Pith. sign in

REVIEW 3 major objections 5 minor 3 cited by

The power of binaries on stripped-envelope supernovae across metallicity: uniform progenitor parameter space and persistently low ejecta masses, but subtype diversity

T0 review · 3 major / 5 minor · reviewed 2026-08-05 · deepseek-v4-flash

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

Pith's one-line read This paper argues that stripped-envelope supernovae are shaped far more by binary companions than by metallicity or stellar winds, with stable mass transfer in binaries the dominant stripping mechanism and common-envelope evolution contribu

desk verdict First POSYDON-based SESN population synthesis across metallicities; stable binary mass transfer dominates, with the CE<6% headline needing a fiducial qualifier. read the letter →

arxiv 2508.21042 v1 pith:24FOFX5Z submitted 2025-08-28 astro-ph.SR astro-ph.HE

D. Souropanis , E. Zapartas , T. Pessi , M. Briel , M. Renzo , C. P. Gutiérrez , J. J. Andrews , S. Gossage
show 4 more authors
M. U. Kruckow C. Liotine P. M. Srivastava E. Teng
This is my paper
classification astro-ph.SRastro-ph.HE
keywords stripped-envelopesupernovaebinarypopulationsynthesiscommonenvelopemetallicitydependenceejectamassessupernovasubtypesmasstransferstellarevolution
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper argues that stripped-envelope supernovae—explosions of massive stars that have lost their hydrogen envelopes—are shaped far more by binary companions than by metallicity or stellar winds. Using a binary population synthesis code built on grids of detailed stellar-structure models, the authors evolve 200,000 binary systems at each of six metallicities (0.01 to 2 times solar) and classify their explosions by predicted hydrogen and helium content. They find that the common-envelope channel produces less than 6% of these supernovae, secondary stars produce less than 11%, and the rest come from primary stars stripped through stable Roche-lobe mass transfer. The total stripped-envelope rate relative to hydrogen-rich Type II supernovae stays nearly flat across metallicity, while the subtype mix shifts from Type Ic/Ib at high metallicity toward Type IIb at low metallicity. Predicted ejecta masses remain low and roughly metallicity-independent, in contrast to single-star models, giving observational tests for the binary-dominated picture.

What carries the argument

The load-bearing instrument is a binary population synthesis calculation in which every binary is mapped onto grids of detailed stellar evolution simulations, so mass-transfer rates, envelope binding energies, and final core structures come from stellar-structure models rather than fitting formulas. The central mechanism is the post-core-helium-depletion mass-transfer episode: at low metallicity, partially stripped stars retain enough hydrogen to re-expand and fill their Roche lobe again, stripping the envelope further and erasing metallicity differences in ejecta mass. The common-envelope outcome is governed by the alpha/lambda formalism with envelope binding energies computed from the deta

What would settle it

Compare the stripped-envelope-to-Type-II ratio and the Type IIb/Type Ib split in a volume-limited, untargeted sample of supernovae with host metallicities spanning 0.1 to 2 solar. If the ratio rises steeply with metallicity, or if ejecta masses of Type Ib/IIb supernovae increase toward metal-poor hosts as single-star models predict, the binary-stable-mass-transfer picture would be falsified. A more targeted test: measure the fraction of stripped-envelope supernovae with surviving binary companions on wide orbits; under the paper's picture most should have such companions, while under single-st

Watch

Extended reading notes

Core claim

The paper's central claim is that stable mass transfer in binaries, rather than common-envelope ejection or line-driven winds, is the dominant mechanism producing stripped-envelope supernovae across all metallicities from 0.01 to 2 solar. In the authors' detailed binary grids, unstable mass transfer is rarer than rapid population synthesis codes have assumed, and when it does occur the envelope is usually too tightly bound to be ejected, so common-envelope survivors contribute under 6% of the stripped-envelope population. The majority of progenitors are primary stars that lose their hydrogen envelopes through one or more stable Roche-lobe overflow episodes; a crucial late episode after core

Load-bearing premise

The conclusion that common-envelope evolution contributes less than 6% of stripped-envelope supernovae rests on the model's criteria for when mass transfer turns dynamically unstable and on the assumed common-envelope efficiency; if real envelopes are ejected more easily than the default assumption allows, the common-envelope fraction could climb well above 6%.

Editorial extensions

If this is right

  • If the central claim holds, untargeted surveys should see a stripped-envelope-to-Type-II ratio that is nearly flat from 0.01 to 2 solar metallicity, even as the Ib/Ic fractions drop and IIb fractions rise at low metallicity.
  • Ejecta masses of stripped-envelope supernovae should remain low and roughly constant with host metallicity; a clear rise toward metal-poor hosts would favor single-star stripping instead.
  • The progenitor age sequence should reverse at low metallicity: Type IIb from the most massive (shortest-lived) progenitors, Type Ib from lower-mass stars with long lifetimes—a testable environmental signature.
  • Most stripped-envelope progenitors should show signs of stable Roche-lobe mass transfer (e.g., relatively wide surviving binaries or stripped companions) rather than post-common-envelope tight orbits.
  • Observed subtype-rate differences between surveys may be driven largely by the hydrogen-envelope threshold separating Type IIb and Type Ib; predicting the tentative Type I(I)b class as a distinct category would sharpen the test.

Reading between the lines

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

  • If the common-envelope contribution is truly below 6%, the common-envelope channel is unlikely to be the main factory of compact-object mergers among stripped stars; stable mass-transfer products may deserve more attention as gravitational-wave progenitors.
  • The paper's flat-rate result assumes a binary fraction of 0.6; if low-metallicity galaxies have close-binary fractions near 0.8, as some recent surveys suggest, the predicted stripped-envelope rate would rise with decreasing metallicity, reversing the headline flatness.
  • The tentative Type I(I)b class is a sharp diagnostic: measuring the true hydrogen threshold in real spectra would let observers choose between the paper's Ib and IIb rate assignments, turning a classification nuisance into a physical measurement.
  • If the late post-helium-depletion mass transfer is as common as the models imply, many stripped progenitors should explode while still Roche-lobe filling, making polarization and early circumstellar interaction signatures more frequent in low-metallicity stripped supernovae.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. This paper uses POSYDON v2, with its MESA-based single- and binary-star grids, to evolve 2×10^5 systems at six metallicities (0.01–2 Z_sun) and predict which channels produce stripped-envelope supernovae (SESNe). The authors report that stable mass transfer from primary stars dominates, that common-envelope ejection produces <6% of SESNe and secondaries <11%, that the overall SESN/II ratio is nearly metallicity-independent while subtype fractions (Ic/Ib/IIb) depend strongly on Z, that predicted SESN ejecta masses are low and nearly Z-independent, and that the age (progenitor-mass) ordering of subtypes reverses at low Z. The conclusions are supported by a 15-model robustness suite varying α_CE, core-envelope boundary, SN engine, kicks, binary fraction, and interpolation scheme, and by comparisons to environmental and volumetric SN rate data.

Significance. If the results hold, the paper provides a strong quantitative case that binary interactions—specifically stable Roche-lobe overflow rather than common-envelope episodes or single-star winds—are the dominant formation channel of SESNe across metallicity. The predictions are falsifiable: nearly Z-independent ejecta-mass distributions, a subtype-age reversal at Z<0.2 Z_sun, and a near-constant SESN/II ratio. The study is notable for using published, open POSYDON grids (commit 891c5897), for taking classification thresholds from external spectral models rather than fitting, and for an unusually extensive sensitivity analysis. The central caveat is that one headline quantitative claim (CE<6%) is not robust to the paper's own α_CE=5 run, and the subtype-rate comparisons are sensitive to the explosion engine at high Z.

major comments (3)
  1. [Abstract; §5.1; §6.2 and Table D2] The abstract and conclusion state that the common-envelope (CE) channel contributes <6% of SESNe. From Table 1, the fiducial solar run indeed has a CE-origin fraction of roughly 2–3% among SESNe. However, in the α_CE=5 robustness run (Table D2), Type Ib increases from 16,295 to 17,694 and Type Ic from 420 to 470, while Type II falls from 58,250 to 54,975. Since α_CE changes only CE survival, the net SESN increase of ~1,474 is CE-origin; adding the ~440 CE-origin SESNe of the fiducial run gives at least ~1,900 of 21,428 SESNe, i.e. ~9%, exceeding 6%. The text does not report the CE fraction for this model, so the headline bound is not robust to one of the paper's own tested parameters. Please report CE-origin fractions for all 15 models and qualify the claim.
  2. [§5.2; §6.2; Table D2] The solar IIb/II ratio changes by a factor of 3.3 across explosion engines: 2467/58250=4.2% (default), 4258/51790=8.2% (S+16), and 8410/60641=13.9% (F+12_delayed). Section 5.2 uses the default value to claim that models underpredict observed IIb/II (~12–16% at high Z) and attributes this offset to wind mass loss; the F+12_delayed run in the paper's own Table D2 removes most of that discrepancy. Since the IIb/II trend is central to the subtype-diversity claim and to the quantitative comparison with observations, the conclusions should be stated as engine-dependent, or the paper should discuss which subtype conclusions survive under all three engines.
  3. [§2 (Mass transfer/Common envelope); §6.2] The CE<6% conclusion rests in part on POSYDON's stability criteria (Mdot>0.1 Msun/yr, L2 overflow, photon-trapping radius). None of the 15 models varies these thresholds; only α_CE and the core-envelope boundary are changed. Given that the criteria determine how many systems enter CE, a test with, e.g., a lower or higher Mdot threshold would quantify the uncertainty in 'unstable MT is less frequent than previously thought' (§5.1). Without such a test, the stability boundary remains an untested, load-bearing assumption.
minor comments (5)
  1. [Appendix C, Figure C1 caption] Typo: 'mettalicity' should be 'metallicity'.
  2. [Table 1] Percentage notation is inconsistent: e.g., '86.9 (3.06 %)' vs '91.97 % (3.29 %)'; the Type Ib 'Merged' row reads '0.06 0.03 %' without units. Please unify formatting.
  3. [§6.2; Table D2] The text says '13 distinct binary population models' but Table D2 lists 15 rows including defaults (six variations at solar plus default, seven at subsolar plus default). Please clarify the count.
  4. [§5.2] Typo: 'This highligts that the adopted hydrogen-envelope mass threshold...' should be 'highlights'.
  5. [Conclusions, item 5] Typo: 'core collpase' should be 'core collapse'.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the headline claims are population-synthesis outputs from stated physical assumptions, not quantities fitted to the data they explain.

full rationale

The paper's derivation chain is self-contained: initial conditions are taken from external observational distributions (Kroupa IMF, Sana et al. 2013 periods), stellar and binary evolution is computed with the publicly available POSYDON/MESA grids, SN explodability uses external prescriptions (Patton & Sukhbold 2020, Tauris et al. 2015), and SESN classification thresholds are adopted from external spectroscopic studies (Dessart & Hillier 2011, Hachinger et al. 2012, Dessart et al. 2020). The key claims — CE channel <6% of SESNe, secondary channel <11%, stable mass transfer dominant, flat SESN/II ratio, nearly metallicity-independent ejecta masses — are outputs of the population synthesis, not fitted parameters. The CE fraction is explicitly sensitive to the stated alpha_CE=1 assumption and the stability criteria; the paper reports an alpha_CE=5 sensitivity run (Table D2) and discusses the resulting changes. This is an honest robustness check, not a circularity. Citations to POSYDON (Fragos et al. 2023, Andrews et al. 2024) are code references to open, benchmarked infrastructure, not an unverified uniqueness theorem or an ansatz smuggled in to force the conclusion. Observed rates are used only for comparison, not calibration. Therefore the central results do not reduce by construction to their inputs. The moderate score reflects only the natural reliance of the analysis on the authors' own POSYDON code and prior papers, which is not load-bearing circularity.

Assumptions & free parameters 8 free parameters · 6 assumptions · 0 invented entities

The central claims rest on a suite of modeling choices. Most are explored in the sensitivity study, but the fiducial values anchor the headline numbers: the CE<6% share depends on alpha_CE=1 and on POSYDON's instability criteria; subtype fractions depend on the explodability engine and on the H/He/N classification thresholds; absolute rates depend on the assumed binary fraction. No new physical entities are introduced; the tentative Type I(I)b is a classification bin, not a physical object.

free parameters (8)
  • Common envelope efficiency alpha_CE = 1 (default; 5 also tested)
    Determines the fraction of orbital energy used to eject the envelope; directly sets CE survival and thus the CE channel fraction (the headline <6% claim).
  • Core-envelope boundary for lambda_CE = X_H < 0.3 (default; 0.1 tested)
    Changes envelope binding energy and CE outcome; alters Type Ib/II ratios modestly.
  • Binary fraction f_bin = 0.6 (default; 0.8 tested)
    Scales all binary-channel rates; a higher low-metallicity binary fraction raises SESN/II ratios notably.
  • Supernova explodability prescription = Patton & Sukhbold 2020 N20 (default); Sukhbold+16 and Fryer+12 delayed tested
    Determines which stripped cores explode; switching prescriptions changes the solar IIb/II ratio from about 4% to 15%.
  • Type IIb/Ib classification H threshold = M_H,ej <= 0.5 Msun (IIb); <= 0.001 Msun (Ib); 0.001-0.033 tentative I(I)b
    Adopted from literature; directly sets subtype fractions, especially at low metallicity.
  • Type Ib/Ic classification He/N thresholds = X(4He) < 0.5 and X(14N) < 1e-4 for Ic
    From Dessart et al. 2020; conservative criterion shifts borderline stars to Ib, affecting Ic rates.
  • Wind mass-loss prescription for partially stripped stars = Nugis & Lamers (2000); weaker Vink (2017) rates not adopted
    Stronger winds favor Ib over IIb at high Z; the paper notes this could overproduce Type Ib.
  • Natal kick dispersion = 265 km/s CCSN, 20 km/s ECSN (default); 61.6 km/s tested
    Affects survival and disruption of binaries involving secondaries; minor effect overall.
assumptions (6)
  • domain assumption POSYDON v2's detailed MESA grids accurately represent the evolution of all binary systems in the sampled parameter space
    Nearest-neighbor assignment maps each system to the closest grid model; grid fidelity and coverage are assumed (Section 2).
  • domain assumption The adopted explodability model (Patton & Sukhbold 2020 with N20 engine) maps core C/O mass and carbon abundance to SN outcome
    Section 2. The paper's own sensitivity tests show large variations with Sukhbold+16 and Fryer+12 delayed prescriptions.
  • domain assumption Classification via ejecta H, He, N abundances at core carbon depletion maps monotonically to observed SN spectroscopic types
    Section 2.1, based on Dessart & Hillier 2011, Hachinger 2012, and Dessart et al. 2020.
  • domain assumption Binary parameter distributions (Kroupa IMF, Sana+2013 periods, uniform mass ratio) apply at all six metallicities
    Section 2; the paper notes lower-metallicity environments may have higher binary fractions and tests f_bin=0.8.
  • domain assumption Wind prescriptions (Dutch scheme, Vink, Nugis & Lamers, LBV) with their metallicity scalings are valid across 0.01-2 Zsun
    Section 2 and 6.1; high RSG and LBV wind rates remain uncertain.
  • domain assumption Burst star formation (all stars born at once) is representative for computing rate ratios
    Section 2; single-burst SFH assumed for the fiducial population.

how reviews work

0 comments
Cite this review

Pith. "Pith review of The power of binaries on stripped-envelope supernovae across metallicity: uniform progenitor parameter space and persistently low ejecta masses, but subtype diversity." pith.science (2026). https://pith.science/paper/24FOFX5Z

@misc{pith2026250821042,
  author       = {Pith},
  title        = {Pith review of: The power of binaries on stripped-envelope supernovae across metallicity: uniform progenitor parameter space and persistently low ejecta masses, but subtype diversity},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/24FOFX5Z}},
  note         = {Machine review of arXiv:2508.21042}
}
abstract

Stripped-envelope supernovae (SESNe) originate from massive stars that lose their envelopes through binary interactions or stellar winds. The connection between SESN subtypes and their progenitors remains poorly understood, as does the influence of initial mass, binarity, explodability, and metallicity on their evolutionary pathways, relative rates, ejecta masses, and progenitor ages. Here, we investigate these properties across a wide metallicity range (0.01-2 $Z_{\odot}$) using POSYDON, a state-of-the-art population synthesis code that incorporates detailed single- and binary-star model grids. We find that the common-envelope channel contributes less than 6% of SESNe, since unstable mass transfer is found less frequent than previously thought and rarely leads to CE survival when envelope binding energies are computed from detailed stellar models. The secondary channel accounts for less than 11%, while the vast majority of SESNe originate from primary stars in binaries undergoing stable mass-transfer episodes. These interactions maintain a largely metallicity-independent SESN parameter space, making the overall SESN rate almost insensitive to metallicity. In contrast, subtype fractions exhibit strong metallicity dependence, though their exact values remain affected by classification thresholds. The age distributions and therefore the progenitor masses of different SESN types also vary significantly with metallicity, revealing metallicity-dependent trends that can be tested observationally. Predicted SESN ejecta masses remain nearly constant across metallicity, in contrast to single-star models, and fall within observed ranges. Future transient surveys, combined with statistical environmental studies that constrain metallicity dependence, will provide decisive tests of these predictions and of the dominant role of binary interactions in shaping SESNe.

Figures

Figures reproduced from arXiv: 2508.21042 by the authors.

Figure 1
Figure 1. Parameter space for primary progenitors of SN Ic, Ib, I(I)b, IIb and II at solar metallicity. Each panel refers to a different initial mass ratio. See Section 2.1 for SN type classifications and definitions of mass transfer. Here, blue shaded area refer to Type Ib, cyan to Type Ic, yellow to Type IIb, yellow with a blue hatch to Type I(I)b and red to Type II. Each non circular point in the pannels corresponds to one… view at source ↗
Figure 2
Figure 2. Three 2D slices summarizing the evolution of systems from POSYDON grids of binary star models consisting of a hydrogen-rich star and a 12 M⊙ (left pannel), 7 M⊙ (midle pannel) BH and a 1.38 M⊙ NS (right pannel) at the onset of Roche lobe overflow. At these panels we oveplot the seconaries that remained bounded following the collapse of the primary star, initiated mass transfer and manage to explode as SNe (contoured… view at source ↗
Figure 3
Figure 3. Same as [PITH_FULL_IMAGE:figures/full_fig_p010_3.png] view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: Ratio between different SN types, as a function of metallicity (solid and dashed lines refer to this work, while the different colors refer to ratios between different SN types to Type II) orange: IIb/II, blue: Ibc/II and black (Ic+Ib+IIb)/II. SN observations from the …
Figure 5
Figure 5. Figure 5: Mean values (solid or dashed lines) and standard deviation (shaded areas) of ejecta masses from our fiducial population for Type Ib, IIb and Ic SNe, at different metallicities. For Types Ib and IIb, we consider two alternative assumptions: (i) grouping the tentative I(…
Figure 6
Figure 6. Figure 6: Median explosion times (solid lines) for different SN types as a function of metallicity, with shaded regions indicating the 25th and 75th percentiles. Each color corresponds to a specific SN type: cyan for Type Ic, blue for Type Ib combined with I(I)b, yellow for Type…
Figure 7
Figure 7. Figure 7: The fractions of SESNe subtypes to Type II for our 15 models, see text in subsection 6.2 for the different model assumptions secondaries interacting with a BH is modest, resulting in only a slight increase. We also ran a simulation at 0.1 Z⊙ assuming a binary fraction …

Discussion (0). Sign in to comment.

Forward citations

Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. A statistical study of the environmental age of core-collapse supernovae based on VLT/MUSE integral-field-unit spectroscopy

    astro-ph.SR 2026-04 unverdicted novelty 6.0 of 10

    Type Ic core-collapse supernovae explode in systematically younger environments than Types II, IIb, and Ib, indicating they arise from more massive progenitors via a distinct channel.

  2. A statistical study of the environmental age of core-collapse supernovae based on VLT/MUSE integral-field-unit spectroscopy

    astro-ph.SR 2026-04 conditional novelty 6.0 of 10

    Type Ic core-collapse supernovae sit in systematically younger environments than Types II(P), IIb, and Ib, which show no significant age differences among themselves.

  3. Relative frequencies of core-collapse supernovae as a function of metallicity: observations vs theoretical predictions

    astro-ph.HE 2026-04 unverdicted novelty 4.0 of 10

    Observations show a slight rise in stripped-envelope supernovae relative to hydrogen-rich ones at higher metallicities, with binary-interaction or rotation models able to match the trends though no unique scenario fits best.

Reference graph

Works this paper leans on

214 extracted references · 22 canonical work pages · cited by 2 Pith papers

  1. [1]

    Aguilera-Dena D. R., M \"u ller B., Antoniadis J., Langer N., Dessart L., Vigna-G \'o mez A., Yoon S.-C., 2023, @doi [ ] 10.1051/0004-6361/202243519 , https://ui.adsabs.harvard.edu/abs/2023A&A...671A.134A 671, A134

    doi:10.1051/0004-6361/202243519 2023

  2. [2]

    A., et al., 2017, @doi [ ] 10.1051/0004-6361/201629844 , https://ui.adsabs.harvard.edu/abs/2017A&A...598A..84A 598, A84

    Almeida L. A., et al., 2017, @doi [ ] 10.1051/0004-6361/201629844 , https://ui.adsabs.harvard.edu/abs/2017A&A...598A..84A 598, A84

    doi:10.1051/0004-6361/201629844 2017

  3. [3]

    P., Covarrubias R

    Anderson J. P., Covarrubias R. A., James P. A., Hamuy M., Habergham S. M., 2010, @doi [ ] 10.1111/j.1365-2966.2010.17118.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.407.2660A 407, 2660

    arXiv 2010

  4. [5]

    P., James P

    Anderson J. P., James P. A., Habergham S. M., Galbany L., Kuncarayakti H., 2015, @doi [ ] 10.1017/pasa.2015.19 , https://ui.adsabs.harvard.edu/abs/2015PASA...32...19A 32, e019

    doi:10.1017/pasa.2015.19 2015

  5. [6]

    J., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2411.02376 , https://ui.adsabs.harvard.edu/abs/2024arXiv241102376A p

    Andrews J. J., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2411.02376 , https://ui.adsabs.harvard.edu/abs/2024arXiv241102376A p. arXiv:2411.02376

    arXiv doi:10.48550/arxiv.2411.02376 2024

  6. [7]

    Z., de Wit S., Zapartas E., Munoz-Sanchez G., Maravelias G., 2024, @doi [ ] 10.1051/0004-6361/202449383 , https://ui.adsabs.harvard.edu/abs/2024A&A...686A..88A 686, A88

    Antoniadis K., Bonanos A. Z., de Wit S., Zapartas E., Munoz-Sanchez G., Maravelias G., 2024, @doi [ ] 10.1051/0004-6361/202449383 , https://ui.adsabs.harvard.edu/abs/2024A&A...686A..88A 686, A88

    doi:10.1051/0004-6361/202449383 2024

  7. [8]

    279, Death of Massive Stars: Supernovae and Gamma-Ray Bursts

    Arcavi I., 2012, in Roming P., Kawai N., Pian E., eds, IAU Symposium Vol. 279, Death of Massive Stars: Supernovae and Gamma-Ray Bursts. pp 34--39 ( @eprint arXiv 1209.5474 ), @doi 10.1017/S1743921312012653

    arXiv 2012

  8. [9]

    Arcavi I., et al., 2010, @doi [ ] 10.1088/0004-637X/721/1/777 , https://ui.adsabs.harvard.edu/abs/2010ApJ...721..777A 721, 777

    doi:10.1088/0004-637x/721/1/777 2010

Show all 214 references
  1. [10]

    Arcavi I., et al., 2017, @doi [ ] 10.3847/2041-8213/aa5be1 , https://ui.adsabs.harvard.edu/abs/2017ApJ...837L...2A 837, L2

    2017 doi

  2. [11]

    J., Scott P., 2009, @doi [ ] 10.1146/annurev.astro.46.060407.145222 , https://ui.adsabs.harvard.edu/abs/2009ARA&A..47..481A 47, 481

    Asplund M., Grevesse N., Sauval A. J., Scott P., 2009, @doi [ ] 10.1146/annurev.astro.46.060407.145222 , https://ui.adsabs.harvard.edu/abs/2009ARA&A..47..481A 47, 481

    2009

  3. [12]

    Bacon R., et al., 2014, The Messenger, https://ui.adsabs.harvard.edu/abs/2014Msngr.157...13B 157, 13

    2014

  4. [13]

    I., Evans C

    Banyard G., Sana H., Mahy L., Bodensteiner J., Villase \ n or J. I., Evans C. J., 2022, @doi [ ] 10.1051/0004-6361/202141037 , https://ui.adsabs.harvard.edu/abs/2022A&A...658A..69B 658, A69

    2022 doi

  5. [14]

    Barbarino C., et al., 2021, @doi [ ] 10.1051/0004-6361/202038890 , https://ui.adsabs.harvard.edu/abs/2021A&A...651A..81B 651, A81

    2021 doi

  6. [15]

    S., et al., 2023, @doi [Nature Astronomy] 10.1038/s41550-023-02018-5 , https://ui.adsabs.harvard.edu/abs/2023NatAs...7.1090B 7, 1090

    Bavera S. S., et al., 2023, @doi [Nature Astronomy] 10.1038/s41550-023-02018-5 , https://ui.adsabs.harvard.edu/abs/2023NatAs...7.1090B 7, 1090

    2023 doi

  7. [16]

    R., Smith N., 2022, @doi [ ] 10.3847/1538-4357/ac6dcf , https://ui.adsabs.harvard.edu/abs/2022ApJ...933...41B 933, 41

    Beasor E. R., Smith N., 2022, @doi [ ] 10.3847/1538-4357/ac6dcf , https://ui.adsabs.harvard.edu/abs/2022ApJ...933...41B 933, 41

    2022 doi

  8. [17]

    R., Davies B., Smith N., van Loon J

    Beasor E. R., Davies B., Smith N., van Loon J. T., Gehrz R. D., Figer D. F., 2023, @doi [ ] 10.1093/mnras/stad1818 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.524.2460B 524, 2460

    2023 doi

  9. [18]

    C., Sarazin C

    Begelman M. C., Sarazin C. L., 1986, @doi [ ] 10.1086/184637 , https://ui.adsabs.harvard.edu/abs/1986ApJ...302L..59B 302, L59

    1986 doi

  10. [19]

    L., Ruiter A., Valsecchi F., Vink J

    Belczynski K., Bulik T., Fryer C. L., Ruiter A., Valsecchi F., Vink J. S., Hurley J. R., 2010, @doi [ ] 10.1088/0004-637X/714/2/1217 , https://ui.adsabs.harvard.edu/abs/2010ApJ...714.1217B 714, 1217

    2010 doi

  11. [20]

    C., et al., 2012, @doi [ ] 10.1088/0004-637X/757/1/31 , https://ui.adsabs.harvard.edu/abs/2012ApJ...757...31B 757, 31

    Bersten M. C., et al., 2012, @doi [ ] 10.1088/0004-637X/757/1/31 , https://ui.adsabs.harvard.edu/abs/2012ApJ...757...31B 757, 31

    2012 doi

  12. [21]

    C., et al., 2018, @doi [ ] 10.1038/nature25151 , https://ui.adsabs.harvard.edu/abs/2018Natur.554..497B 554, 497

    Bersten M. C., et al., 2018, @doi [ ] 10.1038/nature25151 , https://ui.adsabs.harvard.edu/abs/2018Natur.554..497B 554, 497

    2018 doi

  13. [22]

    Blaauw A., 1961, , https://ui.adsabs.harvard.edu/abs/1961BAN....15..265B 15, 265

    1961

  14. [23]

    Bloecker T., 1995, , https://ui.adsabs.harvard.edu/abs/1995A&A...297..727B 297, 727

    1995

  15. [24]

    Boissier S., Prantzos N., 2009, @doi [ ] 10.1051/0004-6361/200811234 , https://ui.adsabs.harvard.edu/abs/2009A&A...503..137B 503, 137

    2009 doi

  16. [25]

    Breivik K., et al., 2020, @doi [ ] 10.3847/1538-4357/ab9d85 , https://ui.adsabs.harvard.edu/abs/2020ApJ...898...71B 898, 71

    2020 doi

  17. [26]

    M., Eldridge J

    Briel M. M., Eldridge J. J., Stanway E. R., Stevance H. F., Chrimes A. A., 2022, @doi [ ] 10.1093/mnras/stac1100 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.514.1315B 514, 1315

    2022 doi

  18. [27]

    Bufano F., et al., 2014, @doi [ ] 10.1093/mnras/stu065 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.439.1807B 439, 1807

    2014 doi

  19. [28]

    Burrows A., Radice D., Vartanyan D., 2019, @doi [ ] 10.1093/mnras/stz543 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.485.3153B 485, 3153

    2019 doi

  20. [29]

    Burrows A., Wang T., Vartanyan D., 2025, @doi [ ] 10.3847/1538-4357/addd04 , https://ui.adsabs.harvard.edu/abs/2025ApJ...987..164B 987, 164

    2025 doi

  21. [30]

    Cano Z., 2013, @doi [ ] 10.1093/mnras/stt1048 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.434.1098C 434, 1098

    2013 doi

  22. [31]

    Cappellaro E., Evans R., Turatto M., 1999, @doi [ ] 10.48550/arXiv.astro-ph/9904225 , https://ui.adsabs.harvard.edu/abs/1999A&A...351..459C 351, 459

    1999 doi arXiv

  23. [32]

    I., Abbott D

    Castor J. I., Abbott D. C., Klein R. I., 1975, @doi [ ] 10.1086/153315 , https://ui.adsabs.harvard.edu/abs/1975ApJ...195..157C 195, 157

    1975 doi

  24. [33]

    Chan C., M \"u ller B., Heger A., Pakmor R., Springel V., 2018, @doi [ ] 10.3847/2041-8213/aaa28c , https://ui.adsabs.harvard.edu/abs/2018ApJ...852L..19C 852, L19

    2018 doi

  25. [34]

    Chan C., M \"u ller B., Heger A., 2020, @doi [ ] 10.1093/mnras/staa1431 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.495.3751C 495, 3751

    2020 doi

  26. [35]

    J., Goldberg J

    Cheng S. J., Goldberg J. A., Cantiello M., Bauer E. B., Renzo M., Conroy C., 2024, @doi [ ] 10.3847/1538-4357/ad701e , https://ui.adsabs.harvard.edu/abs/2024ApJ...974..270C 974, 270

    2024 doi

  27. [36]

    D., 2016, @doi [ ] 10.3847/0004-637X/823/2/102 , https://ui.adsabs.harvard.edu/abs/2016ApJ...823..102C 823, 102

    Choi J., Dotter A., Conroy C., Cantiello M., Paxton B., Johnson B. D., 2016, @doi [ ] 10.3847/0004-637X/823/2/102 , https://ui.adsabs.harvard.edu/abs/2016ApJ...823..102C 823, 102

    2016 doi

  28. [37]

    De Donder E., Vanbeveren D., 1998, , https://ui.adsabs.harvard.edu/abs/1998A&A...333..557D 333, 557

    1998

  29. [38]

    arXiv:2410.14778

    De K., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2410.14778 , https://ui.adsabs.harvard.edu/abs/2024arXiv241014778D p. arXiv:2410.14778

    2024 doi

  30. [39]

    Decin L., Richards A. M. S., Marchant P., Sana H., 2024, @doi [ ] 10.1051/0004-6361/202244635 , https://ui.adsabs.harvard.edu/abs/2024A&A...681A..17D 681, A17

    2024 doi

  31. [41]

    Dessart L., Yoon S.-C., Livne E., Waldman R., 2018, @doi [ ] 10.1051/0004-6361/201732363 , https://ui.adsabs.harvard.edu/abs/2018A&A...612A..61D 612, A61

    2018 doi

  32. [42]

    R., Langer N., 2020, @doi [ ] 10.1051/0004-6361/202038763 , https://ui.adsabs.harvard.edu/abs/2020A&A...642A.106D 642, A106

    Dessart L., Yoon S.-C., Aguilera-Dena D. R., Langer N., 2020, @doi [ ] 10.1051/0004-6361/202038763 , https://ui.adsabs.harvard.edu/abs/2020A&A...642A.106D 642, A106

    2020 doi

  33. [43]

    Dewi J. D. M., Tauris T. M., 2000, @doi [ ] 10.48550/arXiv.astro-ph/0007034 , https://ui.adsabs.harvard.edu/abs/2000A&A...360.1043D 360, 1043

    2000 doi arXiv

  34. [44]

    A., Kewley L

    Dopita M. A., Kewley L. J., Sutherland R. S., Nicholls D. C., 2016, @doi [ ] 10.1007/s10509-016-2657-8 , https://ui.adsabs.harvard.edu/abs/2016Ap&SS.361...61D 361, 61

    2016 doi

  35. [45]

    R., et al., 2011, @doi [ ] 10.1088/0004-637X/741/2/97 , https://ui.adsabs.harvard.edu/abs/2011ApJ...741...97D 741, 97

    Drout M. R., et al., 2011, @doi [ ] 10.1088/0004-637X/741/2/97 , https://ui.adsabs.harvard.edu/abs/2011ApJ...741...97D 741, 97

    2011 doi

  36. [46]

    R., G \"o tberg Y., Ludwig B

    Drout M. R., G \"o tberg Y., Ludwig B. A., Groh J. H., de Mink S. E., O'Grady A. J. G., Smith N., 2023, @doi [Science] 10.1126/science.ade4970 , https://ui.adsabs.harvard.edu/abs/2023Sci...382.1287D 382, 1287

    2023 doi

  37. [47]

    E., 2024, @doi [ ] 10.3847/1538-4357/ad284e , https://ui.adsabs.harvard.edu/abs/2024ApJ...964...56D 964, 56

    DuPont M., MacFadyen A., de Mink S. E., 2024, @doi [ ] 10.3847/1538-4357/ad284e , https://ui.adsabs.harvard.edu/abs/2024ApJ...964...56D 964, 56

    2024 doi

  38. [48]

    R., et al., 2015, @doi [ ] 10.1051/0004-6361/201526192 , https://ui.adsabs.harvard.edu/abs/2015A&A...580A..93D 580, A93

    Dunstall P. R., et al., 2015, @doi [ ] 10.1051/0004-6361/201526192 , https://ui.adsabs.harvard.edu/abs/2015A&A...580A..93D 580, A93

    2015 doi

  39. [49]

    o hlich C., Hempel M., Perego A., Liebend \

    Ebinger K., Curtis S., Fr \"o hlich C., Hempel M., Perego A., Liebend \"o rfer M., Thielemann F.-K., 2019, @doi [ ] 10.3847/1538-4357/aae7c9 , https://ui.adsabs.harvard.edu/abs/2019ApJ...870....1E 870, 1

    2019 doi

  40. [50]

    J., Stanway E

    Eldridge J. J., Stanway E. R., 2016, @doi [ ] 10.1093/mnras/stw1772 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.462.3302E 462, 3302

    2016 doi

  41. [51]

    J., Fraser M., Smartt S

    Eldridge J. J., Fraser M., Smartt S. J., Maund J. R., Crockett R. M., 2013, @doi [ ] 10.1093/mnras/stt1612 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.436..774E 436, 774

    2013 doi

  42. [52]

    J., Fraser M., Maund J

    Eldridge J. J., Fraser M., Maund J. R., Smartt S. J., 2015, @doi [ ] 10.1093/mnras/stu2197 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.446.2689E 446, 2689

    2015 doi

  43. [53]

    J., Stanway E

    Eldridge J. J., Stanway E. R., Xiao L., McClelland L. A. S., Taylor G., Ng M., Greis S. M. L., Bray J. C., 2017, @doi [ ] 10.1017/pasa.2017.51 , https://ui.adsabs.harvard.edu/abs/2017PASA...34...58E 34, e058

    2017 doi

  44. [54]

    Ercolino A., Jin H., Langer N., Dessart L., 2024, @doi [ ] 10.1051/0004-6361/202347646 , https://ui.adsabs.harvard.edu/abs/2024A&A...685A..58E 685, A58

    2024 doi

  45. [55]

    T., Woosley S

    Ertl T., Janka H. T., Woosley S. E., Sukhbold T., Ugliano M., 2016, @doi [ ] 10.3847/0004-637X/818/2/124 , https://ui.adsabs.harvard.edu/abs/2016ApJ...818..124E 818, 124

    2016 doi

  46. [56]

    E., Sukhbold T., Janka H

    Ertl T., Woosley S. E., Sukhbold T., Janka H. T., 2020, @doi [ ] 10.3847/1538-4357/ab6458 , https://ui.adsabs.harvard.edu/abs/2020ApJ...890...51E 890, 51

    2020 doi

  47. [57]

    V., 1997, @doi [ ] 10.1146/annurev.astro.35.1.309 , https://ui.adsabs.harvard.edu/abs/1997ARA&A..35..309F 35, 309

    Filippenko A. V., 1997, @doi [ ] 10.1146/annurev.astro.35.1.309 , https://ui.adsabs.harvard.edu/abs/1997ARA&A..35..309F 35, 309

    1997 doi

  48. [58]

    Folatelli G., et al., 2014, @doi [ ] 10.1088/2041-8205/793/2/L22 , https://ui.adsabs.harvard.edu/abs/2014ApJ...793L..22F 793, L22

    2014 doi

  49. [59]

    C., Kuncarayakti H., Benvenuto O

    Folatelli G., Bersten M. C., Kuncarayakti H., Benvenuto O. G., Maeda K., Nomoto K., 2015, @doi [ ] 10.1088/0004-637X/811/2/147 , https://ui.adsabs.harvard.edu/abs/2015ApJ...811..147F 811, 147

    2015 doi

  50. [60]

    Folatelli G., et al., 2016, @doi [ ] 10.3847/2041-8205/825/2/L22 , https://ui.adsabs.harvard.edu/abs/2016ApJ...825L..22F 825, L22

    2016 doi

  51. [61]

    J., Ramirez-Ruiz E., Meynet G., Kalogera V., Taam R

    Fragos T., Andrews J. J., Ramirez-Ruiz E., Meynet G., Kalogera V., Taam R. E., Zezas A., 2019, @doi [ ] 10.3847/2041-8213/ab40d1 , https://ui.adsabs.harvard.edu/abs/2019ApJ...883L..45F 883, L45

    2019 doi

  52. [62]

    Fragos T., et al., 2023, @doi [ ] 10.3847/1538-4365/ac90c1 , https://ui.adsabs.harvard.edu/abs/2023ApJS..264...45F 264, 45

    2023 doi

  53. [63]

    Fremling C., et al., 2014, @doi [ ] 10.1051/0004-6361/201423884 , https://ui.adsabs.harvard.edu/abs/2014A&A...565A.114F 565, A114

    2014 doi

  54. [64]

    Fremling C., et al., 2019, @doi [ ] 10.3847/2041-8213/ab218f , https://ui.adsabs.harvard.edu/abs/2019ApJ...878L...5F 878, L5

    2019 doi

  55. [65]

    L., Belczynski K., Wiktorowicz G., Dominik M., Kalogera V., Holz D

    Fryer C. L., Belczynski K., Wiktorowicz G., Dominik M., Kalogera V., Holz D. E., 2012, @doi [ ] 10.1088/0004-637X/749/1/91 , https://ui.adsabs.harvard.edu/abs/2012ApJ...749...91F 749, 91

    2012 doi

  56. [66]

    Gal-Yam A., et al., 2022, @doi [ ] 10.1038/s41586-021-04155-1 , https://ui.adsabs.harvard.edu/abs/2022Natur.601..201G 601, 201

    2022 doi

  57. [67]

    Galbany L., et al., 2014, @doi [ ] 10.1051/0004-6361/201424717 , https://ui.adsabs.harvard.edu/abs/2014A&A...572A..38G 572, A38

    2014 doi

  58. [69]

    Galbany L., et al., 2016b, @doi [ ] 10.1051/0004-6361/201528045 , https://ui.adsabs.harvard.edu/abs/2016A&A...591A..48G 591, A48

    doi

  59. [70]

    R., Kochanek C

    Gerke J. R., Kochanek C. S., Stanek K. Z., 2015, @doi [ ] 10.1093/mnras/stv776 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.450.3289G 450, 3289

    2015 doi

  60. [71]

    Giacobbo N., Mapelli M., 2019, @doi [ ] 10.1093/mnras/sty2848 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.482.2234G 482, 2234

    2019 doi

  61. [72]

    Gilkis A., Arcavi I., 2022, @doi [ ] 10.1093/mnras/stac088 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.511..691G 511, 691

    2022 doi

  62. [73]

    Gilkis A., Soker N., Papish O., 2016, @doi [ ] 10.3847/0004-637X/826/2/178 , https://ui.adsabs.harvard.edu/abs/2016ApJ...826..178G 826, 178

    2016 doi

  63. [74]

    S., Eldridge J

    Gilkis A., Vink J. S., Eldridge J. J., Tout C. A., 2019, @doi [ ] 10.1093/mnras/stz1134 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.486.4451G 486, 4451

    2019 doi

  64. [75]

    Gilkis A., Laplace E., Arcavi I., Shenar T., Schneider F. R. N., 2025, @doi [ ] 10.1093/mnras/staf884 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.540.3094G 540, 3094

    2025 doi

  65. [76]

    R., 2013, @doi [ ] 10.1093/mnras/stt1268 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.434.3497G 434, 3497

    Glebbeek E., Gaburov E., Portegies Zwart S., Pols O. R., 2013, @doi [ ] 10.1093/mnras/stt1268 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.434.3497G 434, 3497

    2013 doi

  66. [77]

    R., et al., 2017, @doi [ ] 10.1093/mnras/stw2708 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.465..403G 465, 403

    Goldman S. R., et al., 2017, @doi [ ] 10.1093/mnras/stw2708 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.465..403G 465, 403

    2017 doi

  67. [78]

    E., Groh J

    G \"o tberg Y., de Mink S. E., Groh J. H., 2017, @doi [ ] 10.1051/0004-6361/201730472 , https://ui.adsabs.harvard.edu/abs/2017A&A...608A..11G 608, A11

    2017 doi

  68. [79]

    G \"o tberg Y., et al., 2023, @doi [ ] 10.3847/1538-4357/ace5a3 , https://ui.adsabs.harvard.edu/abs/2023ApJ...959..125G 959, 125

    2023 doi

  69. [80]

    B., Huang S., Modjaz M., Shivvers I., Filippenko A

    Graur O., Bianco F. B., Huang S., Modjaz M., Shivvers I., Filippenko A. V., Li W., Eldridge J. J., 2017a, @doi [ ] 10.3847/1538-4357/aa5eb8 , https://ui.adsabs.harvard.edu/abs/2017ApJ...837..120G 837, 120

    doi

  70. [81]

    B., Modjaz M., Shivvers I., Filippenko A

    Graur O., Bianco F. B., Modjaz M., Shivvers I., Filippenko A. V., Li W., Smith N., 2017b, @doi [ ] 10.3847/1538-4357/aa5eb7 , https://ui.adsabs.harvard.edu/abs/2017ApJ...837..121G 837, 121

    doi

  71. [82]

    Groenewegen M. A. T., 2012, @doi [ ] 10.1051/0004-6361/201118287 , https://ui.adsabs.harvard.edu/abs/2012A&A...540A..32G 540, A32

    2012 doi

  72. [83]

    A., Taubenberger S., Hillebrandt W., Nomoto K., Sauer D

    Hachinger S., Mazzali P. A., Taubenberger S., Hillebrandt W., Nomoto K., Sauer D. N., 2012, @doi [ ] 10.1111/j.1365-2966.2012.20464.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.422...70H 422, 70

    2012

  73. [84]

    R., Lyne A

    Hobbs G., Lorimer D. R., Lyne A. G., Kramer M., 2005, @doi [ ] 10.1111/j.1365-2966.2005.09087.x , https://ui.adsabs.harvard.edu/abs/2005MNRAS.360..974H 360, 974

    2005

  74. [85]

    C., Fransson C., 1996, @doi [ ] 10.1086/176699 , https://ui.adsabs.harvard.edu/abs/1996ApJ...456..811H 456, 811

    Houck J. C., Fransson C., 1996, @doi [ ] 10.1086/176699 , https://ui.adsabs.harvard.edu/abs/1996ApJ...456..811H 456, 811

    1996 doi

  75. [86]

    M., Davidson K., 1979, @doi [ ] 10.1086/157301 , https://ui.adsabs.harvard.edu/abs/1979ApJ...232..409H 232, 409

    Humphreys R. M., Davidson K., 1979, @doi [ ] 10.1086/157301 , https://ui.adsabs.harvard.edu/abs/1979ApJ...232..409H 232, 409

    1979 doi

  76. [88]

    Ivanova N., 2011, @doi [ ] 10.1088/0004-637X/730/2/76 , https://ui.adsabs.harvard.edu/abs/2011ApJ...730...76I 730, 76

    2011 doi

  77. [89]

    Ivanova N., Podsiadlowski P., Spruit H., 2002, @doi [ ] 10.1046/j.1365-8711.2002.05543.x , https://ui.adsabs.harvard.edu/abs/2002MNRAS.334..819I 334, 819

    2002

  78. [90]

    Ivanova N., et al., 2013, @doi [ ] 10.1007/s00159-013-0059-2 , https://ui.adsabs.harvard.edu/abs/2013A&ARv..21...59I 21, 59

    2013 doi

  79. [91]

    G., Tout C

    Izzard R. G., Tout C. A., Karakas A. I., Pols O. R., 2004, @doi [ ] 10.1111/j.1365-2966.2004.07446.x , https://ui.adsabs.harvard.edu/abs/2004MNRAS.350..407I 350, 407

    2004

  80. [92]

    G., Dray L

    Izzard R. G., Dray L. M., Karakas A. I., Lugaro M., Tout C. A., 2006, @doi [ ] 10.1051/0004-6361:20066129 , https://ui.adsabs.harvard.edu/abs/2006A&A...460..565I 460, 565

    2006 doi

  81. [93]

    A., Anderson J

    James P. A., Anderson J. P., 2006, @doi [ ] 10.1051/0004-6361:20054509 , https://ui.adsabs.harvard.edu/abs/2006A&A...453...57J 453, 57

    2006 doi

  82. [94]

    Janka H.-T., 2012, @doi [Annual Review of Nuclear and Particle Science] 10.1146/annurev-nucl-102711-094901 , https://ui.adsabs.harvard.edu/abs/2012ARNPS..62..407J 62, 407

    2012 doi

  83. [95]

    S., et al., 2023, @doi [ ] 10.3847/1538-4365/acae8d , https://ui.adsabs.harvard.edu/abs/2023ApJS..265...15J 265, 15

    Jermyn A. S., et al., 2023, @doi [ ] 10.3847/1538-4365/acae8d , https://ui.adsabs.harvard.edu/abs/2023ApJS..265...15J 265, 15

    2023 doi

  84. [96]

    Josiek J., Ekstr \"o m S., Sander A. A. C., 2024, @doi [ ] 10.1051/0004-6361/202449281 , https://ui.adsabs.harvard.edu/abs/2024A&A...688A..71J 688, A71

    2024 doi

  85. [97]

    Kangas T., et al., 2017, @doi [ ] 10.1051/0004-6361/201628705 , https://ui.adsabs.harvard.edu/abs/2017A&A...597A..92K 597, A92

    2017 doi

  86. [98]

    D., Sundqvist J

    Kee N. D., Sundqvist J. O., Decin L., de Koter A., Sana H., 2021, @doi [ ] 10.1051/0004-6361/202039224 , https://ui.adsabs.harvard.edu/abs/2021A&A...646A.180K 646, A180

    2021 doi

  87. [99]

    L., Kirshner R

    Kelly P. L., Kirshner R. P., 2012, @doi [ ] 10.1088/0004-637X/759/2/107 , https://ui.adsabs.harvard.edu/abs/2012ApJ...759..107K 759, 107

    2012 doi

  88. [100]

    D., et al., 2017, @doi [ ] 10.1093/mnras/stw3082 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.465.4650K 465, 4650

    Kilpatrick C. D., et al., 2017, @doi [ ] 10.1093/mnras/stw3082 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.465.4650K 465, 4650

    2017 doi

  89. [101]

    D., et al., 2021, @doi [ ] 10.1093/mnras/stab838 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.504.2073K 504, 2073

    Kilpatrick C. D., et al., 2021, @doi [ ] 10.1093/mnras/stab838 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.504.2073K 504, 2073

    2021 doi

  90. [102]

    G., Pols O., 2020, @doi [ ] 10.1051/0004-6361/202037694 , https://ui.adsabs.harvard.edu/abs/2020A&A...638A..55K 638, A55

    Klencki J., Nelemans G., Istrate A. G., Pols O., 2020, @doi [ ] 10.1051/0004-6361/202037694 , https://ui.adsabs.harvard.edu/abs/2020A&A...638A..55K 638, A55

    2020 doi

  91. [103]

    Klencki J., Istrate A., Nelemans G., Pols O., 2022, @doi [ ] 10.1051/0004-6361/202142701 , https://ui.adsabs.harvard.edu/abs/2022A&A...662A..56K 662, A56

    2022 doi

  92. [104]

    Ko T., Kinugawa T., Tsuna D., Hirai R., Takei Y., 2025, @doi [ ] 10.1093/mnras/staf1241 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.tmp.1187K

    2025 doi

  93. [105]

    A., et al., 2014, @doi [ ] 10.1088/0067-0049/213/2/34 , https://ui.adsabs.harvard.edu/abs/2014ApJS..213...34K 213, 34

    Kobulnicky H. A., et al., 2014, @doi [ ] 10.1088/0067-0049/213/2/34 , https://ui.adsabs.harvard.edu/abs/2014ApJS..213...34K 213, 34

    2014 doi

  94. [106]

    S., et al., 2017, @doi [ ] 10.1088/1538-3873/aa80d9 , https://ui.adsabs.harvard.edu/abs/2017PASP..129j4502K 129, 104502

    Kochanek C. S., et al., 2017, @doi [ ] 10.1088/1538-3873/aa80d9 , https://ui.adsabs.harvard.edu/abs/2017PASP..129j4502K 129, 104502

    2017 doi

  95. [107]

    Kroupa P., 2001, @doi [ ] 10.1046/j.1365-8711.2001.04022.x , https://ui.adsabs.harvard.edu/abs/2001MNRAS.322..231K 322, 231

    2001

  96. [108]

    U., et al., 2024, @doi [ ] 10.1051/0004-6361/202452356 , https://ui.adsabs.harvard.edu/abs/2024A&A...692A.141K 692, A141

    Kruckow M. U., et al., 2024, @doi [ ] 10.1051/0004-6361/202452356 , https://ui.adsabs.harvard.edu/abs/2024A&A...692A.141K 692, A141

    2024 doi

  97. [109]

    Kuncarayakti H., et al., 2018, @doi [ ] 10.1051/0004-6361/201731923 , https://ui.adsabs.harvard.edu/abs/2018A&A...613A..35K 613, A35

    2018 doi

  98. [110]

    Kuroda T., Kotake K., Takiwaki T., Thielemann F.-K., 2018, @doi [ ] 10.1093/mnrasl/sly059 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.477L..80K 477, L80

    2018 doi

  99. [111]

    M., Renzo M., Rau S., Vigna-G \'o mez A., 2025, @doi [ ] 10.3847/1538-4357/ad9d3c , https://ui.adsabs.harvard.edu/abs/2025ApJ...979...57L 979, 57

    Landri C., Ricker P. M., Renzo M., Rau S., Vigna-G \'o mez A., 2025, @doi [ ] 10.3847/1538-4357/ad9d3c , https://ui.adsabs.harvard.edu/abs/2025ApJ...979...57L 979, 57

    2025 doi

  100. [112]

    Langer N., 1998, , https://ui.adsabs.harvard.edu/abs/1998A&A...329..551L 329, 551

    1998

  101. [113]

    E., Justham S., Farmer R., 2020, @doi [ ] 10.1051/0004-6361/201937300 , https://ui.adsabs.harvard.edu/abs/2020A&A...637A...6L 637, A6

    Laplace E., G \"o tberg Y., de Mink S. E., Justham S., Farmer R., 2020, @doi [ ] 10.1051/0004-6361/201937300 , https://ui.adsabs.harvard.edu/abs/2020A&A...637A...6L 637, A6

    2020 doi

  102. [114]

    E., 2021, @doi [ ] 10.1051/0004-6361/202140506 , https://ui.adsabs.harvard.edu/abs/2021A&A...656A..58L 656, A58

    Laplace E., Justham S., Renzo M., G \"o tberg Y., Farmer R., Vartanyan D., de Mink S. E., 2021, @doi [ ] 10.1051/0004-6361/202140506 , https://ui.adsabs.harvard.edu/abs/2021A&A...656A..58L 656, A58

    2021 doi

  103. [115]

    Leloudas G., et al., 2011, @doi [ ] 10.1051/0004-6361/201116692 , https://ui.adsabs.harvard.edu/abs/2011A&A...530A..95L 530, A95

    2011 doi

  104. [117]

    Livio M., Soker N., 1988, @doi [ ] 10.1086/166419 , https://ui.adsabs.harvard.edu/abs/1988ApJ...329..764L 329, 764

    1988 doi

  105. [118]

    Lombardi Jr. J. C., Warren J. S., Rasio F. A., Sills A., Warren A. R., 2002, @doi [ ] 10.1086/339060 , https://ui.adsabs.harvard.edu/abs/2002ApJ...568..939L 568, 939

    2002 doi

  106. [119]

    D., Bersier D., James P

    Lyman J. D., Bersier D., James P. A., Mazzali P. A., Eldridge J. J., Fraser M., Pian E., 2016, @doi [ ] 10.1093/mnras/stv2983 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.457..328L 457, 328

    2016 doi

  107. [120]

    Ma X., et al., 2025, @doi [ ] 10.1051/0004-6361/202452684 , https://ui.adsabs.harvard.edu/abs/2025A&A...698A.305M 698, A305

    2025 doi

  108. [121]

    I., Woosley S

    MacFadyen A. I., Woosley S. E., 1999, @doi [ ] 10.1086/307790 , https://ui.adsabs.harvard.edu/abs/1999ApJ...524..262M 524, 262

    1999 doi

  109. [122]

    J., 2022, @doi [ ] 10.3847/1538-4357/ac4672 , https://ui.adsabs.harvard.edu/abs/2022ApJ...927...25M 927, 25

    Maeda K., Moriya T. J., 2022, @doi [ ] 10.3847/1538-4357/ac4672 , https://ui.adsabs.harvard.edu/abs/2022ApJ...927...25M 927, 25

    2022 doi

  110. [123]

    Maeda K., et al., 2015, @doi [ ] 10.1088/0004-637X/807/1/35 , https://ui.adsabs.harvard.edu/abs/2015ApJ...807...35M 807, 35

    2015 doi

  111. [124]

    Mandel I., M \"u ller B., 2020, @doi [ ] 10.1093/mnras/staa3043 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.499.3214M 499, 3214

    2020 doi

  112. [125]

    M., Moriya T

    Marchant P., Langer N., Podsiadlowski P., Tauris T. M., Moriya T. J., 2016, @doi [ ] 10.1051/0004-6361/201628133 , https://ui.adsabs.harvard.edu/abs/2016A&A...588A..50M 588, A50

    2016 doi

  113. [126]

    Marchant P., Pappas K. M. W., Gallegos-Garcia M., Berry C. P. L., Taam R. E., Kalogera V., Podsiadlowski P., 2021, @doi [ ] 10.1051/0004-6361/202039992 , https://ui.adsabs.harvard.edu/abs/2021A&A...650A.107M 650, A107

    2021 doi

  114. [127]

    A., et al., 2013, @doi [ ] 10.1051/0004-6361/201321956 , https://ui.adsabs.harvard.edu/abs/2013A&A...559A.114M 559, A114

    Marino R. A., et al., 2013, @doi [ ] 10.1051/0004-6361/201321956 , https://ui.adsabs.harvard.edu/abs/2013A&A...559A.114M 559, A114

    2013 doi

  115. [128]

    C., et al., 2015, @doi [ ] 10.1093/mnras/stv1944 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.453.4467M 453, 4467

    Mauerhan J. C., et al., 2015, @doi [ ] 10.1093/mnras/stv1944 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.453.4467M 453, 4467

    2015 doi

  116. [129]

    R., Smartt S

    Maund J. R., Smartt S. J., Kudritzki R. P., Podsiadlowski P., Gilmore G. F., 2004, @doi [ ] 10.1038/nature02161 , https://ui.adsabs.harvard.edu/abs/2004Natur.427..129M 427, 129

    2004 doi

  117. [130]

    Meynet G., et al., 2015, @doi [ ] 10.1051/0004-6361/201424671 , https://ui.adsabs.harvard.edu/abs/2015A&A...575A..60M 575, A60

    2015 doi

  118. [131]

    Moe M., Di Stefano R., 2017, @doi [ ] 10.3847/1538-4365/aa6fb6 , https://ui.adsabs.harvard.edu/abs/2017ApJS..230...15M 230, 15

    2017 doi

  119. [132]

    Morales-Garoffolo A., et al., 2014, @doi [ ] 10.1093/mnras/stu1837 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.445.1647M 445, 1647

    2014 doi

  120. [133]

    Morales-Garoffolo A., et al., 2015, @doi [ ] 10.1093/mnras/stv1972 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.454...95M 454, 95

    2015 doi

  121. [134]

    Nugis T., Lamers H. J. G. L. M., 2000, , https://ui.adsabs.harvard.edu/abs/2000A&A...360..227N 360, 227

    2000

  122. [135]

    D., 2011, @doi [ ] 10.1088/0004-637X/730/2/70 , https://ui.adsabs.harvard.edu/abs/2011ApJ...730...70O 730, 70

    O'Connor E., Ott C. D., 2011, @doi [ ] 10.1088/0004-637X/730/2/70 , https://ui.adsabs.harvard.edu/abs/2011ApJ...730...70O 730, 70

    2011 doi

  123. [136]

    N., Bahramian A., Miller-Jones J

    O'Doherty T. N., Bahramian A., Miller-Jones J. C. A., Goodwin A. J., Mandel I., Willcox R., Atri P., Strader J., 2023, @doi [ ] 10.1093/mnras/stad680 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.521.2504O 521, 2504

    2023 doi

  124. [137]

    D., Roberts L

    Ott C. D., Roberts L. F., da Silva Schneider A., Fedrow J. M., Haas R., Schnetter E., 2018, @doi [ ] 10.3847/2041-8213/aaa967 , https://ui.adsabs.harvard.edu/abs/2018ApJ...855L...3O 855, L3

    2018 doi

  125. [138]

    P., Gayley K

    Owocki S. P., Gayley K. G., Shaviv N. J., 2004, @doi [ ] 10.1086/424910 , https://ui.adsabs.harvard.edu/abs/2004ApJ...616..525O 616, 525

    2004 doi

  126. [139]

    Packet W., 1981, , https://ui.adsabs.harvard.edu/abs/1981A&A...102...17P 102, 17

    1981

  127. [140]

    Pastorello A., et al., 2007, @doi [ ] 10.1038/nature05825 , https://ui.adsabs.harvard.edu/abs/2007Natur.447..829P 447, 829

    2007 doi

  128. [142]

    Pastorello A., et al., 2008b, @doi [ ] 10.1111/j.1365-2966.2008.13602.x , https://ui.adsabs.harvard.edu/abs/2008MNRAS.389..113P 389, 113

    2008

  129. [143]

    A., Sukhbold T., 2020, @doi [ ] 10.1093/mnras/staa3029 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.499.2803P 499, 2803

    Patton R. A., Sukhbold T., 2020, @doi [ ] 10.1093/mnras/staa3029 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.499.2803P 499, 2803

    2020 doi

  130. [144]

    A., Pinsonneault M

    Patton R. A., Pinsonneault M. H., Thompson T. A., 2025, @doi [ ] 10.3847/1538-4357/addd0f , https://ui.adsabs.harvard.edu/abs/2025ApJ...987..212P 987, 212

    2025 doi

  131. [145]

    Paxton B., Bildsten L., Dotter A., Herwig F., Lesaffre P., Timmes F., 2011, @doi [ ] 10.1088/0067-0049/192/1/3 , https://ui.adsabs.harvard.edu/abs/2011ApJS..192....3P 192, 3

    2011 doi

  132. [146]

    Paxton B., et al., 2013, @doi [ ] 10.1088/0067-0049/208/1/4 , https://ui.adsabs.harvard.edu/abs/2013ApJS..208....4P 208, 4

    2013 doi

  133. [147]

    Paxton B., et al., 2015, @doi [ ] 10.1088/0067-0049/220/1/15 , https://ui.adsabs.harvard.edu/abs/2015ApJS..220...15P 220, 15

    2015 doi

  134. [148]

    Paxton B., et al., 2018, @doi [ ] 10.3847/1538-4365/aaa5a8 , https://ui.adsabs.harvard.edu/abs/2018ApJS..234...34P 234, 34

    2018 doi

  135. [149]

    Paxton B., et al., 2019, @doi [ ] 10.3847/1538-4365/ab2241 , https://ui.adsabs.harvard.edu/abs/2019ApJS..243...10P 243, 10

    2019 doi

  136. [150]

    A., et al., 2020, @doi [ ] 10.3847/1538-4357/abbd98 , https://ui.adsabs.harvard.edu/abs/2020ApJ...904...35P 904, 35

    Perley D. A., et al., 2020, @doi [ ] 10.3847/1538-4357/abbd98 , https://ui.adsabs.harvard.edu/abs/2020ApJ...904...35P 904, 35

    2020 doi

  137. [151]

    Pessi T., et al., 2023, @doi [ ] 10.1051/0004-6361/202346512 , https://ui.adsabs.harvard.edu/abs/2023A&A...677A..28P 677, A28

    2023 doi

  138. [152]

    arXiv:2508.10985

    Pessi T., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2508.10985 , https://ui.adsabs.harvard.edu/abs/2025arXiv250810985P p. arXiv:2508.10985

    2025 doi

  139. [153]

    C., Hsu J

    Podsiadlowski P., Joss P. C., Hsu J. J. L., 1992, @doi [ ] 10.1086/171341 , https://ui.adsabs.harvard.edu/abs/1992ApJ...391..246P 391, 246

    1992 doi

  140. [154]

    Powell J., M \"u ller B., 2020, @doi [ ] 10.1093/mnras/staa1048 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.494.4665P 494, 4665

    2020 doi

  141. [155]

    L., Stanek K

    Prieto J. L., Stanek K. Z., Beacom J. F., 2008, @doi [ ] 10.1086/524654 , https://ui.adsabs.harvard.edu/abs/2008ApJ...673..999P 673, 999

    2008 doi

  142. [156]

    Reilly E., et al., 2016, @doi [ ] 10.1093/mnras/stv3005 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.457..288R 457, 288

    2016 doi

  143. [157]

    pp 229--256

    Reimers D., 1975, Circumstellar envelopes and mass loss of red giant stars . pp 229--256

    1975

  144. [158]

    D., Shore S

    Renzo M., Ott C. D., Shore S. N., de Mink S. E., 2017, @doi [ ] 10.1051/0004-6361/201730698 , https://ui.adsabs.harvard.edu/abs/2017A&A...603A.118R 603, A118

    2017 doi

  145. [159]

    D., Jiang Y

    Renzo M., Cantiello M., Metzger B. D., Jiang Y. F., 2020, @doi [ ] 10.3847/2041-8213/abc6a6 , https://ui.adsabs.harvard.edu/abs/2020ApJ...904L..13R 904, L13

    2020 doi

  146. [160]

    D., 2023, @doi [ ] 10.3847/2041-8213/aca4d3 , https://ui.adsabs.harvard.edu/abs/2023ApJ...942L..32R 942, L32

    Renzo M., Zapartas E., Justham S., Breivik K., Lau M., Farmer R., Cantiello M., Metzger B. D., 2023, @doi [ ] 10.3847/2041-8213/aca4d3 , https://ui.adsabs.harvard.edu/abs/2023ApJ...942L..32R 942, L32

    2023 doi

  147. [161]

    Richardson D., Branch D., Baron E., 2006, @doi [ ] 10.1086/500578 , https://ui.adsabs.harvard.edu/abs/2006AJ....131.2233R 131, 2233

    2006 doi

  148. [162]

    Sana H., et al., 2012, @doi [Science] 10.1126/science.1223344 , https://ui.adsabs.harvard.edu/abs/2012Sci...337..444S 337, 444

    2012 doi

  149. [163]

    Sana H., et al., 2013, @doi [ ] 10.1051/0004-6361/201219621 , https://ui.adsabs.harvard.edu/abs/2013A&A...550A.107S 550, A107

    2013 doi

  150. [164]

    Schneider F. R. N., Ohlmann S. T., Podsiadlowski P., R \"o pke F. K., Balbus S. A., Pakmor R., Springel V., 2019, @doi [ ] 10.1038/s41586-019-1621-5 , https://ui.adsabs.harvard.edu/abs/2019Natur.574..211S 574, 211

    2019 doi

  151. [165]

    Schneider F. R. N., Podsiadlowski P., M \"u ller B., 2021, @doi [ ] 10.1051/0004-6361/202039219 , https://ui.adsabs.harvard.edu/abs/2021A&A...645A...5S 645, A5

    2021 doi

  152. [166]

    J., et al., 2014, @doi [ ] 10.1088/0004-637X/788/1/48 , https://ui.adsabs.harvard.edu/abs/2014ApJ...788...48S 788, 48

    Shappee B. J., et al., 2014, @doi [ ] 10.1088/0004-637X/788/1/48 , https://ui.adsabs.harvard.edu/abs/2014ApJ...788...48S 788, 48

    2014 doi

  153. [167]

    Shivvers I., et al., 2017, @doi [ ] 10.1088/1538-3873/aa54a6 , https://ui.adsabs.harvard.edu/abs/2017PASP..129e4201S 129, 054201

    2017 doi

  154. [168]

    J., 2009, @doi [ ] 10.1146/annurev-astro-082708-101737 , https://ui.adsabs.harvard.edu/abs/2009ARA&A..47...63S 47, 63

    Smartt S. J., 2009, @doi [ ] 10.1146/annurev-astro-082708-101737 , https://ui.adsabs.harvard.edu/abs/2009ARA&A..47...63S 47, 63

    2009 doi

  155. [169]

    J., 2015, @doi [ ] 10.1017/pasa.2015.17 , https://ui.adsabs.harvard.edu/abs/2015PASA...32...16S 32, e016

    Smartt S. J., 2015, @doi [ ] 10.1017/pasa.2015.17 , https://ui.adsabs.harvard.edu/abs/2015PASA...32...16S 32, e016

    2015 doi

  156. [170]

    J., Eldridge J

    Smartt S. J., Eldridge J. J., Crockett R. M., Maund J. R., 2009, @doi [ ] 10.1111/j.1365-2966.2009.14506.x , https://ui.adsabs.harvard.edu/abs/2009MNRAS.395.1409S 395, 1409

    2009

  157. [171]

    Smith N., 2014, @doi [ ] 10.1146/annurev-astro-081913-040025 , https://ui.adsabs.harvard.edu/abs/2014ARA&A..52..487S 52, 487

    2014 doi

  158. [172]

    P., 2006, @doi [ ] 10.1086/506523 , https://ui.adsabs.harvard.edu/abs/2006ApJ...645L..45S 645, L45

    Smith N., Owocki S. P., 2006, @doi [ ] 10.1086/506523 , https://ui.adsabs.harvard.edu/abs/2006ApJ...645L..45S 645, L45

    2006 doi

  159. [173]

    V., Chornock R., 2011, @doi [ ] 10.1111/j.1365-2966.2011.17229.x , https://ui.adsabs.harvard.edu/abs/2011MNRAS.412.1522S 412, 1522

    Smith N., Li W., Filippenko A. V., Chornock R., 2011, @doi [ ] 10.1111/j.1365-2966.2011.17229.x , https://ui.adsabs.harvard.edu/abs/2011MNRAS.412.1522S 412, 1522

    2011

  160. [174]

    Soker N., 2019, @doi [Research in Astronomy and Astrophysics] 10.1088/1674-4527/19/7/95 , https://ui.adsabs.harvard.edu/abs/2019RAA....19...95S 19, 095

    2019 doi

  161. [175]

    Solar M., et al., 2024, @doi [Nature Communications] 10.1038/s41467-024-51863-z , https://ui.adsabs.harvard.edu/abs/2024NatCo..15.7667S 15, 7667

    2024 doi

  162. [176]

    Spera M., Mapelli M., Bressan A., 2015, @doi [ ] 10.1093/mnras/stv1161 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.451.4086S 451, 4086

    2015 doi

  163. [177]

    A., Bressan A., Costa G., 2019, @doi [ ] 10.1093/mnras/stz359 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.485..889S 485, 889

    Spera M., Mapelli M., Giacobbo N., Trani A. A., Bressan A., Costa G., 2019, @doi [ ] 10.1093/mnras/stz359 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.485..889S 485, 889

    2019 doi

  164. [178]

    Sravan N., Marchant P., Kalogera V., 2019, @doi [ ] 10.3847/1538-4357/ab4ad7 , https://ui.adsabs.harvard.edu/abs/2019ApJ...885..130S 885, 130

    2019 doi

  165. [179]

    R., Eldridge J

    Stanway E. R., Eldridge J. J., 2018, @doi [ ] 10.1093/mnras/sty1353 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.479...75S 479, 75

    2018 doi

  166. [180]

    R., Eldridge J

    Stanway E. R., Eldridge J. J., Becker G. D., 2016, @doi [ ] 10.1093/mnras/stv2661 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.456..485S 456, 485

    2016 doi

  167. [181]

    W., Neijssel C

    Stevenson S., Vigna-G \'o mez A., Mandel I., Barrett J. W., Neijssel C. J., Perkins D., de Mink S. E., 2017, @doi [Nature Communications] 10.1038/ncomms14906 , https://ui.adsabs.harvard.edu/abs/2017NatCo...814906S 8, 14906

    2017 doi

  168. [182]

    E., Brown J

    Sukhbold T., Ertl T., Woosley S. E., Brown J. M., Janka H. T., 2016, @doi [ ] 10.3847/0004-637X/821/1/38 , https://ui.adsabs.harvard.edu/abs/2016ApJ...821...38S 821, 38

    2016 doi

  169. [183]

    R., Crowther P

    Sun N.-C., Maund J. R., Crowther P. A., 2023, @doi [ ] 10.1093/mnras/stad690 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.521.2860S 521, 2860

    2023 doi

  170. [184]

    Taddia F., et al., 2015, @doi [ ] 10.1051/0004-6361/201423915 , https://ui.adsabs.harvard.edu/abs/2015A&A...574A..60T 574, A60

    2015 doi

  171. [185]

    Taddia F., et al., 2018, @doi [ ] 10.1051/0004-6361/201730844 , https://ui.adsabs.harvard.edu/abs/2018A&A...609A.136T 609, A136

    2018 doi

  172. [186]

    M., Langer N., Podsiadlowski P., 2015, @doi [ ] 10.1093/mnras/stv990 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.451.2123T 451, 2123

    Tauris T. M., Langer N., Podsiadlowski P., 2015, @doi [ ] 10.1093/mnras/stv990 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.451.2123T 451, 2123

    2015 doi

  173. [187]

    Tramper F., et al., 2015, @doi [ ] 10.1051/0004-6361/201425390 , https://ui.adsabs.harvard.edu/abs/2015A&A...581A.110T 581, A110

    2015 doi

  174. [188]

    D., de Mink S

    Van Dyk S. D., de Mink S. E., Zapartas E., 2016, @doi [ ] 10.3847/0004-637X/818/1/75 , https://ui.adsabs.harvard.edu/abs/2016ApJ...818...75V 818, 75

    2016 doi

  175. [189]

    Vartanyan D., Burrows A., Radice D., 2019, @doi [ ] 10.1093/mnras/stz2307 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.489.2227V 489, 2227

    2019 doi

  176. [190]

    E., 2021, @doi [ ] 10.3847/2041-8213/ac0b42 , https://ui.adsabs.harvard.edu/abs/2021ApJ...916L...5V 916, L5

    Vartanyan D., Laplace E., Renzo M., G \"o tberg Y., Burrows A., de Mink S. E., 2021, @doi [ ] 10.3847/2041-8213/ac0b42 , https://ui.adsabs.harvard.edu/abs/2021ApJ...916L...5V 916, L5

    2021 doi

  177. [191]

    Vigna-G \'o mez A., et al., 2018, @doi [ ] 10.1093/mnras/sty2463 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.481.4009V 481, 4009

    2018 doi

  178. [192]

    I., et al., 2021, @doi [ ] 10.1093/mnras/stab2197 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.507.5348V 507, 5348

    Villase \ n or J. I., et al., 2021, @doi [ ] 10.1093/mnras/stab2197 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.507.5348V 507, 5348

    2021 doi

  179. [193]

    I., et al., 2025, @doi [ ] 10.1051/0004-6361/202453166 , https://ui.adsabs.harvard.edu/abs/2025A&A...698A..41V 698, A41

    Villase \ n or J. I., et al., 2025, @doi [ ] 10.1051/0004-6361/202453166 , https://ui.adsabs.harvard.edu/abs/2025A&A...698A..41V 698, A41

    2025 doi

  180. [194]

    S., 2017, @doi [ ] 10.1051/0004-6361/201731902 , https://ui.adsabs.harvard.edu/abs/2017A&A...607L...8V 607, L8

    Vink J. S., 2017, @doi [ ] 10.1051/0004-6361/201731902 , https://ui.adsabs.harvard.edu/abs/2017A&A...607L...8V 607, L8

    2017 doi

  181. [195]

    S., de Koter A., Lamers H

    Vink J. S., de Koter A., Lamers H. J. G. L. M., 2000, @doi [ ] 10.48550/arXiv.astro-ph/0008183 , https://ui.adsabs.harvard.edu/abs/2000A&A...362..295V 362, 295

    2000 doi arXiv

  182. [196]

    S., de Koter A., Lamers H

    Vink J. S., de Koter A., Lamers H. J. G. L. M., 2001, @doi [ ] 10.1051/0004-6361:20010127 , https://ui.adsabs.harvard.edu/abs/2001A&A...369..574V 369, 574

    2001 doi

  183. [197]

    C., 2008, @doi [ ] 10.1146/annurev.astro.46.060407.145139 , https://ui.adsabs.harvard.edu/abs/2008ARA&A..46..433W 46, 433

    Wang L., Wheeler J. C., 2008, @doi [ ] 10.1146/annurev.astro.46.060407.145139 , https://ui.adsabs.harvard.edu/abs/2008ARA&A..46..433W 46, 433

    2008

  184. [198]

    F., 1984, @doi [ ] 10.1086/161701 , https://ui.adsabs.harvard.edu/abs/1984ApJ...277..355W 277, 355

    Webbink R. F., 1984, @doi [ ] 10.1086/161701 , https://ui.adsabs.harvard.edu/abs/1984ApJ...277..355W 277, 355

    1984 doi

  185. [199]

    Wei D., Schneider F. R. N., Podsiadlowski P., Laplace E., R \"o pke F. K., Vetter M., 2024, @doi [ ] 10.1051/0004-6361/202348560 , https://ui.adsabs.harvard.edu/abs/2024A&A...688A..87W 688, A87

    2024 doi

  186. [200]

    F., Peterson S., Murphy J., Gilbert K., Dalcanton J

    Williams B. F., Peterson S., Murphy J., Gilbert K., Dalcanton J. J., Dolphin A. E., Jennings Z. G., 2014, @doi [ ] 10.1088/0004-637X/791/2/105 , https://ui.adsabs.harvard.edu/abs/2014ApJ...791..105W 791, 105

    2014 doi

  187. [201]

    F., Hillis T

    Williams B. F., Hillis T. J., Murphy J. W., Gilbert K., Dalcanton J. J., Dolphin A. E., 2018, @doi [ ] 10.3847/1538-4357/aaba7d , https://ui.adsabs.harvard.edu/abs/2018ApJ...860...39W 860, 39

    2018 doi

  188. [202]

    E., Eastman R

    Woosley S. E., Eastman R. G., Weaver T. A., Pinto P. A., 1994, @doi [ ] 10.1086/174319 , https://ui.adsabs.harvard.edu/abs/1994ApJ...429..300W 429, 300

    1994 doi

  189. [203]

    E., Langer N., Weaver T

    Woosley S. E., Langer N., Weaver T. A., 1995, @doi [ ] 10.1086/175963 , https://ui.adsabs.harvard.edu/abs/1995ApJ...448..315W 448, 315

    1995 doi

  190. [204]

    C., Fuller J., 2022, @doi [ ] 10.3847/2041-8213/ac9b3d , https://ui.adsabs.harvard.edu/abs/2022ApJ...940L..27W 940, L27

    Wu S. C., Fuller J., 2022, @doi [ ] 10.3847/2041-8213/ac9b3d , https://ui.adsabs.harvard.edu/abs/2022ApJ...940L..27W 940, L27

    2022 doi

  191. [205]

    R., Niu Z., Singleton A

    Xi Q., Sun N.-C., Zhao Y.-H., Maund J. R., Niu Z., Singleton A. J., Liu J., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2412.02667 , https://ui.adsabs.harvard.edu/abs/2024arXiv241202667X p. arXiv:2412.02667

    2024 doi arXiv

  192. [206]

    J., Galbany L., Stanway E., 2019, in Oskinova L

    Xiao L., Eldridge J. J., Galbany L., Stanway E., 2019, in Oskinova L. M., Bozzo E., Bulik T., Gies D. R., eds, IAU Symposium Vol. 346, High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects. pp 342--343, @doi 10.1017/S1743921318008062

    2019 doi

  193. [207]

    D., 2022, @doi [ ] 10.1093/mnras/stac2551 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.516.5816X 516, 5816

    Xin C., Renzo M., Metzger B. D., 2022, @doi [ ] 10.1093/mnras/stac2551 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.516.5816X 516, 5816

    2022 doi

  194. [208]

    Yang M., et al., 2023, @doi [ ] 10.1051/0004-6361/202244770 , https://ui.adsabs.harvard.edu/abs/2023A&A...676A..84Y 676, A84

    2023 doi

  195. [209]

    Yoon S.-C., 2015, @doi [ ] 10.1017/pasa.2015.16 , https://ui.adsabs.harvard.edu/abs/2015PASA...32...15Y 32, e015

    2015 doi

  196. [210]

    C., Woosley S

    Yoon S. C., Woosley S. E., Langer N., 2010, @doi [ ] 10.1088/0004-637X/725/1/940 , https://ui.adsabs.harvard.edu/abs/2010ApJ...725..940Y 725, 940

    2010 doi

  197. [211]

    C., Dierks A., Langer N., 2012, @doi [ ] 10.1051/0004-6361/201117769 , https://ui.adsabs.harvard.edu/abs/2012A&A...542A.113Y 542, A113

    Yoon S. C., Dierks A., Langer N., 2012, @doi [ ] 10.1051/0004-6361/201117769 , https://ui.adsabs.harvard.edu/abs/2012A&A...542A.113Y 542, A113

    2012 doi

  198. [212]

    Yoon S.-C., Dessart L., Clocchiatti A., 2017, @doi [ ] 10.3847/1538-4357/aa6afe , https://ui.adsabs.harvard.edu/abs/2017ApJ...840...10Y 840, 10

    2017 doi

  199. [213]

    Zapartas E., et al., 2017a, @doi [ ] 10.1051/0004-6361/201629685 , https://ui.adsabs.harvard.edu/abs/2017A&A...601A..29Z 601, A29

    doi

  200. [214]

    Zapartas E., et al., 2017b, @doi [ ] 10.3847/1538-4357/aa7467 , https://ui.adsabs.harvard.edu/abs/2017ApJ...842..125Z 842, 125

    doi

  201. [215]

    Zapartas E., et al., 2021, @doi [ ] 10.1051/0004-6361/202141506 , https://ui.adsabs.harvard.edu/abs/2021A&A...656L..19Z 656, L19

    2021 doi

  202. [216]

    arXiv:2410.07335

    Zapartas E., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2410.07335 , https://ui.adsabs.harvard.edu/abs/2024arXiv241007335Z p. arXiv:2410.07335

    2024 doi arXiv

  203. [217]

    arXiv:2508.12677

    Zapartas E., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2508.12677 , https://ui.adsabs.harvard.edu/abs/2025arXiv250812677Z p. arXiv:2508.12677

    2025 doi

  204. [218]

    A., 1988, , https://ui.adsabs.harvard.edu/abs/1988A&AS...72..259D 72, 259

    de Jager C., Nieuwenhuijzen H., van der Hucht K. A., 1988, , https://ui.adsabs.harvard.edu/abs/1988A&AS...72..259D 72, 259

    1988

  205. [219]

    T., Cioni M

    van Loon J. T., Cioni M. R. L., Zijlstra A. A., Loup C., 2005, @doi [ ] 10.1051/0004-6361:20042555 , https://ui.adsabs.harvard.edu/abs/2005A&A...438..273V 438, 273

    2005 doi

  206. [220]

    van den Heuvel E. P. J., 1969, @doi [ ] 10.1086/110909 , https://ui.adsabs.harvard.edu/abs/1969AJ.....74.1095V 74, 1095

    1969 doi

Pith tools

Reviewed August 5, 2026 · model on record in the stance chip above.