74. [74]

    , keywords =

    How much hydrogen is in Type Ib and IIb supernova progenitors?. , keywords =. doi:10.1093/mnras/stac088 , archivePrefix =. 2111.04432 , primaryClass =

    work page doi:10.1093/mnras/stac088

  75. [75]

    Winds from stripped low-mass Helium stars and Wolf-Rayet stars

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201731902

  76. [76]

    Pulsations in red supergiants with high L/M ratio -- Implications for the stellar and circumstellar structure of supernova progenitors

    Pulsations in red supergiants with high L/M ratio. Implications for the stellar and circumstellar structure of supernova progenitors. , keywords =. doi:10.48550/arXiv.astro-ph/9705097 , archivePrefix =. astro-ph/9705097 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9705097

  77. [77]

    Implications of massive close binaries for black hole formation and supernovae

    Implications of massive close binaries for black hole formation and supernovae. , keywords =. doi:10.48550/arXiv.astro-ph/9904256 , archivePrefix =. astro-ph/9904256 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9904256

  78. [78]

    Efficiency of mass transfer in massive close binaries, Tests from double-lined eclipsing binaries in the SMC

    Efficiency of mass transfer in massive close binaries. Tests from double-lined eclipsing binaries in the SMC. , keywords =. doi:10.1051/0004-6361:20067007 , archivePrefix =. astro-ph/0703480 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20067007

  79. [79]

    The massive binary companion star to the progenitor of supernova 1993J

    The massive binary companion star to the progenitor of supernova 1993J. , keywords =. doi:10.1038/nature02161 , archivePrefix =. astro-ph/0401090 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature02161

  80. [80]

    Structure and Evolution of Close Binary Systems , year = 1976, editor =

    Common Envelope Binaries. Structure and Evolution of Close Binary Systems , year = 1976, editor =

    work page 1976

Showing first 80 references.