pith. sign in

arxiv: 2606.05119 · v1 · pith:RUILKOTXnew · submitted 2026-06-03 · 🌌 astro-ph.SR · astro-ph.HE

Observational signatures of thermonuclear electron-capture supernovae -- Ne II line strengthening and color evolution as traces of the explosion mechanism

Alexander Holas , Fionntan P. Callan , Samuel W. Jones , Friedrich K. Roepke , R\"udiger Pakmor , Alexandra Kozyreva , Christine E. Collins , Luke J. Shingles
show 2 more authors
Stuart A. Sim Joshua M. Pollin
This is my paper

Pith reviewed 2026-06-28 04:04 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.HE
keywords thermonuclear electron-capture supernovaeobservational signaturesNe II emission lineSN Iaxmid-infrared spectroscopycolor evolutionradiative transferONe core explosions
0
0 comments X

The pith

tECSN models show a strengthening 12.8 μm Ne II line over time unlike CO deflagrations of similar nickel yield.

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

The paper runs radiative transfer calculations on 3D explosion models of thermonuclear electron-capture supernovae from ONe cores and compares them to CO white dwarf deflagrations. Both produce light curves and spectra similar to observed SNe Iax at early times, with the tECSN model declining more slowly in red colors due to extra titanium and chromium. At late times the tECSN model develops a much stronger and still growing Ne II emission line at 12.8 microns while the deflagration model does not. The work finds no clear contradictions with existing data but points to mid-infrared wavelengths as the most promising way to tell the two mechanisms apart.

Core claim

Thermonuclear electron-capture supernovae produce ejecta with a 25 percent lower nickel-to-total-mass ratio than comparable CO deflagrations and synthesize more titanium and chromium. When these yields are fed into radiative transfer calculations the resulting observables match SN Iax-like events at photospheric phases but diverge at late times through the exceptional strengthening of the 12.8 μm Ne II line, which remains nearly constant in the deflagration case.

What carries the argument

Late-time 1D radiative transfer spectra computed with the Artis code on 3D Leafs explosion models, isolating the time evolution of the 12.8 μm Ne II emission line as the distinguishing diagnostic.

If this is right

  • tECSNe remain viable candidates for some observed SN Iax events.
  • Early-time photometry alone cannot separate tECSNe from CO deflagrations.
  • Mid-infrared monitoring at late times offers the clearest route to mechanism discrimination.
  • The lower nickel fraction and higher titanium-chromium content alter the color evolution in a measurable way.
  • No current observables rule out tECSNe occurring in nature.

Where Pith is reading between the lines

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

  • Targeted mid-IR observations of known SN Iax events could test whether any match the predicted Ne II strengthening.
  • If the line signature is confirmed, it would tighten constraints on the fraction of intermediate-mass stars that end as ONe-core explosions rather than white-dwarf deflagrations.
  • The same modeling approach could be applied to other candidate channels such as hybrid CONe white dwarfs to map out additional spectral diagnostics.

Load-bearing premise

The nucleosynthetic yields and density structure taken from the 3D explosion simulations remain accurate when mapped into the radiative transfer calculation without major additional mixing at late times.

What would settle it

Mid-infrared spectra of a real SN Iax-like transient taken at multiple epochs after maximum light that either show or fail to show a steadily strengthening 12.8 μm Ne II line.

Figures

Figures reproduced from arXiv: 2606.05119 by Alexander Holas, Alexandra Kozyreva, Christine E. Collins, Fionntan P. Callan, Friedrich K. Roepke, Joshua M. Pollin, Luke J. Shingles, R\"udiger Pakmor, Samuel W. Jones, Stuart A. Sim.

Figure 1
Figure 1. Figure 1: Slices of the mapped ejecta structure of both explosion models at 100 s after the explosion. Here, we show the density, [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Elemental masses contained in the ejecta of both masses [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Synthetic early-time light curves of both explosion along selected colors. For comparison, we also show observational data [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Spectral energy decomposition plots of both explosion models at 10 and 25 days after the explosion. Here, we only color [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of our synthetic model spectra to observed spectra of SN 2005hk and SN 2019muj. The data of the observed [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Late-time emission spectra of both explosion models at 60 and 100 days after the explosion colored by the last emission type. [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Evolution of the (normalized) flux ration between the [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Sobolev escape probability, βS, for the Ne ii transition for the rho9.964_r35_sfs and r10_d2.0_Z models. The x-axis shows the initial velocity coordinate of each radial shell of the input model. We show βS for various epochs between 60 and 160 days with a 10-day spacing. The escape probability increases with time as indicated by the upward arrow. In the inset plot, we show the normalized value of βS at the… view at source ↗
Figure 9
Figure 9. Figure 9: Comparison of our late-time model spectra to a NIR [PITH_FULL_IMAGE:figures/full_fig_p013_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Synthetic light curve of the rho9.964_r35_sfs model generated with Stella, assuming that the explosion takes place within an sAGB star H envelope. dip at the beginning of the radioactive tail is caused by a numer￾ical viscosity. The light curve of our rho9.964_r35_sfs model is rather faint and exhibits a particularly long plateau duration, around 170 days, caused by the rather low kinetic energy of the ej… view at source ↗
read the original abstract

Thermonuclear electron-capture supernovae (tECSNe) are a potential fate of certain intermediate mass stars forming ONe cores at the end of their evolution. Simulations suggest that these explosions are a viable alternative to collapse, yet no synthetic observables exist that allow for their identification among observed transients. We present first of their kind synthetic observables of a tECSN simulation, aiming to establish whether these explosions can occur in nature, and investigate potential observational signatures to separate them from similar transients such as pure deflagrations in CO white dwarfs. We carry out 3D photospheric phase and 1D late phase simulations using the radiative transfer code Artis. As input, we use a tECSN explosion simulation and a CO deflagration simulation with comparable $^{56}$Ni production, both computed with the Leafs code. Both models have similar observational characteristics, akin to SNe~Iax-like events. The tECSN ejecta model are characterized by a $M(^{56}\mathrm{Ni})/M_\mathrm{ej}$ ratio $25\%$ lower than that of comparable CO deflagration models. At early times, the tECSN model shows a slower decline in the red colors compared to the CO deflagration due the greater amount of Ti and Cr synthesized in the tECSN explosion. At late times, the tECSN model exhibits an exceptionally strong $12.8\,\mu$m Ne II emission line, that strengthens substantially over time, whereas its strength remains largely unchanged in the CO deflagration. Our results suggest tECSNe could potentially result in SN~Iax-like transients. Importantly, we find no features that are in tension with existing observables. So far, there are no indicators that unambiguously and robustly separate tECSNe from deflagrations in CO white dwarfs. Nonetheless, our work highlights the potential importance of the mid-infrared wavelength range for distinguishing possible explosion mechanisms.

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 presents the first synthetic observables for a thermonuclear electron-capture supernova (tECSN) model computed with the Leafs code, compared against a CO white-dwarf deflagration model with comparable 56Ni yield. Using 3D photospheric-phase and 1D late-phase Artis radiative-transfer calculations, the authors report that both models produce SN Iax-like transients; the tECSN model exhibits slower early-time red-color decline due to higher Ti/Cr production and, at late times, an exceptionally strong 12.8 μm Ne II line whose strength increases substantially, while the line remains roughly constant in the deflagration model. They conclude that tECSNe remain viable but lack unambiguous observational discriminants from CO deflagrations.

Significance. If the reported Ne II line evolution and color differences prove robust, the work supplies the first quantitative, forward-model predictions that could guide mid-infrared searches for tECSNe and tests of explosion mechanisms in the Iax-like population. The direct comparison of two models with matched 56Ni mass run through an identical Artis pipeline is a clear methodological strength.

major comments (2)
  1. [late-phase simulations] Abstract and late-phase results section: the central claim that the 12.8 μm Ne II line strengthens substantially over time in the tECSN model (while remaining constant in the CO deflagration) rests on 1D late-phase Artis calculations applied to 3D Leafs ejecta. No test is presented of whether 3D asymmetries, clumping, or non-spherical ionization balance in the Ne-rich zones at t ≳ 100 d would alter the reported line evolution.
  2. [model selection and yields] Methods and results on nucleosynthesis: the paper states that the two models were chosen with comparable 56Ni production, yet provides no quantitative uncertainty estimates, convergence tests, or sensitivity analysis on how variations in the Ne, Ti, or Cr mass fractions (or their spatial distributions) propagate into the Ne II line strength or color curves.
minor comments (2)
  1. [abstract] Notation: the ratio M(56Ni)/M_ej is given as 25% lower for the tECSN model; the exact numerical values and the total ejecta masses should be stated explicitly for reproducibility.
  2. [figures] Figure clarity: the late-time spectral plots should indicate the wavelength range and resolution used for the Ne II line measurement and whether any continuum subtraction was applied.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive report and for recognizing the methodological strength of the direct model comparison. We address the two major comments below and will incorporate revisions to clarify limitations and strengthen the discussion of uncertainties.

read point-by-point responses

  1. Referee: [late-phase simulations] Abstract and late-phase results section: the central claim that the 12.8 μm Ne II line strengthens substantially over time in the tECSN model (while remaining constant in the CO deflagration) rests on 1D late-phase Artis calculations applied to 3D Leafs ejecta. No test is presented of whether 3D asymmetries, clumping, or non-spherical ionization balance in the Ne-rich zones at t ≳ 100 d would alter the reported line evolution.

    Authors: We agree that the late-time calculations use a 1D approximation applied to the 3D ejecta structure and that no explicit tests of 3D effects (asymmetries, clumping, or non-spherical ionization) on the Ne II line evolution have been performed. Full 3D radiative-transfer calculations at t ≳ 100 d remain computationally prohibitive for this initial study. We will revise the manuscript to expand the discussion of this approximation, including references to prior work that has examined the validity of 1D late-time modeling for similar events, and to qualify the reported line evolution accordingly. revision: partial

  2. Referee: [model selection and yields] Methods and results on nucleosynthesis: the paper states that the two models were chosen with comparable 56Ni production, yet provides no quantitative uncertainty estimates, convergence tests, or sensitivity analysis on how variations in the Ne, Ti, or Cr mass fractions (or their spatial distributions) propagate into the Ne II line strength or color curves.

    Authors: The two models were deliberately selected for comparable 56Ni yields to enable a controlled comparison. We acknowledge that the manuscript does not include quantitative uncertainty estimates, convergence tests, or sensitivity analyses on variations in Ne, Ti, or Cr abundances. As this is the first presentation of synthetic observables for a tECSN model, such explorations were outside the present scope. We will add a dedicated paragraph in the discussion section that qualitatively assesses how plausible variations in these species could affect the reported color evolution and Ne II line, and we will flag this as an important avenue for future work. revision: yes

Circularity Check

0 steps flagged

No circularity: forward radiative-transfer predictions from independent explosion simulations

full rationale

The paper computes synthetic observables by feeding nucleosynthetic yields and ejecta structures from pre-existing Leafs 3D explosion simulations into the Artis radiative-transfer code. No parameters are fitted to observed spectra or light curves, no self-referential definitions appear in the derivation of the Ne II line evolution or color differences, and no load-bearing step reduces to a prior result by the same authors that itself depends on the target claim. The reported differences between tECSN and CO-deflagration models are therefore direct consequences of the input yields rather than constructions internal to the present work.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on the accuracy of two external simulation codes and the assumption that the chosen models are representative of their respective channels.

axioms (2)
  • domain assumption Leafs-code explosion models accurately capture the nucleosynthesis and density structure of tECSN and CO deflagration events.
    These models are used as direct input to Artis without independent verification described in the abstract.
  • domain assumption Artis radiative transfer calculations in 3D photospheric and 1D nebular phases are sufficient to predict the reported line and color differences.
    No discussion of 3D effects in the late phase or missing physics is provided.

pith-pipeline@v0.9.1-grok · 5956 in / 1351 out tokens · 36725 ms · 2026-06-28T04:04:15.547412+00:00 · methodology

discussion (0)

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

Reference graph

Works this paper leans on

299 extracted references · 265 canonical work pages · 14 internal anchors

  1. [1]

    Abbott, B. P. and Abbott, R. and Abbott, T. D. and Abernathy, M. R. and Acernese, F. and Ackley, K. and Adams, C. and Adams, T. and Addesso, P. and Adhikari, R. X. and Adya, V. B. and Affeldt, C. and Agathos, M. and Agatsuma, K. and Aggarwal, N. and Aguiar, O. D. and Ain, A. and Ajith, P. and Allen, B. and Allocca, A. and Altin, P. A. and Amariutei, D. V....

    work page doi:10.1007/lrr-2016-1 2016

  2. [2]

    and Sethian, J

    Adalsteinsson, D. and Sethian, J. A. , year = 1999, month = jan, journal =. The. doi:10.1006/jcph.1998.6090 , urldate =

    work page doi:10.1006/jcph.1998.6090 1999

  3. [3]

    A&A , volume =

    Stripped-Envelope Stars in Different Metallicity Environments -. A&A , volume =. doi:10.1051/0004-6361/202142895 , urldate =

    work page doi:10.1051/0004-6361/202142895

  4. [4]

    and Bolton, Adam S

    Alam, Shadab and Ata, Metin and Bailey, Stephen and Beutler, Florian and Bizyaev, Dmitry and Blazek, Jonathan A. and Bolton, Adam S. and Brownstein, Joel R. and Burden, Angela and Chuang, Chia-Hsun and Comparat, Johan and Cuesta, Antonio J. and Dawson, Kyle S. and Eisenstein, Daniel J. and Escoffier, Stephanie and. The Clustering of Galaxies in the Comple...

    work page doi:10.1093/mnras/stx721

  5. [5]

    and Antilogus, P

    Aldering, G. and Antilogus, P. and Bailey, S. and Baltay, C. and Bauer, A. and Blanc, N. and Bongard, S. and Copin, Y. and Gangler, E. and Gilles, S. and Kessler, R. and Kocevski, D. and Lee, B. C. and Loken, S. and Nugent, P. and Pain, R. and P. Nearby. ApJ , volume =. doi:10.1086/507020 , urldate =

    work page doi:10.1086/507020

  6. [6]

    and Bell, John B

    Almgren, Ann S. and Bell, John B. and Colella, Phillip and Howell, Louis H. and Welcome, Michael L. , year = 1998, month = may, journal =. A. doi:10.1006/jcph.1998.5890 , urldate =

    work page doi:10.1006/jcph.1998.5890 1998

  7. [7]

    doi:10.1007/978-3-319-21846-5 , urldate =

    Handbook of. doi:10.1007/978-3-319-21846-5 , urldate =

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

  8. [8]

    MNRAS , volume =

    Evidence for a Maximum Mass Cut-off in the Neutron Star Mass Distribution and Constraints on the Equation of State , author =. MNRAS , volume =. doi:10.1093/mnras/sty1065 , urldate =

    work page doi:10.1093/mnras/sty1065

  9. [9]

    Astronomy and Astrophysics , volume =

    Structure and Evolution of Ultra-Massive White Dwarfs in General Relativity , author =. Astronomy and Astrophysics , volume =. doi:10.1051/0004-6361/202244604 , urldate =

    work page doi:10.1051/0004-6361/202244604

  10. [10]

    Astrophysical

    An, Zhen-Dong and Chen, Zhen-Peng and Ma, Yu-Gang and Yu, Jian-Kai and Sun, Ye-Ying and Fan, Gong-Tao and Li, Yong-Jiang and Xu, Hang-Hua and Huang, Bo-Song and Wang, Kan , year = 2015, month = oct, journal =. Astrophysical. doi:10.1103/PhysRevC.92.045802 , urldate =

    work page doi:10.1103/physrevc.92.045802 2015

  11. [11]

    and Rizzi, Luca and Tully, R

    Anand, Gagandeep S. and Rizzi, Luca and Tully, R. Brent and Shaya, Edward J. and Karachentsev, Igor D. and Makarov, Dmitry I. and Makarova, Lidia and Wu, Po-Feng and Dolphin, Andrew E. and Kourkchi, Ehsan , year = 2021, month = aug, journal =. The. doi:10.3847/1538-3881/ac0440 , urldate =

    work page doi:10.3847/1538-3881/ac0440 2021

  12. [12]

    and Koblischke, Nolan W

    Anderson, Richard I. and Koblischke, Nolan W. and Eyer, Laurent , year = 2024, month = mar, journal =. Small-Amplitude. doi:10.3847/2041-8213/ad284d , urldate =

    work page doi:10.3847/2041-8213/ad284d 2024

  13. [13]

    and Chanlaridis, S

    Antoniadis, J. and Chanlaridis, S. and Gr. Type. A&A , volume =. doi:10.1051/0004-6361/201936991 , urldate =

    work page doi:10.1051/0004-6361/201936991

  14. [14]

    A&A , volume =

    Electron Fraction Constraints Based on Nuclear Statistical Equilibrium with Beta Equilibrium , author =. A&A , volume =. doi:10.1051/0004-6361/201014276 , urldate =

    work page doi:10.1051/0004-6361/201014276

  15. [15]

    David , year = 1969, month = oct, journal =

    Arnett, W. David , year = 1969, month = oct, journal =. A Possible Model of Supernovae:. doi:10.1007/BF00650291 , urldate =

    work page doi:10.1007/bf00650291 1969

  16. [16]

    David and Bahcall, John N

    Arnett, W. David and Bahcall, John N. and Kirshner, Robert P. and Woosley, Stanford E. , year = 1989, month = jan, journal =. Supernova. doi:10.1146/annurev.aa.27.090189.003213 , urldate =

    work page doi:10.1146/annurev.aa.27.090189.003213 1989

  17. [17]

    Supernovae and

    Arnett, David , year = 1996, month = jan, urldate =. Supernovae and

    1996

  18. [18]

    Artis (V2025.11.11) , author =

  19. [19]

    J., & Scott, P

    Asplund, Martin and Grevesse, Nicolas and Sauval, A. Jacques and Scott, Pat , year = 2009, month = sep, journal =. The. doi:10.1146/annurev.astro.46.060407.145222 , urldate =

    work page doi:10.1146/annurev.astro.46.060407.145222 2009

  20. [20]

    and Amarsi, A

    Asplund, M. and Amarsi, A. M. and Grevesse, N. , year = 2021, month = sep, journal =. The Chemical Make-up of the. doi:10.1051/0004-6361/202140445 , urldate =

    work page internal anchor Pith review doi:10.1051/0004-6361/202140445 2021

  21. [21]

    and Gustafsson, B

    Asplund, M. and Gustafsson, B. and Lambert, D. L. and Rao, N. K. , year = 2000, month = jan, journal =. The

    2000

  22. [22]

    and Zwicky, F

    Baade, W. and Zwicky, F. , year = 1934, month = may, journal =. Cosmic. doi:10.1073/pnas.20.5.259 , urldate =

    work page doi:10.1073/pnas.20.5.259 1934

  23. [23]

    and Zwicky, F

    Baade, W. and Zwicky, F. , year = 1934, month = jan, journal =. On

    1934

  24. [24]

    and Zwicky, F

    Baade, W. and Zwicky, F. , year = 1934, month = may, journal =. On. doi:10.1073/pnas.20.5.254 , urldate =

    work page doi:10.1073/pnas.20.5.254 1934

  25. [25]

    and Zwicky, F

    Baade, W. and Zwicky, F. , year = 1934, month = jul, journal =. Remarks on. doi:10.1103/PhysRev.46.76.2 , urldate =

    work page doi:10.1103/physrev.46.76.2 1934

  26. [26]

    and Zwicky, F

    Baade, W. and Zwicky, F. , year = 1938, month = nov, journal =. Photographic. doi:10.1086/143996 , urldate =

    work page doi:10.1086/143996 1938

  27. [27]

    , year = 1945, month = nov, journal =

    Baade, W. , year = 1945, month = nov, journal =. B. doi:10.1086/144761 , urldate =

    work page doi:10.1086/144761 1945

  28. [28]

    A Semi-Implicit Mid-Point Rule for Stiff Systems of Ordinary Differential Equations , author =. Numer. Math. , volume =. doi:10.1007/BF01418331 , urldate =

    work page doi:10.1007/bf01418331

  29. [29]

    Badwaik, Jayesh and Chandrashekar, Praveen and Klingenberg, Christian , year = 2020, month = dec, journal =. Single-. doi:10.1007/s42967-019-00054-5 , urldate =

    work page doi:10.1007/s42967-019-00054-5 2020

  30. [30]

    and Nugent, Peter and Coppi, Paolo and Ellman, Nancy and Feindt, Ulrich and McKinnon, Ryan and Horowitz, Benjamin and Effron, Aaron , year = 2013, month = may, journal =

    Baltay, Charles and Rabinowitz, David and Hadjiyska, Elena and Walker, Emma S. and Nugent, Peter and Coppi, Paolo and Ellman, Nancy and Feindt, Ulrich and McKinnon, Ryan and Horowitz, Benjamin and Effron, Aaron , year = 2013, month = may, journal =. The. doi:10.1086/671198 , urldate =

    work page doi:10.1086/671198 2013

  31. [31]

    and Ciatti, F

    Barbon, R. and Ciatti, F. and Rosino, L. , year = 1979, month = feb, journal =. Photometric Properties of Type

    1979

  32. [32]

    MNRAS , volume =

    Barna, Barnab. MNRAS , volume =. doi:10.1093/mnras/staa3543 , urldate =

    work page doi:10.1093/mnras/staa3543

  33. [33]

    Nucleosynthesis

    Batziou, Eirini and Glas, Robert and Janka, H.-Thomas and Ehring, Jakob and Abdikamalov, Ernazar and Just, Oliver , year = 2024, month = dec, number =. Nucleosynthesis. doi:10.48550/arXiv.2412.02756 , urldate =. arXiv , langid =:2412.02756 , primaryclass =

    work page doi:10.48550/arxiv.2412.02756 2024

  34. [34]

    C., Kulkarni, S

    Bellm, Eric C. and Kulkarni, Shrinivas R. and Graham, Matthew J. and Dekany, Richard and Smith, Roger M. and Riddle, Reed and Masci, Frank J. and Helou, George and Prince, Thomas A. and Adams, Scott M. and Barbarino, C. and Barlow, Tom and Bauer, James and Beck, Ron and Belicki, Justin and Biswas, Rahul and Blagorodnova, Nadejda and Bodewits, Dennis and B...

    work page doi:10.1088/1538-3873/aaecbe

  35. [35]

    and Cappellaro, E

    Benetti, S. and Cappellaro, E. and Mazzali, P. A. and Turatto, M. and Altavilla, G. and Bufano, F. and. The. The Astrophysical Journal , volume =. doi:10.1086/428608 , urldate =

    work page doi:10.1086/428608

  36. [36]

    Journal of Computational Physics , keywords =

    Local Adaptive Mesh Refinement for Shock Hydrodynamics , author =. Journal of Computational Physics , volume =. doi:10.1016/0021-9991(89)90035-1 , urldate =

    work page doi:10.1016/0021-9991(89)90035-1

  37. [37]

    Spectrophotometric

    Bessell, Michael and Murphy, Simon , year = 2012, month = feb, journal =. Spectrophotometric. doi:10.1086/664083 , urldate =

    work page doi:10.1086/664083 2012

  38. [38]

    The Astrophysical Journal , volume =

    Revival of a Stalled Supernova Shock by Neutrino Heating , author =. The Astrophysical Journal , volume =. doi:10.1086/163343 , urldate =

    work page doi:10.1086/163343

  39. [39]

    F., & Quataert, E

    Beutler, Florian and Blake, Chris and Colless, Matthew and Jones, D. Heath and. The. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1111/j.1365-2966.2011.19250.x , urldate =

    work page doi:10.1111/j.1365-2966.2011.19250.x 2011

  40. [40]

    Discovery of a runaway star likely ejected by a Type Iax Supernova

    Bhat, A. and Hollands, M. and Dorsch, M. and Geier, S. and Heber, U. and Koester, D. and Pakmor, R. and Shen, Ken J. , year = 2026, month = feb, number =. Discovery of a Runaway Star Likely Ejected by a. doi:10.48550/arXiv.2602.23900 , urldate =. arXiv , langid =:2602.23900 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2602.23900 2026

  41. [41]

    Blinnikov, S. I. and Bartunov, O. S. , year = 1993, month = jun, journal =. Non-Equilibrium Radiative Transfer in Supernova Theory : Models of Linear Type

    1993

  42. [42]

    Blinnikov, S. I. and R. Theoretical Light Curves for Deflagration Models of Type. A&A , volume =. doi:10.1051/0004-6361:20054594 , urldate =

    work page doi:10.1051/0004-6361:20054594

  43. [43]

    , year = 1995, month = may, journal =

    Bloecker, T. , year = 1995, month = may, journal =. Stellar Evolution of Low and Intermediate-Mass Stars

    1995

  44. [44]

    and Matheson, T

    Blondin, S. and Matheson, T. and Kirshner, R. P. and Mandel, K. S. and Berlind, P. and Calkins, M. and Challis, P. and Garnavich, P. M. and Jha, S. W. and Modjaz, M. and Riess, A. G. and Schmidt, B. P. , year = 2012, month = may, journal =. The. doi:10.1088/0004-6256/143/5/126 , urldate =

    work page doi:10.1088/0004-6256/143/5/126 2012

  45. [45]

    Evidence for Sub-

    Blondin, St. Evidence for Sub-. MNRAS , volume =. doi:10.1093/mnras/stw2492 , urldate =

    work page doi:10.1093/mnras/stw2492

  46. [46]

    and Dessart, L

    Blondin, S. and Dessart, L. and Hillier, D. J. and Ramsbottom, C. A. and Storey, P. J. , year = 2023, month = oct, journal =. Nebular Spectra from. doi:10.1051/0004-6361/202347147 , urldate =

    work page doi:10.1051/0004-6361/202347147 2023

  47. [47]

    A&A , volume =

    Blondin, St. A&A , volume =. doi:10.1051/0004-6361/202244134 , urldate =

    work page doi:10.1051/0004-6361/202244134

  48. [48]

    Boccioli, Luca and Roberti, Lorenzo , year = 2024, month = mar, journal =. The. doi:10.3390/universe10030148 , urldate =

    work page doi:10.3390/universe10030148 2024

  49. [49]

    and Fowler, William A

    Bodansky, David and Clayton, Donald D. and Fowler, William A. , year = 1968, month = nov, journal =. Nuclear. doi:10.1086/190176 , urldate =

    work page doi:10.1086/190176 1968

  50. [50]

    and Townsley, Dean M

    Boos, Samuel J. and Townsley, Dean M. and Shen, Ken J. and Caldwell, Spencer and Miles, Broxton J. , year = 2021, month = oct, journal =. Multidimensional. doi:10.3847/1538-4357/ac07a2 , urldate =

    work page doi:10.3847/1538-4357/ac07a2 2021

  51. [51]

    and Townsley, Dean M

    Boos, Samuel J. and Townsley, Dean M. and Shen, Ken J. , year = 2024, month = sep, journal =. Type. doi:10.3847/1538-4357/ad5da2 , urldate =

    work page doi:10.3847/1538-4357/ad5da2 2024

  52. [52]

    and Dessart, Luc and Shen, Ken J

    Boos, Samuel J. and Dessart, Luc and Shen, Ken J. and Townsley, Dean M. , year = 2024, month = oct, doi =. Non-

    2024

  53. [53]

    Azalee and Pearson, Jeniveve and Shrestha, Manisha and Sand, David J

    Bostroem, K. Azalee and Pearson, Jeniveve and Shrestha, Manisha and Sand, David J. and Valenti, Stefano and Jha, Saurabh W. and Andrews, Jennifer E. and Smith, Nathan and Terreran, Giacomo and Green, Elizabeth and Dong, Yize and Lundquist, Michael and Haislip, Joshua and Hoang, Emily T. and Hosseinzadeh, Griffin and Janzen, Daryl and Jencson, Jacob E. and...

    work page doi:10.3847/2041-8213/acf9a4 2041

  54. [54]

    and Porter, Troy A

    Bouchet, Laurent and Strong, Andrew W. and Porter, Troy A. and Moskalenko, Igor V. and Jourdain, Elisabeth and Roques, Jean-Pierre , year = 2011, month = sep, journal =. doi:10.1088/0004-637X/739/1/29 , urldate =

    work page doi:10.1088/0004-637x/739/1/29 2011

  55. [55]

    Numerical

    Brady, Ryan and Zingale, Michael , year = 2025, journal =. Numerical. doi:10.3847/2515-5172/add686 , urldate =. arXiv , langid =:2505.07918 , primaryclass =

    work page doi:10.3847/2515-5172/add686 2025

  56. [56]

    Brahe, Tycho , year = 1573, publisher =

  57. [57]

    and Thomas, R

    Branch, David and Baron, E. and Thomas, R. C. and Kasen, D. and Li, Weidong and Filippenko, Alexei V. , year = 2004, month = oct, journal =. Reading the. doi:10.1086/425081 , urldate =

    work page doi:10.1086/425081 2004

  58. [58]

    Craig , year = 2017, series =

    Branch, David and Wheeler, J. Craig , year = 2017, series =. Supernova. doi:10.1007/978-3-662-55054-0 , isbn =

    work page doi:10.1007/978-3-662-55054-0 2017

  59. [59]

    Bravo, E. and. Coulomb Corrections to the Equation of State of Nuclear Statistical Equilibrium Matter: Implications for. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1046/j.1365-8711.1999.02694.x , urldate =

    work page doi:10.1046/j.1365-8711.1999.02694.x 1999

  60. [60]

    Bravo, E. and. Explosion of White Dwarfs Harboring Hybrid. Astronomy and Astrophysics , volume =. doi:10.1051/0004-6361/201527861 , urldate =

    work page doi:10.1051/0004-6361/201527861

  61. [61]

    and Doherty, Carolyn and Pignatari, Marco and Pols, Onno and Lugaro, Maria , year = 2023, month = jul, journal =

    Brinkman, Hannah E. and Doherty, Carolyn and Pignatari, Marco and Pols, Onno and Lugaro, Maria , year = 2023, month = jul, journal =. Aluminium-26 from. doi:10.3847/1538-4357/acd7ea , urldate =

    work page doi:10.3847/1538-4357/acd7ea 2023

  62. [62]

    Mesoscale

    Brooker, Ezra and Zhiglo, Andrey and Plewa, Tomasz , year = 2025, month = may, number =. Mesoscale. doi:10.48550/arXiv.2505.18482 , urldate =. arXiv , keywords =:2505.18482 , primaryclass =

    work page doi:10.48550/arxiv.2505.18482 2025

  63. [63]

    Convection

    Brooks, Jared and Schwab, Josiah and Bildsten, Lars and Quataert, Eliot and Paxton, Bill , year = 2017, month = jan, journal =. Convection. doi:10.3847/2041-8213/834/2/L9 , urldate =

    work page doi:10.3847/2041-8213/834/2/l9 2017

  64. [64]

    L., Norman, M

    Bryan, Greg L. and Norman, Michael L. and O'Shea, Brian W. and Abel, Tom and Wise, John H. and Turk, Matthew J. and Reynolds, Daniel R. and Collins, David C. and Wang, Peng and Skillman, Samuel W. and Smith, Britton and Harkness, Robert P. and Bordner, James and Kim, Ji-hoon and Kuhlen, Michael and Xu, Hao and Goldbaum, Nathan and Hummels, Cameron and Kri...

    work page doi:10.1088/0067-0049/211/2/19

  65. [65]

    Computer Physics Communications , series =

    A Piecewise Parabolic Method for Cosmological Hydrodynamics , author =. Computer Physics Communications , series =. doi:10.1016/0010-4655(94)00191-4 , urldate =

    work page doi:10.1016/0010-4655(94)00191-4

  66. [66]

    Magnetorotational Core-Collapse Supernovae: The Impact of the Magnetic Field's Structure , shorttitle =

    Bugli, Matteo and Guilet, J. Magnetorotational Core-Collapse Supernovae: The Impact of the Magnetic Field's Structure , shorttitle =. IAU Symp. , volume =. doi:10.1017/S1743921322001193 , keywords =

    work page doi:10.1017/s1743921322001193

  67. [67]

    and Sim, S

    Bulla, M. and Sim, S. A. and Kromer, M. , year = 2015, month = jun, journal =. Polarization Spectral Synthesis for. doi:10.1093/mnras/stv657 , urldate =

    work page doi:10.1093/mnras/stv657 2015

  68. [68]

    Turbulent

    Burkert, Andreas and Bodenheimer, Peter , year = 2000, month = nov, journal =. Turbulent. doi:10.1086/317122 , urldate =

    work page doi:10.1086/317122 2000

  69. [69]

    and Murphy, Jeremiah W

    Burrows, Adam and Dolence, Joshua C. and Murphy, Jeremiah W. , year = 2012, month = oct, journal =. doi:10.1088/0004-637X/759/1/5 , urldate =

    work page doi:10.1088/0004-637x/759/1/5 2012

  70. [70]

    Burrows, Adam and Wang, Tianshu and Vartanyan, David and Coleman, Matthew S. B. , year = 2023, month = nov, number =. A. doi:10.48550/arXiv.2311.12109 , urldate =. arXiv , keywords =:2311.12109 , primaryclass =

    work page doi:10.48550/arxiv.2311.12109 2023

  71. [71]

    Butterworth, Stephen , year = 1930, month = oct, journal =. On the

    1930

  72. [72]

    and Pastorello, A

    Cai, Y.-Z. and Pastorello, A. and Fraser, M. and Botticella, M. T. and. Intermediate-Luminosity Red Transients:. A&A , volume =. doi:10.1051/0004-6361/202141078 , urldate =

    work page doi:10.1051/0004-6361/202141078

  73. [73]

    Investigating the Origins of Thermonuclear Supernovae through Multi-Dimensional Radiative Transfer Modelling , author =

  74. [74]

    Callan, F. P. and Sim, S. A. and Collins, C. E. and Shingles, L. J. and Lach, F. and R. Including a Luminous Central Remnant in Radiative Transfer Simulations for. MNRAS , volume =. doi:10.1093/mnras/stae847 , urldate =

    work page doi:10.1093/mnras/stae847

  75. [75]

    Callan, F. P. and Holas, A. and. A&A , volume =. doi:10.1051/0004-6361/202554548 , urldate =

    work page doi:10.1051/0004-6361/202554548

  76. [76]

    Canal, Ramon and Isern, Jordi and Labay, Javier , year = 1992, month = oct, journal =. The. doi:10.1086/186574 , urldate =

    work page doi:10.1086/186574 1992

  77. [77]

    Monthly Notices of the Royal Astronomical Society , volume =

    Black Dwarf Supernova in the Far Future , author =. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1093/mnras/staa2262 , urldate =

    work page doi:10.1093/mnras/staa2262

  78. [78]

    and Scolnic, Dan and Said, Khaled and Brout, Dillon and Peterson, Erik R

    Carr, Anthony and Davis, Tamara M. and Scolnic, Dan and Said, Khaled and Brout, Dillon and Peterson, Erik R. and Kessler, Richard , year = 2022, month = oct, journal =. The. doi:10.1017/pasa.2022.41 , urldate =

    work page doi:10.1017/pasa.2022.41 2022

  79. [79]

    Kelvin--

    Casanova, Jordi and Jos. Kelvin--. Nature , volume =. doi:10.1038/nature10520 , urldate =

    work page doi:10.1038/nature10520

  80. [80]

    and Potekhin, A

    Cassisi, S. and Potekhin, A. Y. and Pietrinferni, A. and Catelan, M. and Salaris, M. , year = 2007, month = jun, journal =. Updated. doi:10.1086/516819 , urldate =

    work page doi:10.1086/516819 2007

Showing first 80 references.