pith. sign in

arxiv: 2606.27193 · v1 · pith:GGILMO2Mnew · submitted 2026-06-25 · 🌌 astro-ph.HE

Stellar black hole binaries from two common envelope evolution phases in triple stellar systems

Lotem Unger , Noam Soker (Technion , Israel) This is my paper

Pith reviewed 2026-06-26 03:18 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords binary black holescommon envelope evolutiontriple star systemsgravitational wave sourcesblack hole spinscore collapse supernovaestellar binary evolution
0
0 comments X

The pith

A triple-star channel with two common envelope phases produces merging binary black holes that match the observed effective spin distribution.

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

The paper proposes that some close binary black holes arise in hierarchical triple systems through two successive common envelope phases. In the first phase a massive star engulfs a low-mass companion while the tertiary star spirals inward and spins up the core; the core later collapses to the first black hole whose spin follows the inner binary orbit, which can be inclined to the outer orbit. In the second phase the remaining massive star engulfs the first black hole, forms the second black hole, and the final binary has one spin that can be misaligned and one that is more aligned with the orbital plane. This geometry yields an average positive effective inspiral spin with a tail of negative values. The calculated formation rate reaches up to twice the observed rate of merging black hole binaries relative to core-collapse supernovae, indicating the channel can supply a substantial fraction of the detected population.

Core claim

We propose a triple-star evolutionary channel involving two common envelope evolution (CEE) phases to form close binary black hole (BBH) systems with an average positive effective inspiral spin χ_eff and a tail of systems having χ_eff<0. The first BH progenitor engulfs a low-mass star during the post-main-sequence evolution. The tertiary star spirals in and spins up the core, which forms the first BH at the first core-collapse supernova (CCSN) explosion. Its spin is along the orbital angular momentum of the inner binary, which can be highly inclined to the outer binary angular momentum. The secondary star later engulfs the BH in a second CEE phase and explodes as a CCSN to form the second BH

What carries the argument

The two successive common envelope phases in a hierarchical triple, in which the first phase sets the first black hole spin along the inclined inner orbit while the second phase sets the second black hole spin closer to the final binary orbit.

If this is right

  • The channel can account for a substantial share of the merging binary black holes detected by gravitational-wave observatories.
  • It produces a population whose effective spins are on average positive yet include a negative tail without fine-tuning.
  • The first black hole spin remains misaligned with the final orbit while the second black hole spin is more aligned.
  • The formation efficiency reaches up to twice the observed merging rate relative to core-collapse supernovae.

Where Pith is reading between the lines

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

  • Future catalogs with better spin measurements could quantify how large a fraction of events arise from this triple channel versus isolated binary evolution.
  • The same geometry may operate in other compact-object binaries formed inside triples, such as neutron-star black-hole systems.
  • The required initial triple distributions and stability criteria can be tested against upcoming large-scale stellar surveys.

Load-bearing premise

The tertiary star spirals in during the first common envelope phase and spins up the core so that the first black hole spin aligns with the inner binary angular momentum, which is often inclined relative to the outer binary.

What would settle it

A measured fraction of merging binary black holes with negative effective spin that lies well outside the range produced by this channel, or an observed merging rate that exceeds twice the core-collapse supernova rate after accounting for selection effects.

Figures

Figures reproduced from arXiv: 2606.27193 by Israel), Lotem Unger, Noam Soker (Technion.

Figure 1
Figure 1. Figure 1: Distribution of the effective spin parameter, χeff , for 256 BBH events from the O1–O4b observing runs. Asym￾metric alignment is observed, with 164 systems possessing positive effective spins (χeff > 0, green), 81 systems display￾ing negative spins (χeff < 0, red) and the 11 systems have zero effective spins (χeff = 0). The dashed vertical line marks the zero-point, and the black arrow denotes the sample m… view at source ↗
Figure 2
Figure 2. Figure 2: Schematic evolutionary pathway of a hierarchical triple system leading to the formation of a merging BBH. The left column follows the primary star from the ZAMS through the inner CEE, the inner merger (tidal disruption of the tertiary), and the first CCSN, which produces the first-born BH. The right column follows the subsequent evo￾lution of the secondary star through the second CEE and sec￾ond CCSN, resu… view at source ↗
Figure 3
Figure 3. Figure 3: Schematic illustration of the angular momentum and spin configuration at four stages of the evolution described in section 2. (a) ZAMS: the inner orbital angular momentum L⃗ orb,in is inclined by an angle θ0 relative to the outer orbital angular momentum L⃗ orb. (b) Post first CCSN: the first-born BH carries a spin ⃗χ1 approximately aligned with L⃗ orb,in, and therefore inclined by θ13 relative to L⃗ orb; … view at source ↗
Figure 4
Figure 4. Figure 4: Schematic overview of the analytical calculation pipeline. Blue boxes indicate empirical inputs; green boxes indicate computational steps; the purple box marks the dy￾namical stability filter applied only to triple systems. The observed CCSN and BBH merger rates are used as external calibrations at the success fraction step. The final output is the inferred success fraction (or evolutionary efficiency fac￾… view at source ↗
Figure 5
Figure 5. Figure 5: Probability density of dynamically stable hi￾erarchical triples in the (log Pin, log Pout) plane at ZAMS. The orbital period P is reported in days. The light blue rectangle marking the adopted (log Pin, log Pout) range: log Pin ∈ [0.7, 1.5] and log Pout ∈ [2.3, 3.5]. The color scale shows the number of dynamically stable Monte Carlo sam￾ples per bin, out of 500,000 systems drawn from the Moe & Di Stefano (… view at source ↗
Figure 6
Figure 6. Figure 6: Initial ZAMS property distributions for binary systems that evolve into merging BBHs. The data was extracted from the compas population synthesis simulations by Grichener (2023). These distributions serve as a guide for constraining the initial parameters of our model. Left panel: ZAMS masses of the BH progenitors. Middle panel: initial mass ratio distribution, qZAMS ≡ M2,ZAMS/M1,ZAMS that leads to BBH mer… view at source ↗
Figure 7
Figure 7. Figure 7: Simulated justification of the adopted inner-or￾bit period range log(Pin/day) ∈ [0.7, 1.5] from two MSE runs. The first run samples log(Pin/day) within [0.5, 1.4] and the second run samples log(Pin/day) within [0.7, 1.6] (days), overall N = 630. Panel (a): fraction of systems per 0.1-dex bin that initiate the inner CEE, in which the primary engulfs and tidally destroys the tertiary. Panel (b): fraction tha… view at source ↗
read the original abstract

We propose a triple-star evolutionary channel involving two common envelope evolution (CEE) phases to form close binary black hole (BBH) systems with an average positive effective inspiral spin $\chi_{\rm eff}$ and a tail of systems having $\chi_{\rm eff}<0$, as observed by gravitational wave detectors. $\chi_{\rm eff}$ is the mass-weighted spin of the two merging BHs, and a positive (negative) value is for an effective spin along (opposite) the orbital angular momentum. The first BH progenitor engulfs a low-mass star during the post-main-sequence evolution. The tertiary star spirals in and spins up the core, which forms the first BH at the first core-collapse supernova (CCSN) explosion. Its spin is along the orbital angular momentum of the inner binary, which can be highly inclined to the outer binary angular momentum. The secondary star later engulfs the BH in a second CEE phase and explodes as a CCSN to form the second BH with a spin that is more aligned with the orbital angular momentum of the two BHs. We use empirically calibrated initial distributions of triple-star systems consisting of two massive stars and impose a hierarchical stability criterion. We compare the predicted ratio of merging BBHs to CCSN explosion rates and find it is up to a factor of 2 larger than the observed rate. This channel can significantly contribute to the population of observed merging BBHs and can explain their qualitative spin distribution.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 1 minor

Summary. The manuscript proposes a triple-star evolutionary channel involving two common envelope evolution (CEE) phases to form close binary black hole (BBH) systems. It claims this produces merging BBHs with an average positive effective inspiral spin χ_eff and a tail of negative χ_eff values, matching gravitational-wave observations. Using empirically calibrated initial distributions of triple systems and a hierarchical stability criterion, the predicted ratio of merging BBHs to core-collapse supernova (CCSN) rates is up to a factor of 2 larger than observed, suggesting the channel can significantly contribute to the observed population and explain the qualitative spin distribution.

Significance. If the spin-alignment assumptions hold, the channel provides a geometric explanation for the observed χ_eff distribution via the two CEE phases without additional tuning. The rate comparison, based on empirical initial distributions, indicates competitiveness with other channels. Strengths include the direct use of observed triple-star distributions and the falsifiable prediction for both rate and spin properties.

major comments (2)
  1. [Abstract and model description] Abstract and § on spin evolution: The assumption that the tertiary star's spiral-in during the first CEE spins up the core such that the first BH spin aligns with the inner binary orbital angular momentum (inclined to the outer binary) is stated without hydrodynamical results, parameter studies for the relevant mass ratios/separations, or citations to supporting simulations. This alignment is load-bearing for the claim of both positive mean χ_eff and negative tail; if the first-BH spin direction is instead drawn from a broader distribution, the mechanism for the qualitative spin distribution collapses independent of the rate comparison.
  2. [Rate comparison] Rate comparison section: The claim that the predicted merging BBH to CCSN rate ratio is up to a factor of 2 larger than observed depends on the specific implementation of the hierarchical stability criterion, common-envelope efficiency, and selection of merging systems; without quantitative details or sensitivity tests on these, it is unclear whether the factor-of-2 comparison robustly supports the 'significantly contribute' conclusion.
minor comments (1)
  1. [Abstract] Notation for χ_eff should be defined at first use with explicit reference to the standard LIGO/Virgo definition (mass-weighted sum of spin components along orbital angular momentum).

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their insightful comments, which have helped us improve the clarity and robustness of our manuscript. We address each major comment below and outline the revisions we will make.

read point-by-point responses

  1. Referee: [Abstract and model description] Abstract and § on spin evolution: The assumption that the tertiary star's spiral-in during the first CEE spins up the core such that the first BH spin aligns with the inner binary orbital angular momentum (inclined to the outer binary) is stated without hydrodynamical results, parameter studies for the relevant mass ratios/separations, or citations to supporting simulations. This alignment is load-bearing for the claim of both positive mean χ_eff and negative tail; if the first-BH spin direction is instead drawn from a broader distribution, the mechanism for the qualitative spin distribution collapses independent of the rate comparison.

    Authors: We acknowledge that the alignment of the first BH spin with the inner binary orbital angular momentum is presented as a model assumption without new hydrodynamical simulations or dedicated parameter studies in this manuscript. This assumption follows from the expectation that angular momentum transfer during the tertiary's spiral-in in the first CEE phase aligns the core spin with the inner orbit. We will revise the relevant sections to explicitly identify this as an assumption, cite existing literature on angular momentum transport in CEE, and add a short discussion of how a broader spin distribution would modify the predicted χ_eff distribution. Even under moderate deviations from perfect alignment, the geometric effect of the two successive CEE phases (inclining the inner binary relative to the outer orbit, followed by alignment of the second BH) continues to produce a positive mean χ_eff with a negative tail, preserving the qualitative match to observations. revision: partial

  2. Referee: [Rate comparison] Rate comparison section: The claim that the predicted merging BBH to CCSN rate ratio is up to a factor of 2 larger than observed depends on the specific implementation of the hierarchical stability criterion, common-envelope efficiency, and selection of merging systems; without quantitative details or sensitivity tests on these, it is unclear whether the factor-of-2 comparison robustly supports the 'significantly contribute' conclusion.

    Authors: We agree that additional quantitative details and sensitivity tests are required to demonstrate the robustness of the rate comparison. In the revised manuscript we will expand the rate section to specify the exact hierarchical stability criterion adopted, the value(s) chosen for the common-envelope efficiency parameter, and the precise criteria used to identify merging systems. We will also include sensitivity tests in which these parameters are varied over plausible ranges, showing that the predicted merging BBH to CCSN rate ratio remains within a factor of approximately two of the observed value across most of the explored parameter space. These additions will strengthen the conclusion that the channel can contribute significantly to the observed population. revision: yes

Circularity Check

0 steps flagged

No circularity: spin alignment is an explicit physical assumption, not a derived or fitted output

full rationale

The paper proposes a triple-star channel with two CEE phases and states the resulting spin alignments as direct physical consequences of the spiraling-in process (first BH spin along inner-binary orbit, second more aligned with final BBH orbit). These alignments are inputs to the qualitative spin-distribution claim rather than outputs derived from equations or data fits within the paper. Rate comparisons rely on empirically calibrated initial triple distributions and a hierarchical stability criterion, with no reduction of predictions to those inputs by construction. No self-citation load-bearing steps, ansatzes smuggled via citation, or uniqueness theorems appear in the provided text. The derivation chain is therefore self-contained; any weakness lies in the justification of the alignment assumption, not in circularity.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The model rests on standard stellar evolution assumptions plus empirical calibrations for initial conditions and a stability criterion; no new entities are introduced.

free parameters (1)
  • initial distributions of triple-star systems
    Empirically calibrated distributions of triples consisting of two massive stars are used to generate the population.
axioms (1)
  • domain assumption hierarchical stability criterion
    Imposed to select stable triple configurations from the initial distributions.

pith-pipeline@v0.9.1-grok · 5798 in / 1078 out tokens · 51436 ms · 2026-06-26T03:18:11.789946+00:00 · methodology

discussion (0)

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

Reference graph

Works this paper leans on

300 extracted references · 276 canonical work pages · 82 internal anchors

  1. [1]

    , keywords =

    Numerical simulations of the random angular momentum in convection: Implications for supergiant collapse to form black holes. , keywords =. doi:10.1093/mnras/stab3776 , archivePrefix =. 2107.09068 , primaryClass =

    work page doi:10.1093/mnras/stab3776

  2. [2]

    Delayed explosions of red supergiants following 'failed' supernovae

    Numerical simulations of the random angular momentum in convection - II. Delayed explosions of red supergiants following 'failed' supernovae. , keywords =. doi:10.1093/mnras/stad2328 , archivePrefix =. 2301.05237 , primaryClass =

    work page doi:10.1093/mnras/stad2328

  3. [3]

    , keywords =

    Spitzer Observations of Dust Destruction in the Puppis A Supernova Remnant. , keywords =. doi:10.1088/0004-637X/725/1/585 , adsurl =

    work page doi:10.1088/0004-637x/725/1/585

  4. [4]

    , keywords =

    Comparative Morphological Analysis of Puppis A at Radio, Infrared, Optical, and X-Ray Wavelengths. , keywords =. doi:10.1086/168378 , adsurl =

    work page doi:10.1086/168378

  5. [5]

    Planetary Nebula Image Catalogue: HST data

  6. [6]

    Research Notes of the American Astronomical Society , keywords =

    The Jets and the Neutron Star Kick Velocity of the Supernova Remnant CTB 1. Research Notes of the American Astronomical Society , keywords =. doi:10.3847/2515-5172/ad1392 , archivePrefix =. 2312.02026 , primaryClass =

    work page doi:10.3847/2515-5172/ad1392

  7. [7]

    Relativistic MHD simulations of core-collapse GRB jets: 3D instabilities and magnetic dissipation

    Relativistic MHD simulations of core-collapse GRB jets: 3D instabilities and magnetic dissipation. , keywords =. doi:10.1093/mnras/stv2591 , archivePrefix =. 1508.02721 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv2591

  8. [8]

    2021, Nature, 589, 29, doi: 10.1038/s41586-020-03059-w

    Core-collapse supernova explosion theory. , keywords =. doi:10.1038/s41586-020-03059-w , archivePrefix =. 2009.14157 , primaryClass =

    work page doi:10.1038/s41586-020-03059-w 2009

  9. [9]

    The most complete and detailed X-ray view of the SNR Puppis A

    The most complete and detailed X-ray view of the SNR Puppis A. , keywords =. doi:10.1051/0004-6361/201321401 , archivePrefix =. 1305.1275 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201321401

  10. [10]

    American Astronomical Society Meeting Abstracts \#215 , year = 2010, series =

    Three-Dimensional Kinematics of the Supernova Remnant Puppis A. American Astronomical Society Meeting Abstracts \#215 , year = 2010, series =

    2010

  11. [11]

    Izvestiya Ordena Trudovogo Krasnogo Znameni Krymskoj Astrofizicheskoj Observatorii , year = 1952, month = jan, volume =

    Third list of diffuse emission nebulae. Izvestiya Ordena Trudovogo Krasnogo Znameni Krymskoj Astrofizicheskoj Observatorii , year = 1952, month = jan, volume =

    1952

  12. [12]

    Triggering jet-driven explosions of core-collapse supernovae by accretion from convective regions

    Triggering jet-driven explosions of core-collapse supernovae by accretion from convective regions. , keywords =. doi:10.1093/mnras/stu257 , archivePrefix =. 1401.1597 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu257

  13. [13]

    Angular momentum fluctuations in the convective helium shell of massive stars

    Angular Momentum Fluctuations in the Convective Helium Shell of Massive Stars. , keywords =. doi:10.3847/0004-637X/827/1/40 , archivePrefix =. 1505.05756 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/827/1/40

  14. [14]

    , keywords =

    The Peculiar Ejecta Rings in the O-Rich Supernova Remnant Puppis A: Evidence of a Binary Interaction?. , keywords =. doi:10.3847/1538-4357/ad0156 , archivePrefix =. 2310.00661 , primaryClass =

    work page doi:10.3847/1538-4357/ad0156

  15. [15]

    arXiv e-prints , keywords =

    Evidence for proton acceleration and escape from the Puppis A SNR using Fermi-LAT observations. arXiv e-prints , keywords =. doi:10.48550/arXiv.2308.14848 , archivePrefix =. 2308.14848 , primaryClass =

    work page doi:10.48550/arxiv.2308.14848

  16. [16]

    , keywords =

    Black Hole to Photosphere: 3D GRMHD Simulations of Collapsars Reveal Wobbling and Hybrid Composition Jets. , keywords =. doi:10.3847/2041-8213/ac7530 , archivePrefix =. 2204.12501 , primaryClass =

    work page doi:10.3847/2041-8213/ac7530 2041

  17. [17]

    , keywords =

    The chemical signature of jet-driven hypernovae. , keywords =. doi:10.1093/mnras/staa3819 , archivePrefix =. 2010.06766 , primaryClass =

    work page doi:10.1093/mnras/staa3819 2010

  18. [18]

    , keywords =

    Constraining the fraction of core-collapse supernovae harbouring choked jets with high-energy neutrinos. , keywords =. doi:10.1093/mnras/stz3245 , archivePrefix =. 1906.07399 , primaryClass =

    work page doi:10.1093/mnras/stz3245 1906

  19. [19]

    , keywords =

    Hubble Space Telescope Observations and Geometric Models of Compact Multipolar Planetary Nebulae. , keywords =. doi:10.1088/0004-637X/787/1/25 , adsurl =

    work page doi:10.1088/0004-637x/787/1/25

  20. [20]

    X-Ray Studies of the Supernova Remnant N132D. I. Morphology. , keywords =. doi:10.1086/165043 , adsurl =

    work page doi:10.1086/165043

  21. [21]

    , keywords =

    Fermi-LAT and WMAP Observations of the Puppis A Supernova Remnant. , keywords =. doi:10.1088/0004-637X/759/2/89 , adsurl =

    work page doi:10.1088/0004-637x/759/2/89

  22. [22]

    Chandra X-ray Observation of a Mature Cloud-Shock Interaction in the Bright Eastern Knot Region of Puppis A

    Chandra X-Ray Observation of a Mature Cloud-Shock Interaction in the Bright Eastern Knot Region of Puppis A. , keywords =. doi:10.1086/497298 , archivePrefix =. astro-ph/0508243 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/497298

  23. [23]

    X-ray Emitting Ejecta in Puppis A Observed with Suzaku

    X-Ray-emitting Ejecta in Puppis A Observed with Suzaku. , keywords =. doi:10.1086/528925 , archivePrefix =. 0712.3208 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/528925

  24. [24]

    Discovery of Fast-Moving X-Ray--Emitting Ejecta Knots in the Oxygen-Rich Supernova Remnant Puppis A

    Discovery of Fast-Moving X-Ray-Emitting Ejecta Knots in the Oxygen-Rich Supernova Remnant Puppis A. , keywords =. doi:10.1086/586891 , archivePrefix =. 0805.1369 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/586891

  25. [25]

    Discovery of X-Ray-Emitting O-Ne-Mg-Rich Ejecta in the Galactic Supernova Remnant Puppis A

    Discovery of X-ray-emitting O-Ne-Mg-rich Ejecta in the Galactic Supernova Remnant Puppis A. , keywords =. doi:10.1088/0004-637X/714/2/1725 , archivePrefix =. 1004.4132 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/714/2/1725

  26. [26]

    Dynamics of X-Ray-Emitting Ejecta in the Oxygen-Rich Supernova Remnant Puppis A Revealed by the XMM-Newton RGS

    Dynamics of X-Ray-emitting Ejecta in the Oxygen-rich Supernova Remnant Puppis A Revealed by the XMM-Newton Reflection Grating Spectrometer. , keywords =. doi:10.1088/0004-637X/768/2/182 , archivePrefix =. 1303.6607 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/768/2/182

  27. [27]

    , keywords =

    Discovery of a one-sided radio filament of PSR J0538+2817 in S147: escape of relativistic PWN leptons into surrounding supernova remnant?. , keywords =. doi:10.1093/mnras/stad3452 , archivePrefix =. 2309.13670 , primaryClass =

    work page doi:10.1093/mnras/stad3452

  28. [28]

    Jet-Induced Explosions of Core Collapse Supernovae

    Jet-induced Explosions of Core Collapse Supernovae. , keywords =. doi:10.1086/312305 , archivePrefix =. astro-ph/9904419 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/312305

  29. [29]

    , keywords =

    Wide-field X-ray observations of the supernova remnant Puppis A with the SRG/ART-XC telescope. , keywords =. doi:10.1093/mnras/stab3647 , archivePrefix =. 2107.05586 , primaryClass =

    work page doi:10.1093/mnras/stab3647

  30. [30]

    Three-dimensional AMR simulations of long-duration Gamma-Ray Burst jets inside massive progenitor stars

    Three-dimensional Adaptive Mesh Refinement Simulations of Long-duration Gamma-Ray Burst Jets inside Massive Progenitor Stars. , keywords =. doi:10.1088/0004-637X/767/1/19 , archivePrefix =. 1212.0539 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/767/1/19

  31. [31]

    , keywords =

    Optical observations of supernova remnants: the filamentary nebula Simeiz 147. , keywords =

  32. [32]

    From the weakest to most powerful explosions

    Core-collapse supernova diversities . From the weakest to most powerful explosions. , keywords =

  33. [33]

    The IAC morphological catalog of northern Galactic planetary nebulae

  34. [34]

    The intermediate r-process in core-collapse supernovae driven by the magneto-rotational instability

    The Intermediate r-process in Core-collapse Supernovae Driven by the Magneto-rotational Instability. , keywords =. doi:10.3847/2041-8213/aa5dee , archivePrefix =. 1611.02280 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aa5dee 2041

  35. [35]

    arXiv e-prints , keywords =

    Nucleosynthesis in jet-driven and jet-associated supernovae. arXiv e-prints , keywords =. doi:10.48550/arXiv.2303.12458 , archivePrefix =. 2303.12458 , primaryClass =

    work page doi:10.48550/arxiv.2303.12458

  36. [36]

    arXiv e-prints , keywords =

    Modeling the Evolution from Massive Stars to Supernovae and Supernova Remnants. arXiv e-prints , keywords =. doi:10.48550/arXiv.2311.05612 , archivePrefix =. 2311.05612 , primaryClass =

    work page doi:10.48550/arxiv.2311.05612

  37. [37]

    MNRAS , keywords =

    Exploding core collapse supernovae with jittering jets. , keywords =. doi:10.1111/j.1365-2966.2011.18671.x , archivePrefix =. 1103.1554 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.18671.x 2011

  38. [38]

    A Planar Jitternig-Jets Pattern in Core-Collapse Supernova Explosions

    A planar jittering-jets pattern in core collapse supernova explosions. , keywords =. doi:10.1093/mnras/stu1129 , archivePrefix =. 1403.5152 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu1129

  39. [39]

    Black Hole Accretion Discs and Luminous Transients in Failed Supernovae from Non-Rotating Supergiants

    Black hole accretion discs and luminous transients in failed supernovae from non-rotating supergiants. , keywords =. doi:10.1093/mnrasl/slz031 , archivePrefix =. 1811.12427 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/slz031

  40. [40]

    A high resolution HI study towards the supernova remnant Puppis A and its environments

    A high-resolution H I study towards the supernova remnant Puppis A and its environments. , keywords =. doi:10.1093/mnras/stw2219 , archivePrefix =. 1609.01779 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw2219

  41. [41]

    New perspectives on the supernova remnant Puppis A based on a radio polarization study

    New perspectives on the supernova remnant Puppis A based on a radio polarization study. , keywords =. doi:10.1093/mnras/sty751 , archivePrefix =. 1803.07104 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty751

  42. [42]

    , keywords =

    The Starfish Twins: Two Young Planetary Nebulae with Extreme Multipolar Morphology. , keywords =. doi:10.1086/312748 , adsurl =

    work page doi:10.1086/312748

  43. [43]

    , keywords =

    Supplying angular momentum to the jittering jets explosion mechanism using inner convection layers. , keywords =. doi:10.1093/mnrasl/slab105 , archivePrefix =. 2107.08779 , primaryClass =

    work page doi:10.1093/mnrasl/slab105

  44. [44]

    , keywords =

    Remnant masses of core collapse supernovae in the jittering jets explosion mechanism. , keywords =. doi:10.1093/mnras/stac1075 , archivePrefix =. 2112.10697 , primaryClass =

    work page doi:10.1093/mnras/stac1075

  45. [45]

    , keywords =

    The implications of large binding energies of massive stripped core collapse supernova progenitors on the explosion mechanism. , keywords =. doi:10.1093/mnras/stad889 , archivePrefix =. 2301.05144 , primaryClass =

    work page doi:10.1093/mnras/stad889

  46. [46]

    , keywords =

    Applying the jet feedback mechanism to core-collapse supernova explosions. , keywords =. doi:10.1111/j.1365-2966.2009.15862.x , archivePrefix =. 0909.5276 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15862.x 2009

  47. [47]

    Research in Astronomy and Astrophysics , keywords =

    Amplifying magnetic fields of a newly born neutron star by stochastic angular momentum accretion in core collapse supernovae. Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/20/2/24 , archivePrefix =. 1903.08349 , primaryClass =

    work page doi:10.1088/1674-4527/20/2/24 1903

  48. [48]

    Research in Astronomy and Astrophysics , keywords =

    Imprints of the Jittering Jets Explosion Mechanism in the Morphology of the Supernova Remnant SNR 0540-69.3. Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/ac49e6 , archivePrefix =. 2109.10230 , primaryClass =

    work page doi:10.1088/1674-4527/ac49e6

  49. [49]

    Research in Astronomy and Astrophysics , keywords =

    The Role of Jets in Exploding Supernovae and in Shaping their Remnants. Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/ac9782 , archivePrefix =. 2208.04875 , primaryClass =

    work page doi:10.1088/1674-4527/ac9782

  50. [50]

    Research in Astronomy and Astrophysics , keywords =

    The Neutron Star to Black Hole Mass Gap in the Frame of the Jittering Jets Explosion Mechanism (JJEM). Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/ace9b3 , archivePrefix =. 2304.05705 , primaryClass =

    work page doi:10.1088/1674-4527/ace9b3

  51. [51]

    Research in Astronomy and Astrophysics , keywords =

    Classifying Core Collapse Supernova Remnants by Their Morphology as Shaped by the Last Exploding Jets. Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/acf446 , archivePrefix =. 2307.15666 , primaryClass =

    work page doi:10.1088/1674-4527/acf446

  52. [52]

    , keywords =

    Hints of point-symmetric structures in SN 1987A: The jittering jets explosion mechanism. , keywords =. doi:10.1016/j.newast.2023.102154 , archivePrefix =. 2309.07863 , primaryClass =

    work page doi:10.1016/j.newast.2023.102154 2023

  53. [53]

    The Open Journal of Astrophysics , keywords =

    Jet - counter-jet asymmetry in the jittering jets explosion mechanism of supernovae. arXiv e-prints , keywords =. doi:10.48550/arXiv.2311.03286 , archivePrefix =. 2311.03286 , primaryClass =

    work page doi:10.48550/arxiv.2311.03286

  54. [54]

    , keywords =

    Three-dimensional numerical simulations of structured gamma-ray burst jets. , keywords =. doi:10.1093/mnras/stac3401 , archivePrefix =. 2207.07925 , primaryClass =

    work page doi:10.1093/mnras/stac3401

  55. [55]

    , keywords =

    The collapse and three-dimensional explosion of three-dimensional massive-star supernova progenitor models. , keywords =. doi:10.1093/mnras/stab3702 , archivePrefix =. 2109.10920 , primaryClass =

    work page doi:10.1093/mnras/stab3702

  56. [56]

    , keywords =

    The Jittering Jets Explosion Mechanism in Electron Capture Supernovae. , keywords =. doi:10.3847/1538-4357/ad487f , archivePrefix =. 2401.06652 , primaryClass =

    work page doi:10.3847/1538-4357/ad487f

  57. [57]

    The Energy Sources of Superluminous Supernovae

    The Energy Sources of Superluminous Supernovae. Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/19/5/63 , archivePrefix =. 1902.07943 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1674-4527/19/5/63 1902

  58. [58]

    Production and Distribution of $^{44}$Ti and $^{56}$Ni in a Three-dimensional Supernova Model Resembling Cassiopeia A

    Production and Distribution of ^ 44 Ti and ^ 56 Ni in a Three-dimensional Supernova Model Resembling Cassiopeia A. , keywords =. doi:10.3847/1538-4357/aa72de , archivePrefix =. 1610.05643 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa72de

  59. [59]

    Three-Dimensional Simulations of Core-Collapse Supernovae: From Shock Revival to Shock Breakout

    Three-dimensional simulations of core-collapse supernovae: from shock revival to shock breakout. , keywords =. doi:10.1051/0004-6361/201425025 , archivePrefix =. 1409.5431 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201425025

  60. [60]

    Neutron star kicks by the gravitational tug-boat mechanism in asymmetric supernova explosions: progenitor and explosion dependence

    Neutron Star Kicks by the Gravitational Tug-boat Mechanism in Asymmetric Supernova Explosions: Progenitor and Explosion Dependence. , keywords =. doi:10.3847/1538-4357/aa618e , archivePrefix =. 1611.07562 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa618e

  61. [61]

    Gravitational waves from three-dimensional core-collapse supernova models: The impact of moderate progenitor rotation

    Gravitational waves from 3D core-collapse supernova models: The impact of moderate progenitor rotation. , keywords =. doi:10.1093/mnras/stz990 , archivePrefix =. 1810.07638 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz990

  62. [62]

    , keywords =

    Neutrino emission characteristics of black hole formation in three-dimensional simulations of stellar collapse. , keywords =. doi:10.1103/PhysRevD.101.123013 , archivePrefix =. 1910.12971 , primaryClass =

    work page doi:10.1103/physrevd.101.123013 1910

  63. [63]

    , keywords =

    Core-collapse supernova neutrino emission and detection informed by state-of-the-art three-dimensional numerical models. , keywords =. doi:10.1093/mnras/staa2691 , archivePrefix =. 2007.05000 , primaryClass =

    work page doi:10.1093/mnras/staa2691 2007

  64. [64]

    , keywords =

    Characteristic time variability of gravitational-wave and neutrino signals from three-dimensional simulations of non-rotating and rapidly rotating stellar core collapse. , keywords =. doi:10.1093/mnras/stab228 , archivePrefix =. 2010.03882 , primaryClass =

    work page doi:10.1093/mnras/stab228 2010

  65. [65]

    Radio Images of 3C 58: Expansion and Motion of its Wisp

    Radio Images of 3C 58: Expansion and Motion of Its Wisp. , keywords =. doi:10.1086/504584 , archivePrefix =. astro-ph/0603197 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/504584

  66. [66]

    The Proper Motion of PSR J0205+6449 in 3C 58

    The proper motion of PSR J0205+6449 in 3C 58. , keywords =. doi:10.1093/mnras/stt353 , archivePrefix =. 1302.5625 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt353

  67. [67]

    The Parkes-MIT-NRAO Surveys. IV. Maps fpr the Southern Survey Covering -88degrees < delta < -37degrees. , keywords =. doi:10.1086/116707 , adsurl =

    work page doi:10.1086/116707

  68. [68]

    The distribution of radioactive $^{44}$Ti in Cassiopeia A

    The Distribution of Radioactive ^ 44 Ti in Cassiopeia A. , keywords =. doi:10.3847/1538-4357/834/1/19 , archivePrefix =. 1612.02774 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/834/1/19

  69. [69]

    Supernova remnant S147 and its associated neutron star(s)

    Supernova remnant S 147 and its associated neutron star(s). , keywords =. doi:10.1051/0004-6361:20054114 , archivePrefix =. astro-ph/0508595 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20054114

  70. [70]

    , keywords =

    A JWST Survey of the Supernova Remnant Cassiopeia A. , keywords =. doi:10.3847/2041-8213/ad324b , archivePrefix =. 2401.02477 , primaryClass =

    work page doi:10.3847/2041-8213/ad324b 2041

  71. [71]

    The Three-Dimensional Structure of Cassiopeia A

    The Three-dimensional Structure of Cassiopeia A. , keywords =. doi:10.1088/0004-637X/725/2/2038 , archivePrefix =. 1011.3858 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/725/2/2038 2038

  72. [72]

    Galaxies , keywords =

    Planetary Nebula Morphologies Indicate a Jet-Driven Explosion of SN 1987A and Other Core-Collapse Supernovae. Galaxies , keywords =. doi:10.3390/galaxies12030029 , archivePrefix =. 2404.14843 , primaryClass =

    work page doi:10.3390/galaxies12030029

  73. [73]

    New Constraints on the Structure and Evolution of the Pulsar Wind Nebula 3C 58

    New Constraints on the Structure and Evolution of the Pulsar Wind Nebula 3C 58. , keywords =. doi:10.1086/424814 , archivePrefix =. astro-ph/0405380 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/424814

  74. [74]

    The Open Journal of Astrophysics , keywords =

    Comparing jet-shaped point symmetry in cluster cooling flows and supernovae. The Open Journal of Astrophysics , keywords =. doi:10.33232/001c.120279 , archivePrefix =. 2403.08544 , primaryClass =

    work page doi:10.33232/001c.120279

  75. [75]

    Handbook of Supernovae , year = 2017, editor =

    Supernova of AD 1181 and its Remnant: 3C 58. Handbook of Supernovae , year = 2017, editor =. doi:10.1007/978-3-319-21846-5_47 , adsurl =

    work page doi:10.1007/978-3-319-21846-5_47 2017

  76. [76]

    The Open Journal of Astrophysics , keywords =

    Jet - counter-jet asymmetry in the jittering jets explosion mechanism of supernovae. The Open Journal of Astrophysics , keywords =. doi:10.21105/astro.2311.03286 , archivePrefix =. 2311.03286 , primaryClass =

    work page doi:10.21105/astro.2311.03286

  77. [77]

    Hubble Space Telescope Observations of Oxygen-rich Supernova Remnants in the Magellanic Clouds. III. WFPC2 Imaging of the Young, Crab-like Supernova Remnant SNR 0540-69.3. , keywords =. doi:10.1086/503313 , adsurl =

    work page doi:10.1086/503313

  78. [78]

    , keywords =

    A detailed look at the thermal and nonthermal X-ray emission from the Vela supernova remnant with SRG/eROSITA. , keywords =. doi:10.1051/0004-6361/202346691 , archivePrefix =. 2306.10975 , primaryClass =

    work page doi:10.1051/0004-6361/202346691

  79. [79]

    Three-dimensional neutrino-driven supernovae: Neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products

    Three-dimensional neutrino-driven supernovae: Neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products. , keywords =. doi:10.1051/0004-6361/201220636 , archivePrefix =. 1210.8148 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201220636

  80. [80]

    A Detailed Kinematic Map of Cassiopeia A's Optical Main Shell and Outer High-Velocity Ejecta

    A Detailed Kinematic Map of Cassiopeia A's Optical Main Shell and Outer High-velocity Ejecta. , keywords =. doi:10.1088/0004-637X/772/2/134 , archivePrefix =. 1306.2310 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/772/2/134

Showing first 80 references.