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arxiv: 1906.09553 · v2 · pith:Z7XAJK33new · submitted 2019-06-23 · 🌌 astro-ph.SR · astro-ph.HE

The impact of asymmetric neutrino emissions on nucleosynthesis in core-collapse supernovae

Shin-ichiro Fujimoto , Hiroki Nagakura This is my paper

Pith reviewed 2026-05-25 18:02 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.HE
keywords core-collapse supernovaeneutrino emissionsnucleosynthesisasymmetric emissionsneutron-rich ejectasupernova remnantsheavy elementselectron fraction
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The pith

Asymmetric neutrino emissions above 30 percent produce excess heavy elements heavier than zinc in core-collapse supernovae, implying an upper limit on such asymmetry.

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

The paper examines how differences in neutrino emissions between hemispheres alter the electron fraction in supernova ejecta and the resulting element production. Higher electron neutrino output in one direction creates proton-rich material while the opposite direction yields neutron-rich matter. At asymmetry levels of 30 percent or higher, the neutron-rich regions overproduce elements beyond zinc compared with solar ratios. Elements lighter than calcium show little sensitivity to the asymmetry, but zinc and germanium yields rise even at smaller asymmetry values of 10 percent or less. These patterns could link to observed element distributions and neutron star motions in supernova remnants.

Core claim

Asymmetric neutrino emissions in neutrino-driven core-collapse supernovae yield proton-rich ejecta with electron fraction Ye greater than 0.51 in the hemisphere of stronger electron neutrino emission and neutron-rich ejecta with Ye less than 0.49 in the opposite hemisphere of stronger antineutrino emission. For asymmetry percentages of 30 or greater, the neutron-rich ejecta overproduces elements heavier than zinc relative to solar abundances, which may establish an upper bound on allowable asymmetry in such explosions. Abundances below calcium remain largely unchanged while zinc and germanium production increases in neutron-rich material even for asymmetries of 10 percent or less.

What carries the argument

The imposed percentage asymmetry in neutrino emissions between hemispheres, which shifts the electron fraction Ye of the ejected material and thereby changes nucleosynthesis pathways in the neutron-rich versus proton-rich sides.

If this is right

  • Elements lighter than calcium maintain abundances insensitive to the level of neutrino asymmetry.
  • Zinc and germanium yields increase in neutron-rich ejecta even at asymmetry levels of 10 percent or below.
  • The results may account for observed anticorrelations between heavy-element asymmetries and neutron-star kicks in supernova remnants.
  • Direct measurements of alpha elements, iron, zinc, and germanium distributions in remnants could constrain the degree of neutrino asymmetry.

Where Pith is reading between the lines

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

  • If confirmed, the 30 percent threshold would restrict the range of viable neutrino-driven explosion models that rely on strong directional neutrino emission differences.
  • The predicted hemispheric contrasts in zinc and germanium could be tested against abundance maps from future high-resolution remnant observations.
  • The insensitivity of lighter elements might allow their use as a baseline to isolate asymmetry effects in multi-messenger supernova data.

Load-bearing premise

The nucleosynthesis results for different imposed asymmetry levels accurately reflect the true hydrodynamic and neutrino transport behavior without large modeling errors.

What would settle it

Detection of supernova remnants in which regions with neutron-rich signatures show no excess of elements heavier than zinc, or in which zinc and germanium distributions lack the predicted hemispheric contrast even when other indicators suggest asymmetry greater than 30 percent.

Figures

Figures reproduced from arXiv: 1906.09553 by Hiroki Nagakura, Shin-ichiro Fujimoto.

Figure 1
Figure 1. Figure 1: Schematic picture of CCSN explosion with asymmetric νe and ¯νe emission. The asymmetry leads to the compositional differences in SN ejecta, which become n(p)-rich in the high-νe (high-¯νe) hemisphere due to the enhancement of νe (¯νe) and the decline of ¯νe (νe). of 19.4M⊙ up to ∼ 1.2s after the core bounce, in which shock fronts for all models have reached to a layer with r = 10, 000 km in almost all dire… view at source ↗
Figure 2
Figure 2. Figure 2: Evolution of average shock radius, rsh, for cases with masy = 0%(solid line), 10/3%(dashed line), 10%(dotted line), 30%(dash-dotted line), and 50%(double dotted line) as a func￾tion of the time from the core bounce tpb. previous study (Fujimoto et al. 2011), we checked the sen￾sitivity of nuclear abundances to the particle numbers, and found that the difference of the ejected mass of heavy nuclei between 3… view at source ↗
Figure 3
Figure 3. Figure 3: Mass profiles of dMej in Ye,1 of the inner ejecta (rcc 6 10, 000 km) for cases with masy = 0%, 10/3%, 10%, 30%, and 50% in panels from top to bottom, respectively. the excess of νe or ¯νe absorptions by asymmetric neutrino emissions [PITH_FULL_IMAGE:figures/full_fig_p003_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: [X/Fe] of all ejecta for cases with masy = 0%, 10/3%, 10%, 30%, and 50% in panels from top to bottom. Cases with large asymmetry (masy = 30% (fourth panel) and 50% (bottom panel)), produce too much elements with Z > 30. 1.5 1.0 0.5 0 -0.5 -1.0 -1.5 [X/Fe] C N O F Ne Na Mg Al Si P S Cl Ar K Ca Sc Ti V Cr Mn Fe Co Ni Cu Zn Ga Ge As Se Br Kr Rb Sr Y Zr Nb Mo Tc Ru Rh 1.0 0.5 0 -0.5 -1.0 -1.5 [X/Fe] C N O F Ne… view at source ↗
Figure 5
Figure 5. Figure 5: [X/Fe] of ejecta in the high-νe (solid lines) and high-¯νe (dotted lines) hemispheres for masy = 0% (top), 10/3% (middle), and 10% (bottom). Compositional differences between the high￾νe and high-¯νe hemispheres are prominent for Sc and elements with Z > 29 for cases of aspherical ν emission. abundantly produced in the ejecta with some overproduc￾tion of elements (Z = 34-37 and 40), while models with large… view at source ↗
read the original abstract

We investigate the impact of asymmetric neutrino emissions on the explosive nucleosynthesis in neutrino-driven core-collapse supernovae (CCSNe). We find that the asymmetric emissions tend to yield larger amounts of proton-rich ejecta (electron fraction, $Y_e > 0.51$) in the hemisphere of the higher $\nu_{\rm e}$ emissions, meanwhile neutron-rich matter ($Y_e < 0.49$) are ejected in the opposite hemisphere of the higher ${\bar \nu}_{\rm e}$ emissions. For larger asymmetric cases with $\ge 30\%$, the neutron-rich ejecta is abundantly produced, in which there are too much elements heavier than Zn compared to the solar abundances. This may place an upper limit of the asymmetric neutrino emissions in CCSNe. The characteristic features are also observed in elemental distribution; (1) abundances lighter than Ca are insensitive to the asymmetric neutrino emissions: (2) the production of Zn and Ge is larger in the neutron-rich ejecta even for smaller asymmetric cases with $\le 10\%$. We discuss these observational consequences, which may account for the (anti-)correlations among asymmetries of heavy elements and neutron star kicks in supernova remnants (SNRs). Future SNR observations of the direct measurement for the mass and spatial distributions of $\alpha$ elements, Fe, Zn and Ge will provide us the information on the asymmetric degree of neutrino emissions.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 2 minor

Summary. The paper investigates the impact of asymmetric neutrino emissions on explosive nucleosynthesis in neutrino-driven core-collapse supernovae. Simulations with imposed asymmetries show that higher ν_e emission in one hemisphere produces proton-rich ejecta (Y_e > 0.51) while the opposite hemisphere yields neutron-rich matter (Y_e < 0.49) from higher ν-bar_e emission. For asymmetries ≥30%, abundant neutron-rich ejecta overproduces elements heavier than Zn relative to solar abundances, suggesting an upper limit on asymmetry. Lighter elements (<Ca) are insensitive to asymmetry, while Zn and Ge production is enhanced even at ≤10% asymmetry. The work discusses implications for elemental (anti-)correlations and neutron star kicks in supernova remnants.

Significance. If the modeling holds, the result supplies a nucleosynthesis-based constraint on neutrino emission asymmetry in CCSNe and links microphysical neutrino properties to observable abundance patterns and kinematics in remnants. The identification of Zn/Ge enhancement at modest asymmetry levels offers a potentially falsifiable signature for future SNR observations.

major comments (2)
  1. [Methods and Results sections describing the asymmetry implementation] The central claim that ≥30% asymmetry produces enough neutron-rich ejecta to overproduce elements >Zn (and thus set an upper limit) rests on the mapping from imposed asymmetry to final Y_e and entropy distributions. The manuscript does not demonstrate that the hydrodynamic and neutrino treatment (e.g., whether ray-by-ray or fixed-luminosity asymmetry without feedback) yields realistic low-Y_e mass and expansion timescales; this is load-bearing for the threshold result.
  2. [Nucleosynthesis calculations and yield tables] The nucleosynthesis post-processing must be shown to accurately capture the effects of the imposed asymmetry levels. Without explicit verification that the Y_e < 0.49 ejecta mass and its thermodynamic history are robust to the transport approximations, the overproduction conclusion at 30% cannot be taken as definitive.
minor comments (2)
  1. [Numerical setup] Clarify the exact definition of the asymmetry percentage (e.g., luminosity ratio between hemispheres) and how it is maintained throughout the simulation.
  2. [Results on heavy-element yields] Add quantitative error estimates or sensitivity tests on the reported elemental overproduction factors relative to solar abundances.

Simulated Author's Rebuttal

2 responses · 2 unresolved

We thank the referee for their careful reading of the manuscript and for identifying key points regarding the robustness of our asymmetry implementation and nucleosynthesis results. We address each major comment below.

read point-by-point responses

  1. Referee: [Methods and Results sections describing the asymmetry implementation] The central claim that ≥30% asymmetry produces enough neutron-rich ejecta to overproduce elements >Zn (and thus set an upper limit) rests on the mapping from imposed asymmetry to final Y_e and entropy distributions. The manuscript does not demonstrate that the hydrodynamic and neutrino treatment (e.g., whether ray-by-ray or fixed-luminosity asymmetry without feedback) yields realistic low-Y_e mass and expansion timescales; this is load-bearing for the threshold result.

    Authors: Our study imposes neutrino emission asymmetries by scaling luminosities hemisphere-by-hemisphere on top of otherwise spherically symmetric models, as described in the Methods section. This fixed-luminosity approach without full hydrodynamical feedback is an exploratory approximation chosen to isolate nucleosynthetic effects; it is consistent with prior parameterized studies of asymmetric neutrino-driven winds. We agree that a direct demonstration of realism for the resulting low-Y_e mass and expansion timescales would require additional simulations with self-consistent transport, which lies outside the present scope. We will revise the manuscript to explicitly state this limitation and its implications for the 30% threshold. revision: partial

  2. Referee: [Nucleosynthesis calculations and yield tables] The nucleosynthesis post-processing must be shown to accurately capture the effects of the imposed asymmetry levels. Without explicit verification that the Y_e < 0.49 ejecta mass and its thermodynamic history are robust to the transport approximations, the overproduction conclusion at 30% cannot be taken as definitive.

    Authors: Nucleosynthesis yields are obtained via post-processing of tracer particles using a standard nuclear reaction network, with Y_e and thermodynamic trajectories taken directly from the hydrodynamic runs. The overproduction of elements heavier than Zn at ≥30% asymmetry follows from the increased mass of Y_e < 0.49 material in those models. We acknowledge that robustness to alternative transport schemes is not explicitly verified here. We will add a dedicated paragraph in the revised manuscript discussing the post-processing assumptions and citing supporting literature on the sensitivity of yields to Y_e and entropy. revision: partial

standing simulated objections not resolved
  • Full demonstration via new simulations that the imposed fixed-luminosity asymmetry produces realistic low-Y_e ejecta masses and expansion timescales under ray-by-ray or other transport treatments
  • Explicit cross-checks of Y_e < 0.49 ejecta mass and thermodynamic histories against alternative neutrino transport approximations

Circularity Check

0 steps flagged

No significant circularity; results are direct simulation outputs

full rationale

The paper imposes parameterized neutrino emission asymmetries as inputs to hydrodynamic simulations, then computes resulting Y_e distributions and post-processed nucleosynthesis yields as direct numerical outputs. No equations reduce predictions to input definitions by construction, no parameters are fitted to the target abundances, and no load-bearing self-citations or uniqueness theorems are invoked in the provided abstract or described chain. The central claim (upper limit on asymmetry from overproduction of heavy elements) follows from the simulation results without self-referential reduction.

Axiom & Free-Parameter Ledger

1 free parameters · 0 axioms · 0 invented entities

Abstract-only; no explicit free parameters, axioms, or invented entities listed. The asymmetry percentages (10%, 30%) function as input variations whose effects are reported, but no fitting details given.

free parameters (1)
  • asymmetry percentage
    Values such as ≥30% and ≤10% are used to classify cases; treated as controlled inputs rather than fitted outputs.

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Works this paper leans on

37 extracted references · 37 canonical work pages · 1 internal anchor

  1. [1]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

    work page

  2. [2]

    Anders E., Grevesse N., 1989, @doi [ ] 10.1016/0016-7037(89)90286-X , http://ads.nao.ac.jp/abs/1989GeCoA..53..197A 53, 197

    work page doi:10.1016/0016-7037(89)90286-x 1989

  3. [3]

    Eichler M., et al., 2018, @doi [Journal of Physics G Nuclear Physics] 10.1088/1361-6471/aa8891 , http://ads.nao.ac.jp/abs/2018JPhG...45a4001E 45, 014001

    work page doi:10.1088/1361-6471/aa8891 2018

  4. [4]

    Fujimoto S.-i., Hashimoto M.-a., Kotake K., Yamada S., 2007, @doi [ ] 10.1086/509908 , http://ads.nao.ac.jp/abs/2007ApJ...656..382F 656, 382

    work page doi:10.1086/509908 2007

  5. [5]

    Fujimoto S.-i., Kotake K., Hashimoto M.-a., Ono M., Ohnishi N., 2011, @doi [ ] 10.1088/0004-637X/738/1/61 , http://ads.nao.ac.jp/abs/2011ApJ...738...61F 738, 61

    work page doi:10.1088/0004-637x/738/1/61 2011

  6. [6]

    A., Hix W

    Harris J. A., Hix W. R., Chertkow M. A., Lee C. T., Lentz E. J., Messer O. E. B., 2017, @doi [ ] 10.3847/1538-4357/aa76de , http://ads.nao.ac.jp/abs/2017ApJ...843....2H 843, 2

    work page doi:10.3847/1538-4357/aa76de 2017

  7. [7]

    Janka H.-T., 2017, @doi [ ] 10.3847/1538-4357/aa618e , https://ui.adsabs.harvard.edu/abs/2017ApJ...837...84J 837, 84

    work page doi:10.3847/1538-4357/aa618e 2017

  8. [8]

    Katsuda S., et al., 2018a, @doi [ ] 10.3847/1538-4357/aab092 , http://ads.nao.ac.jp/abs/2018ApJ...856...18K 856, 18

    work page doi:10.3847/1538-4357/aab092

  9. [9]

    J., Nakamura K., 2018b, @doi [ ] 10.3847/1538-4357/aad2d8 , http://ads.nao.ac.jp/abs/2018ApJ...863..127K 863, 127

    Katsuda S., Takiwaki T., Tominaga N., Moriya T. J., Nakamura K., 2018b, @doi [ ] 10.3847/1538-4357/aad2d8 , http://ads.nao.ac.jp/abs/2018ApJ...863..127K 863, 127

    work page doi:10.3847/1538-4357/aad2d8

  10. [10]

    Kifonidis K., Plewa T., Scheck L., Janka H.-T., M \"u ller E., 2006, @doi [ ] 10.1051/0004-6361:20054512 , http://ads.nao.ac.jp/abs/2006A&A...453..661K 453, 661

    work page doi:10.1051/0004-6361:20054512 2006

  11. [11]

    Nagakura H., et al., 2018, @doi [ ] 10.3847/1538-4357/aaac29 , http://ads.nao.ac.jp/abs/2018ApJ...854..136N 854, 136

    work page doi:10.3847/1538-4357/aaac29 2018

  12. [12]

    arXiv:1907.04863

    Nagakura H., Sumiyoshi K., Yamada S., 2019, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2019arXiv190704863N p. arXiv:1907.04863

    work page arXiv 2019

  13. [13]

    Nagataki S., Hashimoto M.-a., Sato K., Yamada S., 1997, @doi [ ] 10.1086/304565 , http://ads.nao.ac.jp/abs/1997ApJ...486.1026N 486, 1026

    work page doi:10.1086/304565 1997

  14. [14]

    O'Connor E., 2015, @doi [ ] 10.1088/0067-0049/219/2/24 , http://ads.nao.ac.jp/abs/2015ApJS..219...24O 219, 24

    work page doi:10.1088/0067-0049/219/2/24 2015

  15. [15]

    P., Couch S

    O'Connor E. P., Couch S. M., 2018, @doi [ ] 10.3847/1538-4357/aadcf7 , http://ads.nao.ac.jp/abs/2018ApJ...865...81O 865, 81

    work page doi:10.3847/1538-4357/aadcf7 2018

  16. [16]

    Ohnishi N., Kotake K., Yamada S., 2006, @doi [ ] 10.1086/500554 , http://ads.nao.ac.jp/abs/2006ApJ...641.1018O 641, 1018

    work page doi:10.1086/500554 2006

  17. [17]

    Ohnishi N., Kotake K., Yamada S., 2007, @doi [ ] 10.1086/520755 , http://ads.nao.ac.jp/abs/2007ApJ...667..375O 667, 375

    work page doi:10.1086/520755 2007

  18. [18]

    E., Buras R., Janka H.-T., Hoffman R

    Pruet J., Woosley S. E., Buras R., Janka H.-T., Hoffman R. D., 2005, @doi [ ] 10.1086/428281 , http://ads.nao.ac.jp/abs/2005ApJ...623..325P 623, 325

    work page doi:10.1086/428281 2005

  19. [19]

    D., Woosley S

    Pruet J., Hoffman R. D., Woosley S. E., Janka H.-T., Buras R., 2006, @doi [ ] 10.1086/503891 , http://ads.nao.ac.jp/abs/2006ApJ...644.1028P 644, 1028

    work page doi:10.1086/503891 2006

  20. [20]

    D., Woosley S

    Rauscher T., Heger A., Hoffman R. D., Woosley S. E., 2002, @doi [ ] 10.1086/341728 , http://ads.nao.ac.jp/abs/2002ApJ...576..323R 576, 323

    work page doi:10.1086/341728 2002

  21. [21]

    Scheck L., Kifonidis K., Janka H.-T., M \"u ller E., 2006, @doi [ ] 10.1051/0004-6361:20064855 , http://ads.nao.ac.jp/abs/2006A&A...457..963S 457, 963

    work page doi:10.1051/0004-6361:20064855 2006

  22. [22]

    J., Reeves J

    Seitenzahl I. R., R \"o pke F. K., Fink M., Pakmor R., 2010, @doi [ ] 10.1111/j.1365-2966.2010.17106.x , http://ads.nao.ac.jp/abs/2010MNRAS.407.2297S 407, 2297

    work page doi:10.1111/j.1365-2966.2010.17106.x 2010

  23. [23]

    M., Norman M

    Stone J. M., Norman M. L., 1992, @doi [ ] 10.1086/191681 , http://ads.nao.ac.jp/abs/1992ApJS...80..791S 80, 791

    work page doi:10.1086/191681 1992

  24. [24]

    E., Brown J

    Sukhbold T., Ertl T., Woosley S. E., Brown J. M., Janka H.-T., 2016, @doi [ ] 10.3847/0004-637X/821/1/38 , http://ads.nao.ac.jp/abs/2016ApJ...821...38S 821, 38

    work page internal anchor Pith review doi:10.3847/0004-637x/821/1/38 2016

  25. [25]

    G., Marek A., 2014, @doi [ ] 10.1088/0004-637X/792/2/96 , http://ads.nao.ac.jp/abs/2014ApJ...792...96T 792, 96

    Tamborra I., Hanke F., Janka H.-T., M \"u ller B., Raffelt G. G., Marek A., 2014, @doi [ ] 10.1088/0004-637X/792/2/96 , http://ads.nao.ac.jp/abs/2014ApJ...792...96T 792, 96

    work page doi:10.1088/0004-637x/792/2/96 2014

  26. [26]

    Tamura T., et al., 2019, @doi [ ] 10.1093/pasj/psz023 , https://ui.adsabs.harvard.edu/abs/2019PASJ...71...50T 71, 50

    work page doi:10.1093/pasj/psz023 2019

  27. [27]

    D., 2007, @doi [ ] 10.1086/523263 , http://ads.nao.ac.jp/abs/2007ApJ...671.1717T 671, 1717

    Tsunemi H., Katsuda S., Nemes N., Miller E. D., 2007, @doi [ ] 10.1086/523263 , http://ads.nao.ac.jp/abs/2007ApJ...671.1717T 671, 1717

    work page doi:10.1086/523263 2007

  28. [28]

    Ugliano M., Janka H.-T., Marek A., Arcones A., 2012, @doi [ ] 10.1088/0004-637X/757/1/69 , http://ads.nao.ac.jp/abs/2012ApJ...757...69U 757, 69

    work page doi:10.1088/0004-637x/757/1/69 2012

  29. [29]

    A., Dolence J., 2019, @doi [ ] 10.1093/mnras/sty2585 , http://ads.nao.ac.jp/abs/2019MNRAS.482..351V 482, 351

    Vartanyan D., Burrows A., Radice D., Skinner M. A., Dolence J., 2019, @doi [ ] 10.1093/mnras/sty2585 , http://ads.nao.ac.jp/abs/2019MNRAS.482..351V 482, 351

    work page doi:10.1093/mnras/sty2585 2019

  30. [30]

    Wanajo S., Janka H.-T., M \"u ller B., 2011, @doi [ ] 10.1088/2041-8205/726/2/L15 , http://ads.nao.ac.jp/abs/2011ApJ...726L..15W 726, L15

    work page doi:10.1088/2041-8205/726/2/l15 2011

  31. [31]

    Wanajo S., Janka H.-T., M \"u ller B., 2013a, @doi [ ] 10.1088/2041-8205/767/2/L26 , http://ads.nao.ac.jp/abs/2013ApJ...767L..26W 767, L26

    work page doi:10.1088/2041-8205/767/2/l26 2041

  32. [32]

    Wanajo S., Janka H.-T., M \"u ller B., 2013b, @doi [ ] 10.1088/2041-8205/774/1/L6 , http://ads.nao.ac.jp/abs/2013ApJ...774L...6W 774, L6

    work page doi:10.1088/2041-8205/774/1/l6 2041

  33. [33]

    Wanajo S., M \"u ller B., Janka H.-T., Heger A., 2018, @doi [ ] 10.3847/1538-4357/aa9d97 , http://ads.nao.ac.jp/abs/2018ApJ...852...40W 852, 40

    work page doi:10.3847/1538-4357/aa9d97 2018

  34. [34]

    Wongwathanarat A., Janka H.-T., M \"u ller E., 2013, @doi [ ] 10.1051/0004-6361/201220636 , http://ads.nao.ac.jp/abs/2013A&A...552A.126W 552, A126

    work page doi:10.1051/0004-6361/201220636 2013

  35. [35]

    Wongwathanarat A., Janka H.-T., M \"u ller E., Pllumbi E., Wanajo S., 2017, @doi [ ] 10.3847/1538-4357/aa72de , http://ads.nao.ac.jp/abs/2017ApJ...842...13W 842, 13

    work page doi:10.3847/1538-4357/aa72de 2017

  36. [36]

    E., Heger A., Weaver T

    Woosley S. E., Heger A., Weaver T. A., 2002, @doi [Reviews of Modern Physics] 10.1103/RevModPhys.74.1015 , http://ads.nao.ac.jp/abs/2002RvMP...74.1015W 74, 1015

    work page doi:10.1103/revmodphys.74.1015 2002

  37. [37]

    J., Tsunemi H., Lu F

    Yang X. J., Tsunemi H., Lu F. J., Li A., Xiang F. Y., Xiao H. P., Zhong J. X., 2013, @doi [ ] 10.1088/0004-637X/766/1/44 , https://ui.adsabs.harvard.edu/abs/2013ApJ...766...44Y 766, 44

    work page doi:10.1088/0004-637x/766/1/44 2013