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Influence of effective mass of the relativistic mean field theory on core collapse supernovae and compact objects

T0 review · 2 major / 4 minor · reviewed 2026-08-08 · deepseek-v4-flash

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Pith's one-line read In a relativistic framework, a larger nucleon effective mass softens the supernova equation of state, making proto-neutron stars denser and quicker to collapse into black holes.

desk verdict A solid, honest EOS sensitivity study from the Shen program; the larger-effective-mass table gives more compact PNSs and earlier black-hole collapse, though M* is not fully isolated from correlated vector-repulsion changes. read the letter →

arxiv 2608.05582 v1 pith:SGQP2PQC submitted 2026-08-06 astro-ph.HE nucl-th

Kohsuke Sumiyoshi , Hajime Togashi , Shun Furusawa , Shuying Li , Hong Shen , Ken'ichiro Nakazato , Hideyuki Suzuki This is my paper · ORCID
classification astro-ph.HEnucl-th
keywords effectivemassrelativisticmeanfieldtheorysupernovaequationofstatecore-collapsesupernovaeproto-neutronstarcoolingblackholeformationneutrinoemissionTM1mEOS
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 asks whether the nucleon effective mass changes the evolution of supernova cores and the neutrinos they emit, once the effective mass is computed self-consistently in the relativistic mean field theory rather than inserted only into a kinetic term. It compares two EOS tables, TM1e and TM1m, that share the same saturation density, incompressibility, symmetry energy, and symmetry-energy slope, but differ in the effective mass ratio ($M^*/M = 0.634$ vs $0.793$). The central finding is that the larger effective mass softens the high-density EOS, making proto-neutron stars more compact and, once compression dominates, hotter, so they reach the maximum supported mass and collapse to a black hole earlier. In the 40 solar mass S16 model the black hole forms at 0.64 s after bounce with TM1m, versus 1.03 s with TM1e, and the neutrino burst is shorter but more energetic. The paper also shows that the same physics lengthens proto-neutron star cooling and raises the luminosity and average energy of the emitted neutrinos, giving a distinct imprint in the supernova neutrino signal.

What carries the argument

The central object is the nucleon effective mass $M^*$ in the RMF theory, defined through the Dirac mass term generated by the scalar meson mean field. The comparison pair, TM1e and TM1m, is built so that $M^*$ differs while saturation properties match; the machinery is the self-consistent balance between scalar attraction and vector meson repulsion, which makes a larger $M^*$ simultaneously reduce pressure at intermediate densities and increase entropy per baryon at fixed temperature. This coupled change in stiffness and thermodynamics, rather than the kinetic term alone as in non-relativistic Skyrme-type models, drives the compact proto-neutron stars, earlier black hole collapse, and the altered neutrino signal.

What would settle it

Rerun the 40 solar mass black-hole-formation simulation with two RMF EOS tables that keep the vector mean-field potential identical at all densities while varying only the scalar coupling and hence $M^*$; if the black hole formation time does not move when $M^*$ changes under fixed vector repulsion, the claim that the effective mass drives the earlier collapse would be contradicted.

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Extended reading notes

Core claim

In a relativistic mean field description, a larger nucleon effective mass is not an independent stiffness parameter: it arises from a weaker scalar attraction, which also weakens the vector repulsion that supplies saturation, and together those changes soften the equation of state at densities around and above nuclear saturation. The paper demonstrates this by taking two RMF parametrizations with identical saturation properties except the effective mass and running general relativistic neutrino-radiation hydrodynamics for collapse, bounce, black hole formation, and proto-neutron star cooling. The result is that the TM1m EOS with $M^*/M=0.793$ supports a maximum proto-neutron star mass about 0.2 solar masses smaller than TM1e's, produces more compact proto-neutron stars with higher central density and, after compression dominates, higher temperature, and collapses the 40 solar mass S16 core to a black hole at 0.64 s after bounce instead of 1.03 s; the WW95 40 solar mass case gives 0.82 s versus 1.13 s. During cooling, the compact TM1m star traps neutrinos longer, so the antineutrino luminosity and average energy stay higher over tens of seconds.

Load-bearing premise

The two EOS tables are assumed to differ only in nucleon effective mass, so the dynamical differences are attributed to that mass; in the RMF theory, however, changing the effective mass also changes the scalar and vector mean-field potentials, so the role of the mass alone is not fully isolated.

Editorial extensions

If this is right

  • A larger effective mass lowers the maximum mass a hot proto-neutron star can support by about 0.2 solar masses relative to TM1e, so a given massive progenitor collapses to a black hole earlier.
  • Failed supernovae from 40 solar mass progenitors emit a shorter neutrino burst before black hole formation with a larger effective mass: 0.64 s versus 1.03 s after bounce in the S16 model, and 0.82 s versus 1.13 s in the WW95 model.
  • The same EOS softness makes the proto-neutron star more compact during cooling, keeping neutrino luminosity and average energy higher over tens of seconds, so the effective mass leaves an imprint on the late-time neutrino signal.
  • At early post-bounce times for 11.2 and 15 solar mass progenitors the differences are modest: the larger effective mass gives slightly higher central density and lower central temperature, while the bounce conditions and shock position stay close.

Reading between the lines

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

  • The causal role of $M^*$ is not fully isolated, because within RMF the effective mass and the vector repulsion change together, and the TM1m vector potential crosses and exceeds TM1e's above about 1.3 fm${}^{-3}$; part of the earlier black hole collapse could come from high-density vector repulsion rather than from $M^*$ itself.
  • If the neutrino imprint is as clear as these simulations suggest, a measured black-hole formation time from a future galactic failed-supernova neutrino burst could discriminate between effective masses, provided the progenitor and accretion history are known independently.
  • The same EOS pair in multi-dimensional simulations with convection and the standing accretion shock instability could change the explosion outcome, and the effective mass may also alter neutrino opacities beyond what is implemented in this study.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 4 minor

Summary. This paper investigates the influence of the nucleon effective mass in relativistic mean field (RMF) theory on core-collapse supernova dynamics and proto-neutron star (PNS) cooling. The authors use two published equation-of-state (EOS) tables, TM1e and TM1m, which share the same saturation properties but differ in effective mass (M*/M = 0.634 and 0.793, respectively). They perform one-dimensional general relativistic neutrino-radiation hydrodynamics simulations of gravitational collapse and bounce for 11.2, 15, and 40 solar-mass progenitors, and quasi-hydrostatic PNS cooling simulations. The main findings are that the larger effective mass (TM1m) yields a softer EOS below about 10^15 g/cm^3, leading to more compact PNSs, earlier black hole formation (0.64 s vs. 1.03 s after bounce for the 40 solar-mass S16 progenitor), and higher neutrino luminosities and average energies during PNS cooling. The differences are attributed to the effective mass through its effect on the scalar and vector mean-field potentials.

Significance. This is the first systematic RMF-based comparison of effective mass effects in supernova simulations, complementing earlier studies that used non-relativistic Skyrme-type EOS. The numerical setup follows established and validated algorithms, and the EOS tables are publicly available, which makes the results reproducible. The predicted differences in black hole formation times and neutrino signals are falsifiable with future observations, and the paper explicitly discusses the distinct role of the effective mass in relativistic frameworks. The main caveat, which the authors partially acknowledge, is the intrinsic correlation between the effective mass and the vector potential in RMF parameterizations; this is a point that needs clarification but does not overturn the central trend.

major comments (2)
  1. [Section IV, Fig. 2] The causal attribution of the early black-hole collapse and energetic neutrino emission to the 'softness' caused by the large effective mass is not fully isolated, because the TM1m and TM1e parameterizations also differ in the isoscalar-vector potential (Fig. 2). The authors should explicitly state that the crossing of the vector potentials at about 1.3 fm^-3 occurs above the central densities reached in the simulations (approximately 0.6 fm^-3 at 0.60 s for the 40 solar-mass S16 case, Fig. 8), so that the softening in the probed density range is indeed connected to the effective mass. A short decomposition of the pressure into kinetic, scalar, and vector contributions along the simulation trajectories would remove this ambiguity.
  2. [Section II B, Fig. 6] The maximum proto-neutron star mass sequence in Fig. 6 is computed under beta equilibrium without neutrinos, whereas the dynamical simulations that lead to black hole formation include trapped neutrinos and lepton fractions well above the beta-equilibrium value. The authors should clarify whether the approximately 0.2 solar mass difference between TM1m and TM1e persists under the lepton-rich conditions of the simulations, for example by evaluating the maximum mass along the actual simulation trajectories. This would make the interpretation of the collapse times more robust.
minor comments (4)
  1. [Abstract] The phrase 'high energy neutrinos in short burst from the black hole formation' in the abstract could be misread as a distinct burst with higher energies for the large-effective-mass model; the simulations actually show a truncation of the neutrino signal at earlier times. Consider rephrasing to 'earlier termination of the neutrino signal'.
  2. [Section III B] The initial models for the proto-neutron star cooling simulations are based on the entropy and electron fraction profiles from a simulation using the original TM1 EOS (Ref. [61]), not TM1e or TM1m. While the comparison between the two EOS is still meaningful because both use the same initial profiles, the authors should explicitly note this inconsistency and its possible effect on the early cooling evolution.
  3. [Fig. 8] In Fig. 8, the right panels show the effective mass profiles; adding a vertical line or label for the central density or the neutrinosphere radius would help the reader connect the density and temperature panels.
  4. [Section IV] The statement that 'the effective mass is not a simple parameter but a determining factor of the attraction' is somewhat vague; elaborating on the relation between M*, the scalar coupling, and the vector potential would make the summary more precise.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the simulations propagate externally fixed EOS tables and the neutrino signals are computed, not fitted.

full rationale

The paper's derivation chain is input-to-output: it adopts two fixed RMF EOS tables (TM1e and TM1m), solves general-relativistic neutrino-radiation hydrodynamics from stellar progenitor initial data, and reports the resulting collapse, black-hole formation, and cooling signals. No simulation output is fed back into the EOS construction, and no parameter is fitted to the reported neutrino luminosities or collapse times. The TM1m table is cited to the authors' prior publication [58], but that publication fixes the RMF couplings by nuclear saturation properties (K=281 MeV, Esym=31.4 MeV, L=40 MeV, M*/M=0.793 for TM1m) and does not include the supernova dynamics or neutrino signals that this paper claims to predict; hence the self-citation is data provenance rather than load-bearing circularity. The paper's own discussion that the effective mass is not a simple parameter and that the isoscalar-vector potential for TM1m overtakes TM1e above 1.3 fm^-3 is a limitation in isolating M* from correlated RMF potential changes, but that is a physical-confound issue, not an equation-level equivalence or a fitted-input-called-prediction.

Assumptions & free parameters 1 free parameters · 6 assumptions · 0 invented entities

The central claim rests on the RMF EOS construction (TM1e and TM1m), the neutrino transport and hydrodynamics codes, and the hybrid choice of a common low-density EOS. No new entities are invented. The main free parameter is the effective mass ratio difference between the two tables, a chosen EOS input rather than a fitted outcome.

free parameters (1)
  • Effective nucleon mass ratio M*/M = 0.793 (TM1m), 0.634 (TM1e)
    The central variable of the study. It is chosen in the EOS construction by adjusting the scalar meson coupling (Li et al. 2025); it is an input, not an output, of the simulations.
assumptions (6)
  • standard math General relativity and the Boltzmann neutrino transport equations describe the collapse and cooling dynamics.
    Used as governing equations in Sections III A and III B via established codes from refs [25, 52, 53].
  • domain assumption The RMF Lagrangian with nonlinear sigma and omega meson terms is a valid description of dense matter.
    The TM1e and TM1m tables are generated in this framework [58, 59]; the paper does not test this model against alternatives.
  • domain assumption Interpolation within each EOS table is accurate over the simulated density, temperature, and Ye range.
    No interpolation errors or resolution studies are provided; grid sizes are stated but not tested.
  • domain assumption Spherical symmetry and quasi-hydrostatic evolution are sufficient for PNS cooling and black hole formation.
    All simulations are one-dimensional; Section IV states multi-dimensional dynamics are left for future work.
  • ad hoc to paper Using the TM1e EOS for non-uniform matter below 10^14 g/cm^3 for both models isolates the high-density effective mass effect.
    Stated in Sections II and III as common use of the TM1e table for non-uniform matter; the hybrid choice is acknowledged as a limitation in Section IV.
  • domain assumption Standard weak interaction rates with only partial effective mass dependence are adequate.
    Section III A describes the standard rate set; Section IV admits the effective mass dependence in reaction rates is only partly implemented.

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Cite this review

Pith. "Pith review of Influence of effective mass of the relativistic mean field theory on core collapse supernovae and compact objects." pith.science (2026). https://pith.science/paper/SGQP2PQC

@misc{pith2026260805582,
  author       = {Pith},
  title        = {Pith review of: Influence of effective mass of the relativistic mean field theory on core collapse supernovae and compact objects},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/SGQP2PQC}},
  note         = {Machine review of arXiv:2608.05582}
}
read the original abstract

We study the influence of the effective mass in the relativistic mean field (RMF) theory on the properties of the central core of collapse-driven supernovae and the formation of compact objects. Influence of the effective mass has been so far studied within the non-relativistic frameworks. In order to clarify the role of the effective mass in the relativistic frameworks, which is different from non-relativistic ones, we adopt the set of equation of state (EOS) tables using the parameterizations TM1e and TM1m, which have different effective masses but with the same saturation properties, in the RMF theory. We show that choices of the effective mass in supernova matter affect both the stiffness of the EOS through pressure and the thermodynamical behavior through temperature under the RMF frameworks. We explore differences in matter evolution with neutrino emissions by performing a set of numerical simulations of the gravitational collapse and bounce of massive stars and the cooling of the proto-neutron stars. The EOS with large effective mass leads to compact proto-neutron stars and early collapse to black holes with high densities and temperatures due to the softness. It leads to high energy neutrinos in long emission from the proto-neutron star cooling and in short burst from the black hole formation.

Figures

Figures reproduced from arXiv: 2608.05582 by the authors.

Figure 1
Figure 1. FIG. 1. Properties of uniform matter of nucleons in the cases of TM1m (red, solid) and TM1e [PITH_FULL_IMAGE:figures/full_fig_p007_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2. Mean field potentials of neutron matter ( [PITH_FULL_IMAGE:figures/full_fig_p009_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3. The pressure of cold neutron star matter in the cases of TM1m (red, solid) and TM1e [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figures from the paper (9 more)
Figure 4
Figure 4. Figure 4: FIG. 4. The mass-radius relations in the case of TM1m (red, solid) and TM1e (blue, dashed) are [PITH_FULL_IMAGE:figures/full_fig_p010_4.png]
Figure 5
Figure 5. Figure 5: FIG. 5. Thermodynamical quantities of the hot and dense matter in the case of TM1m (red, [PITH_FULL_IMAGE:figures/full_fig_p011_5.png]
Figure 6
Figure 6. Figure 6: FIG. 6. Maximum mass of the proto-neutron stars evaluated by adopting hot and dense matter [PITH_FULL_IMAGE:figures/full_fig_p012_6.png]
Figure 7
Figure 7. Figure 7: FIG. 7. Profiles of the mass density, temperature, and effective mass are shown as functions of [PITH_FULL_IMAGE:figures/full_fig_p014_7.png]
Figure 8
Figure 8. Figure 8: FIG. 8. Profiles of supernova cores at 0.30 and 0.60 s after the core bounce from the massive star [PITH_FULL_IMAGE:figures/full_fig_p015_8.png]
Figure 9
Figure 9. Figure 9: FIG. 9. The average energies of neutrinos emitted from the collapse of 40M [PITH_FULL_IMAGE:figures/full_fig_p016_9.png]
Figure 7
Figure 7. Figure 7: The density and temperature become high due to compression at 10 s and thermal [PITH_FULL_IMAGE:figures/full_fig_p017_7.png]
Figure 10
Figure 10. Figure 10: FIG. 10. Profiles of the proto-neutron stars at 0, 10, and 50 s in the numerical simulations of [PITH_FULL_IMAGE:figures/full_fig_p018_10.png]
Figure 11
Figure 11. Figure 11: FIG. 11. Time evolution of neutrino emission from the proto-neutron stars in the numerical [PITH_FULL_IMAGE:figures/full_fig_p019_11.png]

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Works this paper leans on

79 extracted references · 38 canonical work pages

  1. [1]

    We show in Fig

    Post bounce evolution In order to examine the influence of the effective mass on the properties of supernova core at and after the core bounce, we follow the time evolution of the collapse and bounce of massive stars of 11.2M⊙ by WHW02 and 15M⊙ by WW95 until 0.30 s after the core bounce (0 s). We show in Fig. 7 the snapshots of the central core for the mo...

    work page

  2. [2]

    After the core bounce, the shock wave stalls and recedes as a result of intense mass accretion

    Black hole formation In order to examine the influence of the effective mass on the dynamics and neutrino signals for non-explosion cases, we follow the time evolution of the collapse and bounce of massive stars of 40M ⊙ up to the dynamical collapse to the black hole formation. After the core bounce, the shock wave stalls and recedes as a result of intens...

    work page

  3. [3]

    H. A. Bethe, Supernova mechanisms, Reviews of Modern Physics62, 801 (1990)

    1990

  4. [4]

    H. A. Bethe and J. R. Wilson, Revival of a stalled supernova shock by neutrino heating, ApJ 295, 14 (1985)

    work page 1985

  5. [5]

    Oertel, M

    M. Oertel, M. Hempel, T. Kl¨ ahn, and S. Typel, Equations of state for supernovae and compact stars, Reviews of Modern Physics89, 015007 (2017), arXiv:1610.03361 [astro-ph.HE]

    arXiv 2017

  6. [6]

    Equation of state in neutron stars and supernovae

    K. Sumiyoshi, T. Kojo, and S. Furusawa, Equation of state in neutron stars and supernovae, Handbook of Nuclear Physics, Springer , 3127 (2023), arXiv:2207.00033 [nucl-th]

    work page Pith review arXiv 2023

  7. [7]

    K. Kotake, Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae, Comptes Rendus Physique14, 318 (2013), arXiv:1110.5107 [astro- 21 ph.HE]

    arXiv 2013

  8. [8]

    Janka, T

    H.-T. Janka, T. Melson, and A. Summa, Physics of Core-Collapse Supernovae in Three Di- mensions: A Sneak Preview, Annual Review of Nuclear and Particle Science66, 341 (2016), arXiv:1602.05576 [astro-ph.SR]

    arXiv 2016

Show all 79 references
  1. [9]

    Janka, Explosion Mechanisms of Core-Collapse Supernovae, Annual Review of Nuclear and Particle Science62, 407 (2012), arXiv:1206.2503 [astro-ph.SR]

    H.-T. Janka, Explosion Mechanisms of Core-Collapse Supernovae, Annual Review of Nuclear and Particle Science62, 407 (2012), arXiv:1206.2503 [astro-ph.SR]

    2012 arXiv

  2. [10]

    Burrows, Colloquium: Perspectives on core-collapse supernova theory, Reviews of Modern Physics85, 245 (2013), arXiv:1210.4921 [astro-ph.SR]

    A. Burrows, Colloquium: Perspectives on core-collapse supernova theory, Reviews of Modern Physics85, 245 (2013), arXiv:1210.4921 [astro-ph.SR]

    2013 arXiv

  3. [11]

    in various ways, but its influence on the explosion dynamics has not yet been fully clari- fied. As a general tendency, the softness of EOS leads to a favorable condition to have more neutrino heating for the explosion, since neutrino emission is enhanced in the compression of...

  4. [12]

    J. M. Lattimer, Neutron Stars and the Nuclear Matter Equation of State, Annual Review of Nuclear and Particle Science71, 433 (2021)

    2021

  5. [13]

    Janka, Neutrino-Driven Explosions, inHandbook of Supernovae, ISBN 978-3-319-21845-

    H.-T. Janka, Neutrino-Driven Explosions, inHandbook of Supernovae, ISBN 978-3-319-21845-

  6. [14]

    1095(Springer, 2017) p

    Springer International Publishing AG, 2017, p. 1095(Springer, 2017) p. 1095

    2017

  7. [15]

    H.-T. Janka, Long-Term Multidimensional Models of Core-Collapse Supernovae: Progress and Challenges, Annual Review of Nuclear and Particle Science75, 425 (2025), arXiv:2502.14836 [astro-ph.HE]

    2025

  8. [16]

    Janka and A

    H.-T. Janka and A. Bauswein, Dynamics and Equation of State Dependencies of Relevance for Nucleosynthesis in Supernovae and Neutron Star Mergers,Handbook of Nuclear Physics, Springer , 4005 (2023), arXiv:2212.07498 [astro-ph.HE]

    2023 arXiv

  9. [17]

    M¨ uller, Neutrino Emission as Diagnostics of Core-Collapse Supernovae, Annual Review of Nuclear and Particle Science69, 253 (2019), arXiv:1904.11067 [astro-ph.HE]

    B. M¨ uller, Neutrino Emission as Diagnostics of Core-Collapse Supernovae, Annual Review of Nuclear and Particle Science69, 253 (2019), arXiv:1904.11067 [astro-ph.HE]

    2019 arXiv

  10. [18]

    G. F. Burgio, H. J. Schulze, I. Vida˜ na, and J. B. Wei, Neutron stars and the nuclear equation of state, Progress in Particle and Nuclear Physics120, 103879 (2021), arXiv:2105.03747 [nucl- th]

    2021 arXiv

  11. [19]

    Chatziioannou, H

    K. Chatziioannou, H. T. Cromartie, S. Gandolfi, I. Tews, D. Radice, A. W. Steiner, and A. L. Watts, Neutron stars and the dense matter equation of state, Reviews of Modern Physics97, 045007 (2025), arXiv:2407.11153 [nucl-th]

    2025

  12. [20]

    Kotake, K

    K. Kotake, K. Sato, and K. Takahashi, Explosion mechanism, neutrino burst and gravitational wave in core-collapse supernovae, Reports on Progress in Physics69, 971 (2006), arXiv:astro- ph/0509456 [astro-ph]

    2006

  13. [21]

    Mirizzi, I

    A. Mirizzi, I. Tamborra, H.-T. Janka, N. Saviano, K. Scholberg, R. Bollig, L. H¨ udepohl, and S. Chakraborty, Supernova neutrinos: production, oscillations and detection, Nuovo Cimento Rivista Serie39, 1 (2016), arXiv:1508.00785 [astro-ph.HE]

    2016 arXiv

  14. [22]

    Takahara and K

    M. Takahara and K. Sato, Supernova Explosions and the Soft Equation of State, ApJ335, 301 (1988)

    1988

  15. [23]

    Abdikamalov, G

    E. Abdikamalov, G. Pagliaroli, and D. Radice, Gravitational Waves from Core-Collapse Su- pernovae, arXiv e-prints , arXiv:2010.04356 (2020), arXiv:2010.04356 [astro-ph.SR]

    2020 arXiv

  16. [24]

    B. M¨ uller, Core-Collapse Supernovae and their Gravitational Wave Signals: The Status of The- 22 ory and Modeling, arXiv e-prints , arXiv:2603.24243 (2026), arXiv:2603.24243 [astro-ph.HE]

    2026 arXiv

  17. [25]

    Sotani, Understanding supernova gravitational waves with protoneutron star asteroseis- mology, Classical and Quantum Gravity43, 093001 (2026)

    H. Sotani, Understanding supernova gravitational waves with protoneutron star asteroseis- mology, Classical and Quantum Gravity43, 093001 (2026)

    2026

  18. [26]

    Baron, J

    E. Baron, J. Cooperstein, and S. Kahana, Type II supernovae in 12M ⊙ and 15M⊙ stars: The equation of state and general relativity, Phys. Rev. Lett.55, 126 (1985)

    1985

  19. [27]

    A. W. Steiner, M. Hempel, and T. Fischer, Core-collapse Supernova Equations of State Based on Neutron Star Observations, ApJ774, 17 (2013), arXiv:1207.2184 [astro-ph.SR]

    2013 arXiv

  20. [28]

    F. D. Swesty, J. M. Lattimer, and E. S. Myra, The Role of the Equation of State in the “Prompt” Phase of Type II Supernovae, ApJ425, 195 (1994)

    1994

  21. [29]

    T. A. Thompson, A. Burrows, and P. A. Pinto, Shock Breakout in Core-Collapse Supernovae and Its Neutrino Signature, ApJ592, 434 (2003), arXiv:astro-ph/0211194 [astro-ph]

    2003 arXiv

  22. [30]

    Sumiyoshi, S

    K. Sumiyoshi, S. Yamada, H. Suzuki, H. Shen, S. Chiba, and H. Toki, Postbounce Evolution of Core-Collapse Supernovae: Long-Term Effects of the Equation of State, ApJ629, 922 (2005), arXiv:astro-ph/0506620 [astro-ph]

    2005 arXiv

  23. [31]

    Fischer, I

    T. Fischer, I. Sagert, G. Pagliara, M. Hempel, J. Schaffner-Bielich, T. Rauscher, F. K. Thiele- mann, R. K¨ appeli, G. Mart ´ ınez-Pinedo, and M. Liebend¨ orfer, Core-collapse Supernova Explo- sions Triggered by a Quark-Hadron Phase Transition During the Early Post-bounce Phas...

    2011 arXiv

  24. [32]

    Richers, C

    S. Richers, C. D. Ott, E. Abdikamalov, E. O’Connor, and C. Sullivan, Equation of state effects on gravitational waves from rotating core collapse, Phys. Rev. D95, 063019 (2017), arXiv:1701.02752 [astro-ph.HE]

    2017 arXiv

  25. [33]

    Marek, H

    A. Marek, H. T. Janka, and E. M¨ uller, Equation-of-state dependent features in shock- oscillation modulated neutrino and gravitational-wave signals from supernovae, A&A496, 475 (2009), arXiv:0808.4136 [astro-ph]

    2009 arXiv

  26. [34]

    Y. Suwa, T. Takiwaki, K. Kotake, T. Fischer, M. Liebend¨ orfer, and K. Sato, On the Impor- tance of the Equation of State for the Neutrino-driven Supernova Explosion Mechanism, ApJ 764, 99 (2013), arXiv:1206.6101 [astro-ph.HE]

    2013 arXiv

  27. [35]

    S. M. Couch, The Dependence of the Neutrino Mechanism of Core-collapse Supernovae on the Equation of State, ApJ765, 29 (2013), arXiv:1206.4724 [astro-ph.HE]

    2013 arXiv

  28. [36]

    Fischer, M

    T. Fischer, M. Hempel, I. Sagert, Y. Suwa, and J. Schaffner-Bielich, Symmetry energy im- pact in simulations of core-collapse supernovae, European Physical Journal A50, 46 (2014), arXiv:1307.6190 [astro-ph.HE]. 23

    2014 arXiv

  29. [37]

    Eggenberger Andersen, S

    O. Eggenberger Andersen, S. Zha, A. da Silva Schneider, A. Betranhandy, S. M. Couch, and E. P. O’Connor, Equation-of-state Dependence of Gravitational Waves in Core-collapse Supernovae, ApJ923, 201 (2021), arXiv:2106.09734 [astro-ph.HE]

    2021 arXiv

  30. [38]

    Burrows, D

    A. Burrows, D. Vartanyan, J. C. Dolence, M. A. Skinner, and D. Radice, Crucial Physical Dependencies of the Core-Collapse Supernova Mechanism, Space Sci. Rev.214, 33 (2018), arXiv:1611.05859 [astro-ph.SR]

    2018 arXiv

  31. [39]

    Nagakura, W

    H. Nagakura, W. Iwakami, S. Furusawa, H. Okawa, A. Harada, K. Sumiyoshi, S. Yamada, H. Matsufuru, and A. Imakura, Simulations of Core-collapse Supernovae in Spatial Axisymme- try with Full Boltzmann Neutrino Transport, ApJ854, 136 (2018), arXiv:1702.01752 [astro- ph.HE]

    2018 arXiv

  32. [40]

    Harada, H

    A. Harada, H. Nagakura, W. Iwakami, H. Okawa, S. Furusawa, H. Matsufuru, K. Sumiyoshi, and S. Yamada, On the Neutrino Distributions in Phase Space for the Rotating Core-collapse Supernova Simulated with a Boltzmann-neutrino-radiation-hydrodynamics Code, ApJ872, 181 (2019), arX...

    2019 arXiv

  33. [41]

    A. S. Schneider, L. F. Roberts, C. D. Ott, and E. O’Connor, Equation of state effects in the core collapse of a 20 -M ⊙ star, Phys. Rev. C100, 055802 (2019), arXiv:1906.02009 [astro- ph.HE]

    2019 arXiv

  34. [42]

    Sumiyoshi, S

    K. Sumiyoshi, S. Yamada, and H. Suzuki, Dynamics and Neutrino Signal of Black Hole For- mation in Nonrotating Failed Supernovae. I. Equation of State Dependence, ApJ667, 382 (2007), arXiv:0706.3762 [astro-ph]

    2007 arXiv

  35. [43]

    Boccioli, G

    L. Boccioli, G. J. Mathews, I.-S. Suh, and E. P. O’Connor, Effect of the Nuclear Equation of State on Relativistic Turbulence-induced Core-collapse Supernovae, ApJ926, 147 (2022), arXiv:2110.05544 [astro-ph.HE]

    2022 arXiv

  36. [44]

    Powell and B

    J. Powell and B. M¨ uller, Impact of the nuclear equation of state on the explodability of massive stars, arXiv e-prints , arXiv:2510.20076 (2025), arXiv:2510.20076 [astro-ph.HE]

    2025 arXiv

  37. [45]

    Rusakov, A

    A. Rusakov, A. Burrows, T. Wang, and D. Vartanyan, An Exploration of the Equation of State Dependence of Core-collapse Supernova Explosion Outcomes and Signatures, ApJ1003, 40 (2026), arXiv:2602.09025 [astro-ph.HE]

    2026 arXiv

  38. [46]

    Sumiyoshi, S

    K. Sumiyoshi, S. Yamada, H. Suzuki, and S. Chiba, Neutrino Signals from the Formation of a Black Hole: A Probe of the Equation of State of Dense Matter, Phys. Rev. Lett.97, 091101 (2006), arXiv:astro-ph/0608509 [astro-ph]. 24

    2006 arXiv

  39. [47]

    Eggenberger Andersen, E

    O. Eggenberger Andersen, E. O’Connor, H. Andresen, A. da Silva Schneider, and S. M. Couch, Black Hole Supernovae, Their Equation of State Dependence, and Ejecta Composition, ApJ 980, 53 (2025), arXiv:2411.11969 [astro-ph.HE]

    2025 arXiv

  40. [48]

    O’Connor and C

    E. O’Connor and C. D. Ott, Black Hole Formation in Failing Core-Collapse Supernovae, ApJ 730, 70 (2011), arXiv:1010.5550 [astro-ph.HE]

    2011 arXiv

  41. [49]

    P. Char, S. Banik, and D. Bandyopadhyay, A Comparative Study of Hyperon Equations of State in Supernova Simulations, ApJ809, 116 (2015), arXiv:1508.01854 [astro-ph.HE]

    2015 arXiv

  42. [50]

    K.-C. Pan, M. Liebend¨ orfer, S. M. Couch, and F.-K. Thielemann, Equation of State Dependent Dynamics and Multi-messenger Signals from Stellar-mass Black Hole Formation, ApJ857, 13 (2018), arXiv:1710.01690 [astro-ph.HE]

    2018 arXiv

  43. [51]

    da Silva Schneider, E

    A. da Silva Schneider, E. O’Connor, E. Granqvist, A. Betranhandy, and S. M. Couch, Equation of State and Progenitor Dependence of Stellar-mass Black Hole Formation, ApJ894, 4 (2020), arXiv:2001.10434 [astro-ph.HE]

    2020 arXiv

  44. [52]

    Suzuki, inPhysics and Astrophysics of Neutrinos, edited by M

    H. Suzuki, inPhysics and Astrophysics of Neutrinos, edited by M. Fukugita and A. Suzuki (Springer-Verlag, Tokyo, 1994) p. 763

    1994

  45. [53]

    Yasin, S

    H. Yasin, S. Sch¨ afer, A. Arcones, and A. Schwenk, Equation of State Effects in Core-Collapse Supernovae, Phys. Rev. Lett.124, 092701 (2020)

    2020

  46. [54]

    A. S. Schneider, C. Constantinou, B. Muccioli, and M. Prakash, The APR equation of state for simulations of supernovae, neutron stars and binary mergers, arXiv e-prints , arXiv:1901.09652 (2019), arXiv:1901.09652 [nucl-th]

    2019 arXiv

  47. [55]

    Togashi, D

    H. Togashi, D. Sen, H. Gil, and C. H. Hyun, Influence of the Effective Mass on the Prop- erties of Nuclear Matter at Finite Density and Temperature, Symmetry17, 445 (2025), arXiv:2503.13963 [nucl-th]

    2025 arXiv

  48. [56]

    Burrows and J

    A. Burrows and J. M. Lattimer, The Birth of Neutron Stars, ApJ307, 178 (1986)

    1986

  49. [57]

    Nakazato and H

    K. Nakazato and H. Suzuki, Cooling Timescale for Protoneutron Stars and Properties of Nuclear Matter: Effective Mass and Symmetry Energy at High Densities, ApJ878, 25 (2019), arXiv:1905.00014 [astro-ph.HE]

    2019 arXiv

  50. [58]

    Sumiyoshi, H

    K. Sumiyoshi, H. Suzuki, and H. Toki, Influence of the symmetry energy on the birth of neutron stars and supernova neutrinos., A&A303, 475 (1995), arXiv:astro-ph/9506024 [astro-ph]

    1995 arXiv

  51. [59]

    J. A. Pons, S. Reddy, M. Prakash, J. M. Lattimer, and J. A. Miralles, Evolution of Proto- Neutron Stars, ApJ513, 780 (1999), arXiv:astro-ph/9807040 [astro-ph]. 25

    1999 arXiv

  52. [60]

    L. F. Roberts, G. Shen, V. Cirigliano, J. A. Pons, S. Reddy, and S. E. Woosley, Protoneutron Star Cooling with Convection: The Effect of the Symmetry Energy, Phys. Rev. Lett.108, 061103 (2012), arXiv:1112.0335 [astro-ph.HE]

    2012 arXiv

  53. [61]

    Nakazato, K

    K. Nakazato, K. Sumiyoshi, H. Suzuki, T. Totani, H. Umeda, and S. Yamada, Supernova Neutrino Light Curves and Spectra for Various Progenitor Stars: From Core Collapse to Proto-neutron Star Cooling, ApJS205, 2 (2013), arXiv:1210.6841 [astro-ph.HE]

    2013 arXiv

  54. [62]

    H. Shen, H. Toki, K. Oyamatsu, and K. Sumiyoshi, Relativistic Equation of State of Nuclear Matter for Supernova Explosion, Progress of Theoretical Physics100, 1013 (1998), arXiv:nucl- th/9806095

    1998

  55. [63]

    S. Li, J. Pang, H. Shen, J. Hu, and K. Sumiyoshi, Influence of Effective Nucleon Mass on Equation of State for Supernova Simulations and Neutron Stars, ApJ980, 54 (2025), arXiv:2407.18739 [nucl-th]

    2025 arXiv

  56. [64]

    H. Shen, F. Ji, J. Hu, and K. Sumiyoshi, Effects of Symmetry Energy on the Equation of State for Simulations of Core-collapse Supernovae and Neutron-star Mergers, ApJ891, 148 (2020), arXiv:2001.10143 [nucl-th]

    2020 arXiv

  57. [65]

    H. Shen, H. Toki, K. Oyamatsu, and K. Sumiyoshi, Relativistic Equation of State for Core- collapse Supernova Simulations, ApJS197, 20 (2011), arXiv:1105.1666 [astro-ph.HE]

    2011 arXiv

  58. [66]

    nucleons, electrons, positrons, and photons by adding the lepton and photon contributions to the nuclear contributions for pressure, energy, and entropy

    (brown) and PSR J0740 +6620 [67] (magenta). nucleons, electrons, positrons, and photons by adding the lepton and photon contributions to the nuclear contributions for pressure, energy, and entropy. We set the condition of the supernova matter by fixing the entropy per baryon,S...

  59. [67]

    H. Shen, H. Toki, K. Oyamatsu, and K. Sumiyoshi, Relativistic equation of state of nu- clear matter for supernova and neutron star, Nuclear Physics A637, 435 (1998), arXiv:nucl- th/9805035

    1998

  60. [68]

    Sumiyoshi, K

    K. Sumiyoshi, K. Nakazato, H. Suzuki, J. Hu, and H. Shen, Influence of Density Dependence of Symmetry Energy in Hot and Dense Matter for Supernova Simulations, ApJ887, 110 (2019), arXiv:1908.02928 [astro-ph.HE]

    2019 arXiv

  61. [69]

    Sugahara and H

    Y. Sugahara and H. Toki, Relativistic mean-field theory for unstable nuclei with non-linearσ andωterms, Nucl. Phys. A579, 557 (1994)

    1994

  62. [70]

    B. P. Abbott, R. Abbott, T. D. Abbott, F. Acernese, K. Ackley, C. Adams, T. Adams, P. Addesso, R. X. Adhikari, and V. B. Adya, GW170817: Measurements of Neutron Star Radii and Equation of State, Phys. Rev. Lett.121, 161101 (2018), arXiv:1805.11581 [gr-qc]. 26

    2018 arXiv

  63. [71]

    T. E. Riley, A. L. Watts, S. Bogdanov, P. S. Ray, R. M. Ludlam, S. Guillot, Z. Arzoumanian, C. L. Baker, A. V. Bilous, D. Chakrabarty, K. C. Gendreau, A. K. Harding, W. C. G. Ho, J. M. Lattimer, S. M. Morsink, and T. E. Strohmayer, A NICER View of PSR J0030+0451: Millisecond P...

    2019 arXiv

  64. [72]

    T. E. Riley, A. L. Watts, P. S. Ray, S. Bogdanov, S. Guillot, S. M. Morsink, A. V. Bilous, Z. Arzoumanian, D. Choudhury, J. S. Deneva, K. C. Gendreau, A. K. Harding, W. C. G. Ho, J. M. Lattimer, M. Loewenstein, R. M. Ludlam, C. B. Markwardt, T. Okajima, C. Prescod- Weinstein, ...

    2021 arXiv

  65. [73]

    S. E. Woosley, A. Heger, and T. A. Weaver, The evolution and explosion of massive stars, Reviews of Modern Physics74, 1015 (2002)

    2002

  66. [74]

    S. E. Woosley and T. A. Weaver, The Evolution and Explosion of Massive Stars. II. Explosive Hydrodynamics and Nucleosynthesis, ApJS101, 181 (1995)

    1995

  67. [75]

    Sukhbold, T

    T. Sukhbold, T. Ertl, S. E. Woosley, J. M. Brown, and H.-T. Janka, Core-collapse Supernovae from 9 to 120 Solar Masses Based on Neutrino-powered Explosions, ApJ821, 38 (2016), arXiv:1510.04643 [astro-ph.HE]

    2016 arXiv

  68. [76]

    Sumiyoshi, S

    K. Sumiyoshi, S. Furusawa, H. Nagakura, A. Harada, H. Togashi, K. Nakazato, and H. Suzuki, Effects of nuclear matter and composition in core-collapse supernovae and long-term proto- neutron star cooling, Progress of Theoretical and Experimental Physics2023, 013E02 (2023), arXi...

    2023 arXiv

  69. [77]

    Nakazato, H

    K. Nakazato, H. Suzuki, and H. Togashi, Heavy nuclei as thermal insulation for protoneutron stars, Phys. Rev. C97, 035804 (2018), arXiv:1710.10441 [astro-ph.HE]

    2018 arXiv

  70. [78]

    Nakazato and H

    K. Nakazato and H. Suzuki, A New Approach to the Mass and Radius of Neutron Stars with Supernova Neutrinos, ApJ891, 156 (2020), arXiv:2002.03300 [astro-ph.HE]

    2020 arXiv

  71. [79]

    Nakazato, F

    K. Nakazato, F. Nakanishi, M. Harada, Y. Koshio, Y. Suwa, K. Sumiyoshi, A. Harada, M. Mori, and R. A. Wendell, Observing Supernova Neutrino Light Curves with Super- Kamiokande. II. Impact of the Nuclear Equation of State, ApJ925, 98 (2022), arXiv:2108.03009 [astro-ph.HE]. 27

    2022 arXiv

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