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This paper claims that stellar rotation has little effect on how entropy perturbations evolve during collapse, leaving their pre-shock amplitudes below one percent of the local sound speed.

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2026-08-04 19:07 UTC pith:ZYKWRH2F

load-bearing objection Useful extension of the vortex work to entropy perturbations, but the central '<0.01' amplitudes rely on an unstated WKB approximation that a referee should check. the 3 major comments →

arxiv 2509.09419 v1 pith:ZYKWRH2F submitted 2025-09-11 astro-ph.SR astro-ph.HE

Impact of rotation on the accretion of entropy perturbations in collapsing massive stars

Olzhas Mukazhanov This is my paper
classification astro-ph.SR astro-ph.HE PACS 95.30.Lz97.60.Bw
keywords core-collapse supernovaentropy perturbationsstellar rotationaccretionlinear perturbation theoryvorticityacoustic wavesBondi accretion
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

Entropy perturbations created by convection in the nuclear-burning shells of massive stars are carried inward by the collapsing flow, and as they fall they generate vorticity and sound waves. This paper asks whether stellar rotation amplifies those perturbations before they reach the supernova shock. Using linear perturbation theory on a rotating transonic Bondi background, it finds that rotation barely changes the outcome: radial velocity and pressure perturbations stay largely insensitive to spin, and even the azimuthal velocity growth at high rotation remains below one percent of the local sound speed. A sympathetic reader would take away that pre-shock entropy perturbations are a subdominant source of shock perturbation, and rotation does not rescue them. The result extends the authors' earlier finding for convective vortices to entropy waves.

Core claim

On the paper's own terms: when entropy waves are advected through the accelerating, rotating collapse flow, the baroclinic torque converts entropy variations into vorticity, and the distorted density surfaces radiate acoustic waves. The paper shows that including rotation—up to a specific angular momentum several times the maximum expected in rapidly rotating pre-supernova cores—changes the growth only modestly: radial velocity and pressure perturbations stay below 10⁻² and nearly independent of L, while the azimuthal component grows with L for m=3,4 but still remains below one percent of c_s. Compared with convective eddies at the same initial Mach number, entropy-wave contributions are sma

What carries the argument

The load-bearing tool is a second-order linear ODE for rδυ̃_φ (Eq. 1/A38), derived on a rotating transonic Bondi background restricted to the equatorial plane with negligible poloidal derivatives. Rotation enters only through the Doppler-shifted frequency ω' = ω − mL/r²; the entropy perturbation is advected as δS ∝ exp(∫ iω'/υ_r dr), and it sources vorticity through the baroclinic term. The regularity condition at the sonic radius selects the homogeneous solution, and the no-incoming-acoustic-wave boundary condition fixes the emitted sound. This isolates rotation's effects (differential spin-up and centrifugal slowdown) from other processes, letting the author scan L from 0 to 3×10¹⁶ cm²/s.

Load-bearing premise

The rotating transonic Bondi background, with its constant-specific-angular-momentum radial profile, equatorial-plane restriction, and neglected poloidal derivatives, captures the actual rotational state of infalling stellar matter all the way to the shock.

What would settle it

A 3D simulation of a rotating pre-supernova core that tracks entropy perturbations through collapse and finds pre-shock velocity or pressure perturbation amplitudes exceeding one percent of the local sound speed—or a strong, rotation-dependent growth toward the shock—would contradict the central claim.

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

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If this is right

  • Pre-shock entropy perturbations will not contribute significantly to the turbulent energy behind the shock for low-order azimuthal modes, regardless of progenitor rotation.
  • The rotation-insensitivity of radial velocity and pressure perturbations means parameterized 1D or 2D pre-shock models that ignore rotation can still capture the entropy-wave contribution.
  • High-m (small-scale) entropy waves can rival convective eddies in amplitude, but since their effect on the critical neutrino luminosity scales as 1/m, they remain dynamically secondary.
  • If the central claim is right, rotation's known role in explosion dynamics must come from post-shock effects (centrifugal support, SASI, magnetorotational mechanisms), not from pre-shock amplification of entropy waves.
  • The method gives a quantitative bound: even at extreme angular momenta, entropy-wave-induced velocity and pressure perturbations at the shock stay below about 1% of the local sound speed or pressure.

Where Pith is reading between the lines

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

  • The same Doppler-shift argument suggests that other passively advected pre-shock perturbations (e.g., composition inhomogeneities or magnetic-field seed fluctuations) will also be weakly amplified by rotation before shock crossing, since spin-up at large radii is slow.
  • If angular momentum were not radially constant but grew more steeply inward—for instance through magnetic braking coupling inner and outer shells—the corotation singularity in ω' could become a genuine amplifier, a regime the constant-L background excludes by construction.
  • One testable extension: relax the equatorial-plane restriction and include poloidal derivatives; if rotationally induced latitudinal shear grows entropy waves faster, the negative result could be confined to the equator.
  • The paper's normalization (δM ~ 0.1 at the shell) means all amplitudes scale linearly; a progenitor with δM ~ 0.3 would still give sub-3% perturbations, leaving order-of-magnitude headroom before entropy waves become relevant.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 7 minor

Summary. This paper analyzes the linear evolution of entropy perturbations in a rotating, transonic Bondi accretion flow modeling the pre-shock collapse of a massive star. The authors derive a second-order ODE for the azimuthal velocity perturbation (Eq. A38), solve it with homogeneous solutions from Paper I, and present closed-form expressions for the vorticity generated by advected entropy perturbations (Eqs. A59–A65). Results are given for m=1–4, two shell radii, and ten values of specific angular momentum up to L_max=3e16 cm^2/s. The main conclusion is that rotation has little effect on the evolution of entropy perturbations: radial velocity and pressure perturbations at 0.1 r_s remain below 10^-2 and are nearly L-independent, while the azimuthal velocity increases with L for m=3,4 but stays below one percent of the local sound speed. The paper argues that pre-shock entropy waves are sub-dominant to convective eddies for large-scale (low-m) modes.

Significance. If the derivation is correct, the paper provides a useful negative result: pre-collapse entropy fluctuations are unlikely to be an important seed for shock revival, and rotation does not change this. The work extends the authors' earlier vortex analysis to the entropy channel, and it includes a systematic parameter study and explicit analytic formulas. The paper is clearly structured and mostly self-contained. However, the central quantitative claim depends on an approximation in Appendix A.2 that is not justified in the text (see major comments), and the cited nonlinear validation (Telman et al. 2024) covers convective vortices rather than entropy perturbations. The result is therefore plausible but currently not established.

major comments (3)
  1. [Appendix A.2, Eqs. (A58)–(A59)] Eq. (A59) solves Eq. (A58) as if the phase q=∫ iω'/υ_r² dX were linear in X. The exact particular solution of (∂²_X+W)Y=A e^q is A e^q/(q_X²+W+q_XX), with q_XX=i(1-M²)/υ_r d/dr(ω'/υ_r²); the paper drops q_XX without stating a WKB condition. In addition, the transcription of Eq. (A38) via Eq. (A25) drops a term proportional to ∂_X[(c²_shell−c²)/υ_r²]. With ω'=ω−mL/r², dω'/dr=2mL/r³, so q_XX is not uniformly small: near r=0.1r_s, m=4, L=L_max it is a few tens of percent of the retained denominator, and it diverges at corotation. Since Eqs. (A60)–(A65) and Figs. 2–4 inherit this step, the '<0.01' amplitudes and the 'little effect of rotation' conclusion are not established by the written derivation. Telman et al. (2024) validates vortices, not this entropy-wave formula.
  2. [Section 2, Eq. (A10)] The pattern frequency ω is never specified. All rotation effects enter through ω'=ω−mL/r² in the source, the exponential phases, and the denominator of Eq. (A59); Figs. 4–5 therefore depend on the choice of ω. The paper should state the adopted value (e.g., ω=m L/R_shell²) and demonstrate that the conclusions are robust to this choice. As written, the calculation is not reproducible.
  3. [Appendix A.1, Eqs. (A45)–(A57)] The acoustic solution is obtained after integration by parts that introduces terms ∝1/ω'. The text says the corotation singularity is avoided by 'combining integration with and without integration by parts,' but no explicit procedure is given. Since the pressure amplitudes in Fig. 4 are acoustic and are part of the central claim, the reader cannot verify that the result is regular and convergent near corotation. Please spell out the combined procedure or point to the exact equations in Paper I that implement it.
minor comments (7)
  1. [Section 2 heading] 'Methdods' should be 'Methods'.
  2. [Section 2, first paragraph] 'a reasonable representation for for stellar matter' contains a duplicated 'for'.
  3. [Section 3.2] 'stretching of voritices' should be 'vortices'.
  4. [Fig. 2] The axis labels appear truncated ('/c' and 'r/c'); please label them δυ_φ/c and δυ_r/c explicitly, in both the figure and the caption.
  5. [Eqs. (2)–(4)] δE is called 'specific energy' but has dimensions of energy; please clarify the division by mass or redefine the symbol.
  6. [Appendix A] The parameter R/μ=1 is introduced without comment; state whether this is a unit choice or an approximation and what it implies for the entropy normalization.
  7. [Data Availability] The data availability statement is minimal; please provide the scripts or a repository that generate Figs. 2–5, or at least specify the numerical quadrature settings used.

Circularity Check

0 steps flagged

No significant circularity: the entropy-perturbation calculation is a forward linear solve; the rotation-independence claim is not fitted to the output, and the main self-citations are either re-derived or independently validated.

full rationale

The paper's central claim—that rotation has little effect on entropy perturbations before the shock—follows from solving the first-order linearized equations (Eq. 1 and Eq. A38) with stated background and boundary conditions, not from fitting parameters to the desired conclusion. The input choices (L_max, R_shell, δM=0.1, M=1.4 M⊙, r_s=1.5×10^3 km) are explicit physical/data choices and are rescalable because the formalism is linear; no fitted parameter is later renamed as a prediction. The use of Paper I for the rotating Bondi background and Frobenius homogeneous solutions is load-bearing but is standard citation of prior published work, and the method has been compared with nonlinear simulations in Telman et al. (2024), so it is not an unverified self-citation chain. The condition δK=m²c_shell²δS/γ is an initial-vorticity-free matching condition, not an output-equivalent definition. The only noteworthy weakness is mathematical rather than circular: Eq. (A59) appears to solve Eq. (A58) by dropping q_XX=d/dX(iω'/υ_r²) without a stated slow-variation criterion, so the small-amplitude result inherits an unverified approximation. This is a correctness/detail gap, not a circular reduction of the conclusion to the inputs.

Axiom & Free-Parameter Ledger

6 free parameters · 6 axioms · 0 invented entities

No new entities are postulated. The paper's quantitative output rests on hand-picked model parameters (M, r_s, dM, R_shell, L range) and on the rotating Bondi background plus equatorial-plane restriction inherited from Paper I, all stated explicitly. The most load-bearing freedom is the initial-condition ansatz dK0 = m^2 c_shell^2 dS0/gamma.

free parameters (6)
  • Central mass M = 1.4 M_sun
    Chosen by hand in Section 2, 'in line with the mass of proto neutron stars obtained in modern 3D simulations'.
  • Sonic radius r_s = 1.5e3 km
    Chosen by hand in Section 2; 'setting its value fixes the pressure scale'.
  • Turbulent Mach number dM = 0.1
    Adopted as default from Collins et al. (2018) in Section 3.1; sets the entropy perturbation amplitude dS and hence the absolute normalization of the results.
  • Initial shell radius R_shell = 2 r_s and 4 r_s
    Parameter choice in Section 3; the results depend on the starting radius of the advected perturbations.
  • Specific angular momentum L = 0 to 3e16 cm^2/s
    Scanned in Section 2; L_max is chosen as an extreme case, exceeding expected pre-supernova values by a factor of a few.
  • Initial vorticity normalization dK0 = m^2 c_shell^2 dS0/gamma
    Chosen in Appendix A.1 so that the vorticity vanishes at the initial radius; an initialization ansatz that selects which superposition of the two solutions is used.
axioms (6)
  • domain assumption The background is a rotating transonic Bondi accretion flow with a constant specific angular momentum radial profile (Appendix B of Paper I).
    Section 2. The entire perturbation calculation is linearized on this flow; if it misrepresents the actual collapse kinematics, the conclusions change.
  • domain assumption Perturbations are small and the flow is adiabatic, with no neutrino cooling, heating, or nuclear dissociation during the pre-shock phase.
    Section 2 and Eqs. (A1)-(A3); the paper acknowledges this is an idealized framework 'not intended to yield precise quantitative predictions'.
  • domain assumption Restriction to the equatorial plane with exp(im phi) angular dependence and neglect of poloidal derivatives.
    Section 2, 'we neglect poloidal derivatives (Walk et al. 2023)'. Suppresses 3D, rotationally driven effects such as meridional flows and non-axisymmetric instabilities.
  • standard math Ideal gas equation of state with gamma = 4/3 and R/mu = 1.
    Section 2 and Appendix A; standard for radiation-dominated stellar matter.
  • standard math Boundary conditions: regularity at the sonic radius and no incoming acoustic waves from infinity.
    Section 2 and Appendix A; standard outgoing-radiation condition for accretion problems.
  • domain assumption Entropy fluctuation amplitude estimate dS ~ dQ/T ~ dv^2/T with dM = 0.1 (Eqs. 5-6).
    Section 3.1; sets the absolute amplitude of the perturbations that the quantitative claims are expressed against; linearity allows rescaling.

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Cite this review

Pith. "Pith review of Impact of rotation on the accretion of entropy perturbations in collapsing massive stars." pith.science (2026). https://pith.science/paper/ZYKWRH2F

@misc{pith2026250909419,
  author       = {Pith},
  title        = {Pith review of: Impact of rotation on the accretion of entropy perturbations in collapsing massive stars},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ZYKWRH2F}},
  note         = {Machine review of arXiv:2509.09419}
}
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read the original abstract

Convection in the innermost shells of massive stars plays an important role in initiating core-collapse supernovae. When these convective motions reach the supernova shock, they create extra turbulence, which helps energize the explosion. In our earlier work, we studied the effect of rotation on the hydrodynamic evolution of convective vortices in collapsing stars. This study focuses on how rotation influences the entropy perturbations, which naturally form in turbulent convection. As these perturbations are carried inward with the collapsing star, they generate both vorticity and sound waves. Using linear perturbation theory, we model entropy waves as small disturbances on top of a steady background flow. Our results show that stellar rotation has little effect on the evolution of entropy perturbations during collapse, prior to encountering the supernova shock. This outcome is consistent with our earlier findings on the limited influence of rotation in the accretion of convective eddies.

discussion (0)

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Reference graph

Works this paper leans on

81 extracted references · 4 canonical work pages

  1. [1]

    MNRAS539(3), 2707–2717 (2025) https://doi.org/10

    Abdikamalov, E., Beniamini, P.: Reverse and forward shock afterglow emission from steep jets viewed off-axis. MNRAS539(3), 2707–2717 (2025) https://doi.org/10. 1093/mnras/staf649 arXiv:2502.12757 [astro-ph.HE]

    Pith/arXiv arXiv 2025

  2. [2]

    Machine Learning: Science and Technology5(4), 045077 (2024) https: //doi.org/10.1088/2632-2153/ada33a arXiv:2409.14508 [astro-ph.HE] 17

    Abylkairov, Y.S., Edwards, M.C., Orel, D., Mitra, A., Shukirgaliyev, B., Abdikamalov, E.: Evaluating machine learning models for supernova gravitational wave signal classification. Machine Learning: Science and Technology5(4), 045077 (2024) https: //doi.org/10.1088/2632-2153/ada33a arXiv:2409.14508 [astro-ph.HE] 17

    Pith/arXiv arXiv 2024

  3. [3]

    MNRAS493(3), 3496–3512 (2020) https://doi.org/10.1093/ mnras/staa533 arXiv:1907.06966 [astro-ph.SR]

    Abdikamalov, E., Foglizzo, T.: Acoustic wave generation in collapsing massive stars with convective shells. MNRAS493(3), 3496–3512 (2020) https://doi.org/10.1093/ mnras/staa533 arXiv:1907.06966 [astro-ph.SR]

    Pith/arXiv arXiv 2020

  4. [4]

    MNRAS503(3), 3617–3628 (2021) https: //doi.org/10.1093/mnras/stab715 arXiv:2012.06710 [astro-ph.SR]

    Abdikamalov, E., Foglizzo, T., Mukazhanov, O.: Impact of rotation on the evolution of convective vortices in collapsing stars. MNRAS503(3), 3617–3628 (2021) https: //doi.org/10.1093/mnras/stab715 arXiv:2012.06710 [astro-ph.SR]

    Pith/arXiv arXiv 2021

  5. [5]

    Particles1(1), 7 (2018) https://doi.org/10.3390/particles1010007

    Abdikamalov, E., Huete, C., Nussupbekov, A., Berdibek, S.: Turbulence generation by shock-acoustic-wave interaction in core-collapse supernovae. Particles1(1), 7 (2018) https://doi.org/10.3390/particles1010007

    work page doi:10.3390/particles1010007 2018

  6. [6]

    In: Revista Mexicana de Astronomia Y Astrofisica Conference Series

    Myrzakul, S., Tuiakbayeva, D., Kostangeldinova, A.: Early-Time Optical Spectral Shape Measurements of GRB 200925B. In: Revista Mexicana de Astronomia Y Astrofisica Conference Series. Revista Mexicana de Astronomia y Astrofisica Con- ference Series, vol. 59, pp. 109–113 (2025). https://doi.org/10.22201/ia.14052059p. 2025.59.20

    work page doi:10.22201/ia.14052059p 2025

  7. [7]

    ApJ741, 33 (2011) https://doi.org/10.1088/0004-637X/741/1/33 arXiv:1012.1848 [astro-ph.SR]

    Arnett, W.D., Meakin, C.: Turbulent Cells in Stars: Fluctuations in Kinetic Energy and Luminosity. ApJ741, 33 (2011) https://doi.org/10.1088/0004-637X/741/1/33 arXiv:1012.1848 [astro-ph.SR]

    Pith/arXiv arXiv 2011

  8. [8]

    ApJ584, 954 (2003) https: //doi.org/10.1086/344135

    Akiyama, S., Wheeler, J.C., Meier, D.L., Lichtenstadt, I.: The Magnetorotational Instability in Core-Collapse Supernova Explosions. ApJ584, 954 (2003) https: //doi.org/10.1086/344135

    doi:10.1086/344135 2003

  9. [9]

    ApJ664, 416–434 (2007) https://doi.org/10.1086/519161 arXiv:astro-ph/0702539

    Burrows, A., Dessart, L., Livne, E., Ott, C.D., Murphy, J.: Simulations of Magnetically Driven Supernova and Hypernova Explosions in the Context of Rapid Rotation. ApJ664, 416–434 (2007) https://doi.org/10.1086/519161 arXiv:astro-ph/0702539

    Pith/arXiv arXiv 2007

  10. [10]

    A&A 674, 205 (2023) https://doi.org/10.1051/0004-6361/202245799 arXiv:2301.01962 [astro-ph.HE]

    Buellet, A.-C., Foglizzo, T., Guilet, J., Abdikamalov, E.: Effect of stellar rotation on the development of post-shock instabilities during core-collapse supernovae. A&A 674, 205 (2023) https://doi.org/10.1051/0004-6361/202245799 arXiv:2301.01962 [astro-ph.HE]

    Pith/arXiv arXiv 2023

  11. [11]

    ApJ416, 75 (1993) https: //doi.org/10.1086/187074

    Burrows, A., Goshy, J.: A Theory of Supernova Explosions. ApJ416, 75 (1993) https: //doi.org/10.1086/187074

    doi:10.1086/187074 1993

  12. [12]

    Rotational instabilities and multi- messenger signatures

    Bugli, M., Guilet, J., Foglizzo, T., Obergaulinger, M.: Three-dimensional core-collapse supernovae with complex magnetic structures - II. Rotational instabilities and multi- messenger signatures. MNRAS520(4), 5622–5634 (2023) https://doi.org/10.1093/ mnras/stad496 arXiv:2210.05012 [astro-ph.HE]

    Pith/arXiv arXiv 2023

  13. [13]

    MNRAS537(2), 1182–1196 (2025) https://doi.org/10.1093/mnras/staf066 18 arXiv:2410.17232 [astro-ph.HE]

    Boccioli, L., Gogilashvili, M., Murphy, J., O’Connor, E.P.: Quantifying the impact of the Si/O interface in CCSN explosions using the Force Explosion Condi- tion. MNRAS537(2), 1182–1196 (2025) https://doi.org/10.1093/mnras/staf066 18 arXiv:2410.17232 [astro-ph.HE]

    Pith/arXiv arXiv 2025

  14. [14]

    ApJ818(2), 123 (2016) https: //doi.org/10.3847/0004-637X/818/2/123 arXiv:1409.5779 [astro-ph.SR]

    Yakunin, K.N.: The Development of Explosions in Axisymmetric Ab Initio Core- collapse Supernova Simulations of 12-25 M Stars. ApJ818(2), 123 (2016) https: //doi.org/10.3847/0004-637X/818/2/123 arXiv:1409.5779 [astro-ph.SR]

    Pith/arXiv arXiv 2016

  15. [15]

    MNRAS482(4), 5430–5440 (2019) https://doi.org/10.1093/mnras/ sty3110 arXiv:1808.07493 [astro-ph.HE]

    Beniamini, P., Nakar, E.: Observational constraints on the structure of gamma- ray burst jets. MNRAS482(4), 5430–5440 (2019) https://doi.org/10.1093/mnras/ sty3110 arXiv:1808.07493 [astro-ph.HE]

    Pith/arXiv arXiv 2019

  16. [16]

    Ap&SS41, 287 (1976) https://doi.org/10

    Bisnovatyi-Kogan, G.S., Popov, I.P., Samokhin, A.A.: The magnetohydrodynamic rotational model of supernova explosion. Ap&SS41, 287 (1976) https://doi.org/10. 1007/BF00646184

    1976

  17. [17]

    Burrows, A.: Colloquium: Perspectives on core-collapse supernova theory. Rev. Mod. Phys.85, 245 (2013) https://doi.org/10.1103/RevModPhys.85.245 arXiv:1210.4921 [astro-ph.SR]

    Pith/arXiv arXiv 2013

  18. [18]

    ApJ964(1), 16 (2024) https: //doi.org/10.3847/2041-8213/ad319e arXiv:2401.06840 [astro-ph.HE]

    Burrows, A., Wang, T., Vartanyan, D.: Physical Correlations and Predictions Emerg- ing from Modern Core-collapse Supernova Theory. ApJ964(1), 16 (2024) https: //doi.org/10.3847/2041-8213/ad319e arXiv:2401.06840 [astro-ph.HE]

    Pith/arXiv arXiv 2024

  19. [19]

    ApJ987(2), 164 (2025) https://doi.org/10.3847/1538-4357/addd04 arXiv:2412.07831 [astro-ph.SR]

    Burrows, A., Wang, T., Vartanyan, D.: Channels of Stellar-mass Black Hole Formation. ApJ987(2), 164 (2025) https://doi.org/10.3847/1538-4357/addd04 arXiv:2412.07831 [astro-ph.SR]

    Pith/arXiv arXiv 2025

  20. [20]

    ApJ915(1), 28 (2021) https://doi.org/10.3847/1538-4357/abf82e arXiv:2010.10506 [astro-ph.HE]

    Bollig, R., Yadav, N., Kresse, D., Janka, H.-T., M¨ uller, B., Heger, A.: Self-consistent 3D Supernova Models From -7 Minutes to +7 s: A 1-bethe Explosion of a 19 M⊙ Progenitor. ApJ915(1), 28 (2021) https://doi.org/10.3847/1538-4357/abf82e arXiv:2010.10506 [astro-ph.HE]

    arXiv 2021

  21. [21]

    ApJ808, 21 (2015) https://doi.org/ 10.1088/2041-8205/808/1/L21 arXiv:1503.02199 [astro-ph.HE]

    Couch, S.M., Chatzopoulos, E., Arnett, W.D., Timmes, F.X.: The Three-dimensional Evolution to Core Collapse of a Massive Star. ApJ808, 21 (2015) https://doi.org/ 10.1088/2041-8205/808/1/L21 arXiv:1503.02199 [astro-ph.HE]

    Pith/arXiv arXiv 2015

  22. [22]

    MNRAS473, 1695–1704 (2018) https://doi.org/10

    Collins, C., M¨ uller, B., Heger, A.: Properties of convective oxygen and silicon burning shells in supernova progenitors. MNRAS473, 1695–1704 (2018) https://doi.org/10. 1093/mnras/stx2470 arXiv:1709.00236 [astro-ph.SR]

    Pith/arXiv arXiv 2018

  23. [23]

    ApJ778, 7 (2013)

    Couch, S.M., Ott, C.D.: Revival of The Stalled Core-Collapse Supernova Shock Triggered by Precollapse Asphericity in the Progenitor Star. ApJ778, 7 (2013)

    2013

  24. [24]

    ApJ988(2), 224 (2025) https://doi.org/10.3847/ 1538-4357/ade2d1 arXiv:2506.06415 [astro-ph.SR] 19

    Dhanpal, S., Benomar, O., Hanasoge, S., Fuller, J.: Anomalously Fast Core and Enve- lope Rotation in Red Giants. ApJ988(2), 224 (2025) https://doi.org/10.3847/ 1538-4357/ade2d1 arXiv:2506.06415 [astro-ph.SR] 19

    Pith/arXiv arXiv 2025

  25. [25]

    A&A564, 27 (2014) https://doi.org/10.1051/ 0004-6361/201322779 arXiv:1401.3096 [astro-ph.SR]

    Campante, T.L., Casagrande, L., Ceillier, T., Davies, G.R., De Cat, P., Fu, J.N., Garc ´ ıa, R.A., Lobel, A., Mosser, B., Reese, D.R., Regulo, C., Schou, J., Stahn, T., Thygesen, A.O., Yang, X.H., Chaplin, W.J., Christensen-Dalsgaard, J., Eggen- berger, P., Gizon, L., Mathis, S., Molenda- ˙Zakowicz, J., Pinsonneault, M.: Seismic constraints on the radial ...

    Pith/arXiv arXiv 2014

  26. [26]

    Fields, C.E., Couch, S.M.: Three-dimensional Hydrodynamic Simulations of Convec- tive Nuclear Burning in Massive Stars Near Iron Core Collapse. ApJ921(1), 28 (2021) https://doi.org/10.3847/1538-4357/ac24fb arXiv:2107.04617 [astro-ph.SR] Fern´ andez, R.: Three-dimensional simulations of SASI- and convection-dominated core-collapse supernovae. MNRAS452, 207...

    Pith/arXiv arXiv 2021

  27. [27]

    ApJ654, 1006 (2007) https: //doi.org/10.1086/509612

    Foglizzo, T., Galletti, P., Scheck, L., Janka, H.-T.: Instability of a Stalled Accretion Shock: Evidence for the Advective-Acoustic Cycle. ApJ654, 1006 (2007) https: //doi.org/10.1086/509612

    doi:10.1086/509612 2007

  28. [28]

    MNRAS450(1), 414–427 (2015) https://doi.org/10.1093/mnras/stv698 arXiv:1501.06951 [astro-ph.HE]

    Fuller, J., Klion, H., Abdikamalov, E., Ott, C.D.: Supernova seismology: gravitational wave signatures of rapidly rotating core collapse. MNRAS450(1), 414–427 (2015) https://doi.org/10.1093/mnras/stv698 arXiv:1501.06951 [astro-ph.HE]

    Pith/arXiv arXiv 2015

  29. [29]

    What does perturbed Bondi accretion sound like? A&A368, 311–324 (2001) https://doi.org/ 10.1051/0004-6361:20000506 arXiv:astro-ph/0101056

    Foglizzo, T.: Entropic-acoustic instability of shocked Bondi accretion I. What does perturbed Bondi accretion sound like? A&A368, 311–324 (2001) https://doi.org/ 10.1051/0004-6361:20000506 arXiv:astro-ph/0101056

    Pith/arXiv arXiv 2001

  30. [30]

    Foglizzo, T.: A Simple Toy Model of the Advective-Acoustic Instability. I. Perturba- tive Approach. ApJ694, 820 (2009) https://doi.org/10.1088/0004-637X/694/2/820 arXiv:0809.2302

    Pith/arXiv arXiv 2009

  31. [31]

    ApJ652, 1436 (2006) https://doi.org/10.1086/508443

    Foglizzo, T., Scheck, L., Janka, H.-T.: Neutrino-driven Convection versus Advection in Core-Collapse Supernovae. ApJ652, 1436 (2006) https://doi.org/10.1086/508443

    doi:10.1086/508443 2006

  32. [32]

    A&A 363, 174–183 (2000) astro-ph/0009193 Fern´ andez, R., Thompson, C.: Stability of a Spherical Accretion Shock with Nuclear Dissociation

    Foglizzo, T., Tagger, M.: Entropic-acoustic instability in shocked accretion flows. A&A 363, 174–183 (2000) astro-ph/0009193 Fern´ andez, R., Thompson, C.: Stability of a Spherical Accretion Shock with Nuclear Dissociation. ApJ697, 1827 (2009)

    Pith/arXiv arXiv 2000

  33. [33]

    ApJ570(2), 61–64 (2002) https://doi.org/10

    Granot, J., Panaitescu, A., Kumar, P., Woosley, S.E.: Off-Axis Afterglow Emission from Jetted Gamma-Ray Bursts. ApJ570(2), 61–64 (2002) https://doi.org/10. 1086/340991 arXiv:astro-ph/0201322 [astro-ph] 20

    Pith/arXiv arXiv 2002

  34. [34]

    Physica Scripta94(9), 094002 (2019) https://doi.org/10.1088/ 1402-4896/ab0228

    Huete, C., Abdikamalov, E.: Response of nuclear-dissociating shocks to vortic- ity perturbations. Physica Scripta94(9), 094002 (2019) https://doi.org/10.1088/ 1402-4896/ab0228

    2019

  35. [35]

    MNRAS475, 3305–3323 (2018) https://doi

    Huete, C., Abdikamalov, E., Radice, D.: The impact of vorticity waves on the shock dynamics in core-collapse supernovae. MNRAS475, 3305–3323 (2018) https://doi. org/10.1093/mnras/stx3360 arXiv:1709.07363 [astro-ph.HE]

    Pith/arXiv arXiv 2018

  36. [36]

    Physical Review Fluids5(11), 113403 (2020) https://doi.org/10.1103/PhysRevFluids.5.113403

    Huete, C., Cobos-Campos, F., Abdikamalov, E., Bouquet, S.: Acoustic stability of nonadiabatic high-energy-density shocks. Physical Review Fluids5(11), 113403 (2020) https://doi.org/10.1103/PhysRevFluids.5.113403

    work page doi:10.1103/physrevfluids.5.113403 2020

  37. [37]

    ApJ626, 350 (2005)

    Heger, A., Woosley, S.E., Spruit, H.C.: Presupernova Evolution of Differentially Rotating Massive Stars Including Magnetic Fields. ApJ626, 350 (2005)

    2005

  38. [38]

    Janka, H.-T., Melson, T., Summa, A.: Physics of Core-Collapse Supernovae in Three Dimensions: A Sneak Preview. Ann. Rev. Nuc. Part. Sc.66, 341 (2016) https: //doi.org/10.1146/annurev-nucl-102115-044747 arXiv:1602.05576 [astro-ph.SR]

    Pith/arXiv arXiv 2016

  39. [39]

    MNRAS494(4), 5360–5373 (2020) https://doi.org/10.1093/mnras/staa944 arXiv:1911.08819 [astro-ph.SR]

    Kazeroni, R., Abdikamalov, E.: The impact of progenitor asymmetries on the neutrino- driven convection in core-collapse supernovae. MNRAS494(4), 5360–5373 (2020) https://doi.org/10.1093/mnras/staa944 arXiv:1911.08819 [astro-ph.SR]

    Pith/arXiv arXiv 2020

  40. [40]

    ApJ896(2), 102 (2020) https://doi.org/10.3847/ 1538-4357/ab9308 arXiv:2003.02004 [astro-ph.HE]

    Kuroda, T., Arcones, A., Takiwaki, T., Kotake, K.: Magnetorotational Explo- sion of a Massive Star Supported by Neutrino Heating in General Relativistic Three-dimensional Simulations. ApJ896(2), 102 (2020) https://doi.org/10.3847/ 1538-4357/ab9308 arXiv:2003.02004 [astro-ph.HE]

    Pith/arXiv arXiv 2020

  41. [41]

    AJ137(5), 4100–4108 (2009) https://doi.org/10.1088/0004-6256/137/5/4100 arXiv:0902.0898 [astro-ph.HE]

    Klotz, A., Bo¨ er, M., Atteia, J.L., Gendre, B.: Early Optical Observations of Gamma-Ray Bursts by the TAROT Telescopes: Period 2001-2008. AJ137(5), 4100–4108 (2009) https://doi.org/10.1088/0004-6256/137/5/4100 arXiv:0902.0898 [astro-ph.HE]

    Pith/arXiv arXiv 2001

  42. [42]

    Shock-free Bondi accretion

    Kovalenko, I.G., Eremin, M.A.: Instability of spherical accretion - I. Shock-free Bondi accretion. MNRAS298, 861–870 (1998) https://doi.org/10.1046/j.1365-8711.1998. 01667.x

    arXiv 1998

  43. [43]

    MNRAS520(4), 6104–6110 (2023) https://doi.org/ 10.1093/mnras/stad538 arXiv:2211.03029 [astro-ph.HE]

    Komesh, T., Grossan, B., Maksut, Z., Abdikamalov, E., Krugov, M., Smoot, G.F.: Evolution of the afterglow optical spectral shape of GRB 201015A in the first hour: evidence for dust destruction. MNRAS520(4), 6104–6110 (2023) https://doi.org/ 10.1093/mnras/stad538 arXiv:2211.03029 [astro-ph.HE]

    Pith/arXiv arXiv 2023

  44. [44]

    Kotake, K., Sumiyoshi, K., Yamada, S., Takiwaki, T., Kuroda, T., Suwa, Y., Nagakura, H.: Core-collapse supernovae as supercomputing science: A status report toward six-dimensional simulations with exact Boltzmann neutrino transport in full general relativity. Prog. Theo. Exp. Phys.2012, 301 (2012) https://doi.org/10.1093/ptep/ pts009 arXiv:1205.6284 [astr...

    Pith/arXiv arXiv 2012

  45. [45]

    Kumar, P., Zhang, B.: The physics of gamma-ray bursts & relativistic jets. Phys. Rep. 561, 1–109 (2015) https://doi.org/10.1016/j.physrep.2014.09.008 arXiv:1410.0679 [astro-ph.HE]

    Pith/arXiv arXiv 2015

  46. [46]

    ApJ535, 402 (2000) https://doi.org/10.1086/308821 arXiv:astro-ph/9906400 M¨ uller, B.: The dynamics of neutrino-driven supernova explosions after shock revival in 2D and 3D

    Lai, D., Goldreich, P.: Growth of Perturbations in Gravitational Collapse and Accre- tion. ApJ535, 402 (2000) https://doi.org/10.1086/308821 arXiv:astro-ph/9906400 M¨ uller, B.: The dynamics of neutrino-driven supernova explosions after shock revival in 2D and 3D. MNRAS453, 287–310 (2015) https://doi.org/10.1093/mnras/stv1611 arXiv:1506.05139 [astro-ph.SR...

    Pith/arXiv arXiv 2000

  47. [47]

    MNRAS516(2), 1752–1767 (2022) https://doi.org/10.1093/mnras/ stac2335 arXiv:2202.07967 [astro-ph.HE]

    Matsumoto, J., Asahina, Y., Takiwaki, T., Kotake, K., Takahashi, H.R.: Magnetic support for neutrino-driven explosion of 3D non-rotating core-collapse super- nova models. MNRAS516(2), 1752–1767 (2022) https://doi.org/10.1093/mnras/ stac2335 arXiv:2202.07967 [astro-ph.HE]

    Pith/arXiv arXiv 2022

  48. [48]

    Living Reviews in Computational Astrophysics6(1), 4 (2020) https://doi

    Mezzacappa, A., Endeve, E., Messer, O.E.B., Bruenn, S.W.: Physical, numerical, and computational challenges of modeling neutrino transport in core-collapse super- novae. Living Reviews in Computational Astrophysics6(1), 4 (2020) https://doi. org/10.1007/s41115-020-00010-8 arXiv:2010.09013 [astro-ph.HE]

    Pith/arXiv arXiv 2020

  49. [49]

    A&A548, 10 (2012) https://doi.org/10.1051/0004-6361/201220106 arXiv:1209.3336 [astro-ph.SR]

    Klaus, T.C., Li, J., Mathur, S., Morris, R.L.: Spin down of the core rotation in red giants. A&A548, 10 (2012) https://doi.org/10.1051/0004-6361/201220106 arXiv:1209.3336 [astro-ph.SR]

    Pith/arXiv arXiv 2012

  50. [50]

    Metzger, B.D., Giannios, D., Thompson, T.A., Bucciantini, N., Quataert, E.: The protomagnetar model for gamma-ray bursts. MNRAS413(3), 2031–2056 (2011) https://doi.org/10.1111/j.1365-2966.2011.18280.x arXiv:1012.0001 [astro-ph.HE] M¨ uller, B., Heger, A., Powell, J.: Minimum Neutron Star Mass in Neutrino-Driven Supernova Explosions. Phys. Rev. Lett.134(7)...

    arXiv 2031

  51. [51]

    MNRAS 529(4), 3582–3592 (2024) https://doi.org/10.1093/mnras/stae714 arXiv:2310.15649 [astro-ph.HE]

    Mitra, A., Orel, D., Abylkairov, Y.S., Shukirgaliyev, B., Abdikamalov, E.: Probing nuclear physics with supernova gravitational waves and machine learning. MNRAS 529(4), 3582–3592 (2024) https://doi.org/10.1093/mnras/stae714 arXiv:2310.15649 [astro-ph.HE]

    Pith/arXiv arXiv 2024

  52. [52]

    Mitra, A., Shukirgaliyev, B., Abylkairov, Y.S., Abdikamalov, E.: Exploring supernova gravitational waves with machine learning. MNRAS520(2), 2473–2483 (2023) https: //doi.org/10.1093/mnras/stad169 arXiv:2209.14542 [astro-ph.HE] M¨ uller, B., Varma, V.: A 3D simulation of a neutrino-driven supernova explosion aided by convection and magnetic fields. MNRAS4...

    Pith/arXiv arXiv 2023

  53. [53]

    arXiv e-prints, 2401–11635 (2024) https://doi.org/10.48550/arXiv.2401.11635 arXiv:2401.11635 [astro-ph.HE]

    Mezzacappa, A., Zanolin, M.: Gravitational Waves from Neutrino-Driven Core Col- lapse Supernovae: Predictions, Detection, and Parameter Estimation. arXiv e-prints, 2401–11635 (2024) https://doi.org/10.48550/arXiv.2401.11635 arXiv:2401.11635 [astro-ph.HE]

    Pith/arXiv arXiv doi:10.48550/arxiv.2401.11635 2024

  54. [54]

    MNRAS492(4), 5764–5779 (2020) https://doi.org/10.1093/mnras/staa261 arXiv:1912.07615 [astro-ph.HE]

    Nagakura, H., Burrows, A., Radice, D., Vartanyan, D.: A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simu- lations. MNRAS492(4), 5764–5779 (2020) https://doi.org/10.1093/mnras/staa261 arXiv:1912.07615 [astro-ph.HE]

    Pith/arXiv arXiv 2020

  55. [55]

    MNRAS461(3), 3296–3313 (2016) https://doi.org/10.1093/ mnras/stw1453 arXiv:1602.03028 [astro-ph.HE]

    Nakamura, K., Horiuchi, S., Tanaka, M., Hayama, K., Takiwaki, T., Kotake, K.: Multimessenger signals of long-term core-collapse supernova simulations: synergetic observation strategies. MNRAS461(3), 3296–3313 (2016) https://doi.org/10.1093/ mnras/stw1453 arXiv:1602.03028 [astro-ph.HE]

    Pith/arXiv arXiv 2016

  56. [56]

    ApJ834(1), 28 (2017) https://doi.org/10.3847/1538-4357/834/1/28 arXiv:1610.05362 [astro- ph.HE] 23

    Nakar, E., Piran, T.: The Observable Signatures of GRB Cocoons. ApJ834(1), 28 (2017) https://doi.org/10.3847/1538-4357/834/1/28 arXiv:1610.05362 [astro- ph.HE] 23

    Pith/arXiv arXiv 2017

  57. [57]

    MNRAS483(1), 208–222 (2019) https://doi.org/10.1093/mnras/sty3114 arXiv:1811.05515 [astro-ph.HE]

    Nagakura, H., Takahashi, K., Yamamoto, Y.: On the importance of progenitor asym- metry to shock revival in core-collapse supernovae. MNRAS483(1), 208–222 (2019) https://doi.org/10.1093/mnras/sty3114 arXiv:1811.05515 [astro-ph.HE]

    Pith/arXiv arXiv 2019

  58. [58]

    ´A.: Magnetorotational core collapse of possible GRB progenitors - I

    Obergaulinger, M., Aloy, M. ´A.: Magnetorotational core collapse of possible GRB progenitors - I. Explosion mechanisms. MNRAS492(4), 4613–4634 (2020) https: //doi.org/10.1093/mnras/staa096 arXiv:1909.01105 [astro-ph.HE] O’Connor, E.P., Couch, S.M.: Exploring Fundamentally Three-dimensional Phenom- ena in High-fidelity Simulations of Core-collapse Supernov...

    Pith/arXiv arXiv 2020

  59. [59]

    ApJ871(2), 25 (2019) https://doi.org/10.3847/2041-8213/aaffce

    Piran, T., Nakar, E., Mazzali, P., Pian, E.: Relativistic Jets in Core-collapse Super- novae. ApJ871(2), 25 (2019) https://doi.org/10.3847/2041-8213/aaffce

    work page doi:10.3847/2041-8213/aaffce 2019

  60. [60]

    Ap&SS341(2), 457–464 (2012) https://doi.org/10.1007/s10509-012-1100-z arXiv:1204.0632 [astro-ph.HE]

    Popov, S.B., Turolla, R.: Initial spin periods of neutron stars in supernova rem- nants. Ap&SS341(2), 457–464 (2012) https://doi.org/10.1007/s10509-012-1100-z arXiv:1204.0632 [astro-ph.HE]

    Pith/arXiv arXiv 2012

  61. [61]

    Science Advances6(11), 2732 (2020) https://doi.org/10.1126/sciadv.aay2732 arXiv:2003.06662 [astro-ph.HE]

    Raynaud, R., Guilet, J., Janka, H.-T., Gastine, T.: Magnetar formation through a convective dynamo in protoneutron stars. Science Advances6(11), 2732 (2020) https://doi.org/10.1126/sciadv.aay2732 arXiv:2003.06662 [astro-ph.HE]

    Pith/arXiv arXiv 2020

  62. [62]

    ApJ852(1), 28 (2018) https://doi.org/10.3847/1538-4357/aa9ce8 arXiv:1708.04154 [astro-ph.HE]

    Summa, A., Janka, H.-T., Melson, T., Marek, A.: Rotation-supported Neutrino-driven Supernova Explosions in Three Dimensions and the Critical Luminosity Condition. ApJ852(1), 28 (2018) https://doi.org/10.3847/1538-4357/aa9ce8 arXiv:1708.04154 [astro-ph.HE]

    Pith/arXiv arXiv 2018

  63. [63]

    MNRAS531(3), 3732–3743 (2024) https://doi.org/10.1093/mnras/stae1361 arXiv:2309.05161 [astro- ph.HE]

    Shibagaki, S., Kuroda, T., Kotake, K., Takiwaki, T., Fischer, T.: Three-dimensional GRMHD simulations of rapidly rotating stellar core collapse. MNRAS531(3), 3732–3743 (2024) https://doi.org/10.1093/mnras/stae1361 arXiv:2309.05161 [astro- ph.HE]

    Pith/arXiv arXiv 2024

  64. [64]

    MNRAS 493(1), 138–142 (2020) https://doi.org/10.1093/mnrasl/slaa021 arXiv:1909.09730 [astro-ph.HE]

    Shibagaki, S., Kuroda, T., Kotake, K., Takiwaki, T.: A new gravitational-wave signa- ture of low-T/—W— instability in rapidly rotating stellar core collapse. MNRAS 493(1), 138–142 (2020) https://doi.org/10.1093/mnrasl/slaa021 arXiv:1909.09730 [astro-ph.HE]

    Pith/arXiv arXiv 2020

  65. [65]

    ApJ519(1), 17–20 (1999) https://doi.org/10.1086/312109 arXiv:astro-ph/9903339 [astro-ph]

    Sari, R., Piran, T., Halpern, J.P.: Jets in Gamma-Ray Bursts. ApJ519(1), 17–20 (1999) https://doi.org/10.1086/312109 arXiv:astro-ph/9903339 [astro-ph]

    Pith/arXiv arXiv 1999

  66. [66]

    MNRAS508(1), 43–47 (2021) https:// 24 doi.org/10.1093/mnrasl/slab105 arXiv:2107.08779 [astro-ph.HE]

    Shishkin, D., Soker, N.: Supplying angular momentum to the jittering jets explosion mechanism using inner convection layers. MNRAS508(1), 43–47 (2021) https:// 24 doi.org/10.1093/mnrasl/slab105 arXiv:2107.08779 [astro-ph.HE]

    Pith/arXiv arXiv 2021

  67. [67]

    MNRAS535(2), 1388–1393 (2024) https://doi.org/10.1093/mnras/stae2448 arXiv:2409.17737 [astro-ph.SR]

    Telman, Y., Abdikamalov, E., Foglizzo, T.: Convective vortices in collapsing stars. MNRAS535(2), 1388–1393 (2024) https://doi.org/10.1093/mnras/stae2448 arXiv:2409.17737 [astro-ph.SR]

    Pith/arXiv arXiv 2024

  68. [68]

    Elasticity, Relativity, and Statistical Physics, (2017)

    2017

  69. [69]

    ApJ831, 75 (2016) https://doi.org/10.3847/0004-637X/831/1/75 arXiv:1605.09524 [astro-ph.HE]

    Takahashi, K., Iwakami, W., Yamamoto, Y., Yamada, S.: Links between the Shock Instability in Core-collapse Supernovae and Asymmetric Accretions of Envelopes. ApJ831, 75 (2016) https://doi.org/10.3847/0004-637X/831/1/75 arXiv:1605.09524 [astro-ph.HE]

    Pith/arXiv arXiv 2016

  70. [70]

    MNRAS461, 112–116 (2016) https://doi.org/10.1093/mnrasl/ slw105 arXiv:1602.06759 [astro-ph.HE]

    Takiwaki, T., Kotake, K., Suwa, Y.: Three-dimensional simulations of rapidly rotating core-collapse supernovae: finding a neutrino-powered explosion aided by non- axisymmetric flows. MNRAS461, 112–116 (2016) https://doi.org/10.1093/mnrasl/ slw105 arXiv:1602.06759 [astro-ph.HE]

    Pith/arXiv arXiv 2016

  71. [71]

    ApJ794, 162 (2014) https://doi.org/10.1088/ 0004-637X/794/2/162 arXiv:1408.3503 [astro-ph.HE]

    Takahashi, K., Yamada, S.: Linear Analysis on the Growth of Non-spherical Perturba- tions in Supersonic Accretion Flows. ApJ794, 162 (2014) https://doi.org/10.1088/ 0004-637X/794/2/162 arXiv:1408.3503 [astro-ph.HE]

    Pith/arXiv arXiv 2014

  72. [72]

    MNRAS510(4), 4689–4705 (2022) https://doi.org/10.1093/mnras/stab3702 arXiv:2109.10920 [astro-ph.SR]

    Vartanyan, D., Coleman, M.S.B., Burrows, A.: The collapse and three- dimensional explosion of three-dimensional massive-star supernova progenitor mod- els. MNRAS510(4), 4689–4705 (2022) https://doi.org/10.1093/mnras/stab3702 arXiv:2109.10920 [astro-ph.SR]

    Pith/arXiv arXiv 2022

  73. [73]

    MNRAS504(1), 636–647 (2021) https://doi.org/10.1093/mnras/ stab883 arXiv:2101.00213 [astro-ph.SR]

    Varma, V., M¨ uller, B.: 3D simulations of oxygen shell burning with and without magnetic fields. MNRAS504(1), 636–647 (2021) https://doi.org/10.1093/mnras/ stab883 arXiv:2101.00213 [astro-ph.SR]

    Pith/arXiv arXiv 2021

  74. [74]

    Nature435(7039), 178–180 (2005) https://doi.org/10.1038/nature03515 arXiv:astro-ph/0503521 [astro-ph]

    Tueller, J.: A link between prompt optical and promptγ-ray emission inγ- ray bursts. Nature435(7039), 178–180 (2005) https://doi.org/10.1038/nature03515 arXiv:astro-ph/0503521 [astro-ph]

    Pith/arXiv arXiv 2005

  75. [75]

    Walk, L., Foglizzo, T., Tamborra, I.: Standing accretion shock instability in the collapse of a rotating stellar core. Phys. Rev. D107(6), 063014 (2023) https: //doi.org/10.1103/PhysRevD.107.063014 arXiv:2212.07467 [astro-ph.HE]

    Pith/arXiv arXiv 2023

  76. [76]

    ApJ637, 914 (2006) 25

    Woosley, S.E., Heger, A.: The Progenitor Stars of Gamma-Ray Bursts. ApJ637, 914 (2006) 25

    2006

  77. [77]

    Winteler, C., K¨ appeli, R., Perego, A., Arcones, A., Vasset, N., Nishimura, N., Liebend¨ orfer, M., Thielemann, F.-K.: Magnetorotationally Driven Supernovae as the Origin of Early Galaxy r-process Elements? ApJ750(1), 22 (2012) https: //doi.org/10.1088/2041-8205/750/1/L22 arXiv:1203.0616 [astro-ph.SR]

    Pith/arXiv arXiv 2012

  78. [78]

    ApJ679, 607 (2008)

    Yamasaki, T., Foglizzo, T.: Effect of Rotation on the Stability of a Stalled Cylindrical Shock and Its Consequences for Core-Collapse Supernovae. ApJ679, 607 (2008)

    2008

  79. [79]

    ApJ890(2), 94 (2020) https://doi.org/10.3847/1538-4357/ab66bb arXiv:1905.04378 [astro-ph.HE]

    Yadav, N., M¨ uller, B., Janka, H.T., Melson, T., Heger, A.: Large-scale Mixing in a Vio- lent Oxygen-Neon Shell Merger Prior to a Core-collapse Supernova. ApJ890(2), 94 (2020) https://doi.org/10.3847/1538-4357/ab66bb arXiv:1905.04378 [astro-ph.HE]

    Pith/arXiv arXiv 2020

  80. [80]

    MNRAS 506(1), 20–25 (2021) https://doi.org/10.1093/mnrasl/slab067 arXiv:2106.09909 [astro-ph.SR]

    Yoshida, T., Takiwaki, T., Aguilera-Dena, D.R., Kotake, K., Takahashi, K., Naka- mura, K., Umeda, H., Langer, N.: A three-dimensional hydrodynamics simulation of oxygen-shell burning in the final evolution of a fast-rotating massive star. MNRAS 506(1), 20–25 (2021) https://doi.org/10.1093/mnrasl/slab067 arXiv:2106.09909 [astro-ph.SR]

    Pith/arXiv arXiv 2021

Showing first 80 references.