Pith. sign in

REVIEW 3 major objections 5 minor 2 cited by

Resolution requirements for numerical modeling of neutrino quantum kinetics

T0 review · 3 major / 5 minor · reviewed 2026-08-10 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read Resolving every unstable inhomogeneous mode is a necessary condition for accurate numerical modeling of neutrino quantum kinetics.

desk verdict A careful two-scheme resolution study with convincing internal evidence, but the 'settles the debate' framing overreaches while the Shalgar contradiction remains unexplained. read the letter →

arxiv 2501.14145 v2 pith:QSJGEBL2 submitted 2025-01-24 astro-ph.HE hep-ph

Hiroki Nagakura , Masamichi Zaizen , Jiabao Liu , Lucas Johns This is my paper · ORCID
classification astro-ph.HEhep-ph
keywords neutrinoquantumkineticsfastflavorconversionspatialresolutionlinearstabilityanalysisELN-XLNcrossingcore-collapsesupernovabinaryneutronstarmergernumericalconvergence
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

The paper argues that the spatial resolution of a neutrino quantum-kinetic simulation is decisive for its result: unless the grid resolves every unstable inhomogeneous mode of the flavor instability, the simulation underestimates the growth of flavor coherence and relaxes to the wrong asymptotic flavor state. The claim is supported by a one-dimensional periodic-box study with two independent numerical schemes, finite-volume WENO and pseudospectral, plus a linear stability analysis including inhomogeneous modes. If correct, this settles a recent debate over resolution requirements and implies that direct global simulations of core-collapse supernovae and neutron-star mergers remain computationally intractable without effective treatments such as attenuation or subgrid models.

What carries the argument

The load-bearing machinery is the dispersion relation of the linearized quantum kinetic equation over inhomogeneous modes, which gives the growth rate $\operatorname{Im}\Omega(K)$ for each spatial wave number $K$; it maps grid resolution directly onto which instabilities can appear, since a grid with $N_z$ points supports only wave numbers up to its Nyquist limit. Two further elements carry the argument: the ELN-XLN angular distribution, whose crossing is the necessary and sufficient condition for fast-flavor instability once all modes are included and whose persistence is used as a diagnostic of an unconverged state, and the norm of the polarization vector $|P|$, whose violation measures artificial depolarization from flavor energy leaking past the grid cutoff. The interplay of these three ingredients explains both the wrong asymptotic states at low resolution and the slow late-time depolarization even in converged runs.

What would settle it

Run a three-dimensional, multi-energy quantum-kinetic simulation with realistic collisions at spatial resolutions below and above the threshold set by the fastest-growing unstable mode and check whether the low-resolution run reaches the same asymptotic survival probabilities and erases the ELN-XLN crossing; if it does, the claimed necessary condition does not transfer to realistic conditions.

Watch

Extended reading notes

Core claim

The paper's central discovery is that the asymptotic outcome of fast neutrino flavor conversion is controlled by whether all unstable wave numbers of the linearized dispersion relation are represented on the grid. Low-resolution models ($N_z = 10, 40, 100$ for a box $L = 10000\,\mu^{-1}$) show suppressed growth of the flavor-coherency amplitude, delayed nonlinear onset, and a final state that retains part of the original electron-lepton-number (ELN-XLN) angular crossing, whereas high-resolution models ($N_z = 1000, 10000$) and the pseudospectral reference solution erase the crossing and agree with each other. Stability analysis of the final state of the lowest-resolution run shows that the under-resolved high-$|K|$ modes remain unstable while the resolved low-$|K|$ modes have stabilized, which explains why the crossing never disappears. The paper concludes that resolving all unstable modes is a necessary condition for accurate modeling, that resolving only the maximum-growth mode is the bare minimum, and that nonlinear turbulent cascades make even finer grids desirable.

Load-bearing premise

The requirement that all unstable inhomogeneous modes be resolved is derived in a simplified one-dimensional, monoenergetic, axisymmetric, collisionless periodic box, and the paper assumes that this requirement still governs the much richer three-dimensional, multi-energy, collisional flows in supernovae and neutron-star mergers.

Editorial extensions

If this is right

  • A simulation that resolves only the homogeneous mode or even the maximum-growth mode can converge to a qualitatively wrong asymptotic flavor state, diagnosed by a leftover ELN-XLN angular crossing.
  • Flavor energy leached past the grid's maximum wave number produces artificial depolarization; even converged runs show slow late-time growth of the $|P|$ violation, so long integrations need this metric monitored.
  • Agreement between the finite-volume WENO run and the pseudospectral FFT run at high resolution rules out a single-method artifact as the source of the resolution dependence.
  • Because resolving all unstable modes is necessary, direct global simulations without effective treatments are currently intractable, strengthening the case for attenuation methods or subgrid models as the near-term route to global modeling.
  • For the tested angular distribution, angular resolution matters little ($N_v = 125$ is enough) because the unstable eigenvector is smooth in angle, while spatial resolution is the controlling factor.

Reading between the lines

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

  • If the criterion transfers to realistic conditions, published global simulations run at standard neutrino-transport resolutions may carry systematic biases in flavor-conversion outcomes; a targeted patch test comparing a global low-resolution run with a high-resolution local box covering the most unstable modes would reveal the bias.
  • A residual ELN-XLN crossing at the end of a simulation that was present initially could serve as a cheap a-posteriori flag for under-resolution, since converged runs erase it.
  • The resolution requirement can be restated as an operational rule for production codes: choose the grid spacing smaller than about half the wavelength of the fastest-growing mode implied by the local dispersion relation, which can be estimated on the fly.
  • Monitoring $\max \delta|P|$ supplies a collision-independent accuracy budget for long quantum-kinetic integrations and could be used to drive adaptive mesh refinement in future global schemes.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. This paper investigates spatial and angular resolution requirements for numerical simulations of neutrino quantum kinetics in a simplified 1D periodic box. The authors simulate fast flavor conversion with a seventh-order WENO finite-volume scheme and a pseudospectral scheme, compare them at high resolution, and use linear stability analysis including inhomogeneous modes to interpret the results. They find that low spatial resolution underestimates the growth of flavor instabilities, leaves the ELN-XLN angular crossing partially unsmoothed, and yields asymptotic flavor-conversion states that differ from high-resolution runs; angular resolution is found to be much less critical. The paper concludes that resolving all unstable inhomogeneous modes is a necessary condition for accurate QKE modeling and that low-resolution simulations can give wrong asymptotic states.

Significance. If correct, the paper provides a useful quantitative benchmark for resolution choices in QKE simulations and strengthens the case that global simulations require effective treatments. The use of two independent numerical schemes (WENO and pseudospectral) with good agreement at the highest resolution, and the use of a linear stability analysis as an independent benchmark, are genuine strengths; no parameters are fitted to the target outcome. The main weakness is that the central claim is derived from a highly idealized configuration, and the manuscript does not resolve a direct contradiction with a previous study that used the same initial distributions.

major comments (3)
  1. [Sec. IV.C, Abstract] The manuscript explicitly states that Shalgar [36], using the same initial angular distributions (Eq. 2), found essentially no spatial-resolution dependence, and that identifying the source of this inconsistency is beyond the scope of the work. This is load-bearing for the central claim, because the internal WENO/pseudospectral agreement does not rule out a common systematic error in the present setup, such as the unspecified random perturbation amplitude in Sec. II, the periodic boundary implementation, or the initialization procedure. Without a head-to-head comparison or an explanation of the discrepancy, the conclusion that low resolution 'leads to wrong asymptotic states' and the abstract's claim to 'settle the debate' are not fully supported. The perturbation amplitude used for the off-diagonal initial condition should be reported, and a comparison with [36] or a physical argument for the difference is needed.
  2. [Secs. II and V] The paper's central 'necessary condition' is derived from a 1D, monoenergetic, axisymmetric, collisionless, periodic-box model with L=10000 mu^-1, a setup the authors themselves describe as chosen 'to isolate the origin of numerical artifacts.' The load-bearing premise is that resolution requirements measured in this simplified box transfer to realistic 3D, multi-energy, collisional CCSN and BNSM conditions. This transfer is not tested; if additional physics changes the instability spectrum or the nonlinear cascade, the specific grid requirement (resolve all unstable modes) could differ. The conclusion should either be restricted to systems with the same instability structure or be accompanied by a physical argument for why the requirement is generic.
  3. [Sec. IV.B, Figs. 9-10] The discussion of |P| conservation is used to support the claim that low-resolution simulations suffer from artificial depolarization. However, the manuscript also states that the highest-resolution model (Nz=10000) shows time-accumulating violation and that the Nz=1000 model has a 'large violation' yet a 'reasonable' asymptotic state. The relation between max(delta|P|) and the accuracy of the asymptotic state is therefore ambiguous; the paper should quantify how much |P| violation is tolerable or how it maps to errors in Pee and the ELN-XLN distribution, otherwise this diagnostic does not sharply distinguish physical saturation from numerical artifacts.
minor comments (5)
  1. [Sec. II] The phrase 'seventh-ordered weighted essentially non-oscillatory (WENO) scheme' should be 'seventh-order'.
  2. [Sec. II] The initial off-diagonal perturbation amplitude is not specified; providing its value and the random-realization procedure would improve reproducibility, especially given the comparison with [36].
  3. [Sec. IV.C] The sentence 'the time scale of flavor conversion is determined by mu^-1 whereas the length scale is not' would benefit from a restatement of the argument being criticized, since the reader is not otherwise told what 'length scale' refers to in [36].
  4. [Sec. II and Fig. 5] The acronym ELN-XLN is used without definition; a brief definition at first use, such as 'electron-lepton-number minus heavy-lepton-number angular distribution,' would aid the reader.
  5. [Fig. 9] The caption uses 'max(δ|P|)' without defining the symbols; adding a one-sentence explanation of the normalization and the spatial/angular maximum would help.

Circularity Check

0 steps flagged · score 2.0 of 10

No load-bearing circularity: the central resolution-dependence claim rests on an independently computed dispersion relation and two-scheme agreement, with only minor non-load-bearing self-citations.

full rationale

The paper's central claim—that resolving all unstable inhomogeneous modes is necessary for accurate QKE modeling—is not obtained by fitting a parameter to the target outcome. The growth rates in Fig. 1 come from a standard linearized-QKE dispersion relation evaluated on the prescribed initial ELN-XLN angular distributions (Eq. 2), which is an independent linear benchmark. The resolution dependence is then demonstrated in Sec. IV with two independent numerical schemes, WENO and pseudospectral, and the highest-resolution WENO model 'shows an excellent agreement with another simulation by pseudospectral method with Nk = 10000' (Sec. IV.A, Fig. 3). The post-hoc dispersion relation computed on the Nz = 10 asymptotic state (Fig. 6) is interpretive rather than circular: it applies the same linear machinery to the averaged final state to explain why low-resolution runs still have unstable under-resolved modes, but the asymptotic-state difference is already established by the simulations themselves. Self-citations to [23] and [38] provide numerical implementations only and are not load-bearing for the conclusion, while [39] is a multi-group code comparison. The one serious caveat is Sec. IV.C: the authors state that Shalgar [36] found essentially no spatial-resolution dependence for the same initial angular distributions and that 'to identify the source of the inconsistency, a detailed comparison study is required, but it is beyond the scope of this work.' This is a genuine verification gap—the 'necessary condition' is not yet reconciled with an external null result—but a verification gap is not circularity under the rules. No equation reduces to its own input, no fitted parameter is renamed as a prediction, and the main conclusion does not rest on an unexamined self-citation. Score 2 reflects only minor, non-load-bearing self-citations.

Assumptions & free parameters 8 free parameters · 6 assumptions · 0 invented entities

All model parameters are inputs from [36] or choices of the numerical experiment; none are fitted to the target outcome. The paper introduces no new physical entity; 'artificial depolarization' is a numerical artifact, not a proposed entity. The central claim is about numerical convergence, so the ledger is dominated by modeling assumptions rather than invented physics.

free parameters (8)
  • Initial electron-neutrino angular distribution constant = 0.5
    Eq 2; uniform in cos theta, taken from [36] to set up the model; not fitted to outcomes.
  • Initial antineutrino angular distribution baseline = 0.47
    Eq 2; from [36]; together with the bump it creates the ELN-XLN crossing.
  • Initial antineutrino angular bump amplitude = 0.05
    Eq 2; from [36]; sets the depth of the ELN-XLN crossing.
  • Initial antineutrino angular bump width exponent = (1 - cos theta)^2 in exponent
    Eq 2; from [36]; sets the angular scale of the crossing.
  • Spatial domain length L = 10000 mu^-1
    Sec II; box size, chosen by hand; together with Nz it determines which wave numbers are resolved.
  • Vacuum frequency omega_vac = 10^-5 mu
    Sec II; used only in with-vacuum models; from [36].
  • Vacuum mixing angle theta_mix = 10^-3
    Sec II; used only in with-vacuum models; from [36].
  • Initial off-diagonal perturbation amplitude = unstated ('small and random')
    Sec II; seeds the instability; amplitude not specified, which could affect the onset time but not the claimed asymptotic conclusions.
assumptions (6)
  • domain assumption The mean-field quantum kinetic equation, Eq (1), correctly describes the flavor evolution in the regimes studied.
    Sec II; the whole study solves this equation without collision or matter terms.
  • standard math A plane-wave linear stability analysis of the initial state predicts the early-time growth rates of flavor instability.
    Sec III; used to identify Kpeak and to compare with simulation growth in Fig 2.
  • domain assumption An ELN-XLN angular crossing is necessary and sufficient for fast-flavor instability when all modes are considered, per [43].
    Sec IV.A; used to interpret why the crossing persists in low-resolution asymptotics.
  • domain assumption The polarization-vector norm |P| is conserved by the continuous collisionless QKE and is a valid accuracy diagnostic.
    Sec IV.B; used to detect artificial depolarization.
  • domain assumption The pseudospectral method with Nk=10000 modes gives a converged reference solution.
    Sec IV.A and Fig 3; the paper asserts exponential convergence for smooth solutions but shows no self-convergence sweep of the spectral run.
  • ad hoc to paper The 1D periodic-box, monoenergetic, axisymmetric, collisionless setup is representative enough to state a general necessary condition for neutrino quantum kinetics.
    Sec V; the 'necessary condition' conclusion is generalized beyond the tested setup.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Resolution requirements for numerical modeling of neutrino quantum kinetics." pith.science (2026). https://pith.science/paper/QSJGEBL2

@misc{pith2026250114145,
  author       = {Pith},
  title        = {Pith review of: Resolution requirements for numerical modeling of neutrino quantum kinetics},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/QSJGEBL2}},
  note         = {Machine review of arXiv:2501.14145}
}
read the original abstract

Neutrino quantum kinetics is a rapidly evolving field in computational astrophysics, with a primary focus on collective neutrino oscillations in core-collapse supernovae and post-merger phases of binary neutron star mergers. In recent years, there has been considerable debate concerning resolution dependence in numerical simulations. In this paper, we conduct a comprehensive resolution study in both angular- and spatial directions by using two independent schemes of quantum kinetic neutrino transport: finite volume and pseudospectral methods. We complement our discussion by linear stability analysis including inhomogeneous modes. Our result suggests that decreasing spatial resolutions underestimates the growth of flavor instability, and then leads to wrong asymptotic states of flavor conversions, which potentially has a critical impact on astrophysical consequences. We further delve into numerical results of low resolution simulations, that reveals the underlying mechanism responsible for numerical artifacts caused by insufficient resolutions. This study settles the debate on requirements of resolutions and serves as a guideline for numerical modeling of quantum kinetic neutrino transport.

Figures

Figures reproduced from arXiv: 2501.14145 by the authors.

Figure 1
Figure 1. FIG. 1. The growth rate (ImΩ) as a function of wave number [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2. Time evolution of the spatial average of flavor coherency ( [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3. Same as the bottom panels in Fig. [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: FIG. 4. Same as the bottom panels in Fig. [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 6
Figure 6. Figure 6: FIG. 6. Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p006_6.png]
Figure 7
Figure 7. Figure 7: FIG. 7. Similar as Figs [PITH_FULL_IMAGE:figures/full_fig_p007_7.png]
Figure 9
Figure 9. Figure 9: FIG. 9. Maximum violation of [PITH_FULL_IMAGE:figures/full_fig_p007_9.png]
Figure 10
Figure 10. Figure 10: FIG. 10. Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p008_10.png]

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Dynamic Competition of Fast and Collisional Neutrino Flavor Instabilities with Collisional Damping in Spatially Inhomogeneous Systems

    astro-ph.HE 2026-05 unverdicted novelty 6.0 of 10

    Numerical quantum-kinetic simulations demonstrate that collisional damping alters intermediate dynamics of coexisting fast and collisional neutrino flavor instabilities yet drives all unstable cases to the identical f...

  2. Theory of neutrino slow flavor evolution. Part II. Space-time evolution of linear instabilities

    hep-ph 2025-01 conditional novelty 6.0 of 10

    All weak fast and slow neutrino flavor instabilities are convective, so they grow spatially along neutrino directions rather than locally in time.

Reference graph

Works this paper leans on

48 extracted references · 5 canonical work pages · cited by 2 Pith papers

  1. [36]

    On the length scale of collective neutrino oscillations,

    Shashank Shalgar, “On the length scale of collective neutrino oscillations,” arXiv e-prints , arXiv:2408.06422 (2024), arXiv:2408.06422 [hep-ph]

    arXiv 2024

  2. [1]

    New Develop- ments in Flavor Evolution of a Dense Neutrino Gas,

    Irene Tamborra and Shashank Shalgar, “New Develop- ments in Flavor Evolution of a Dense Neutrino Gas,” Annual Review of Nuclear and Particle Science 71, 165– 188 (2021), arXiv:2011.01948 [astro-ph.HE]

    arXiv 2021

  3. [2]

    Fast Flavor Transformations,

    Sherwood Richers and Manibrata Sen, “Fast Flavor Transformations,” arXiv e-prints , arXiv:2207.03561 (2022), arXiv:2207.03561 [astro-ph.HE]

    arXiv 2022

  4. [3]

    Neutrinos and nucleosynthesis of elements,

    Tobias Fischer, Gang Guo, Karlheinz Langanke, Gabriel Mart ´ ınez-Pinedo, Yong-Zhong Qian, and Meng-Ru Wu, “Neutrinos and nucleosynthesis of elements,” Progress in Particle and Nuclear Physics 137, 104107 (2024), arXiv:2308.03962 [astro-ph.HE]

    arXiv 2024

  5. [4]

    Neutrinos from dense environments: Flavor mechanisms, theoretical approaches, observations, and new directions,

    M. Cristina Volpe, “Neutrinos from dense environments: Flavor mechanisms, theoretical approaches, observations, and new directions,” Reviews of Modern Physics 96, 025004 (2024), arXiv:2301.11814 [hep-ph]

    arXiv 2024

  6. [5]

    Physical mechanism of core-collapse supernovae that neutrinos drive,

    Shoichi Yamada, Hiroki Nagakura, Ryuichiro Akaho, Akira Harada, Shun Furusawa, Wakana Iwakami, Hiro- tada Okawa, Hideo Matsufuru, and Kohsuke Sumiyoshi, “Physical mechanism of core-collapse supernovae that neutrinos drive,” Proceedings of the Japan Academy, Se- ries B 100, 190–233 (2024)

    work page 2024

  7. [6]

    Collective Neutrino Oscillations,

    Huaiyu Duan, George M. Fuller, and Yong-Zhong Qian, “Collective Neutrino Oscillations,” Annual Re- view of Nuclear and Particle Science 60, 569–594 (2010), arXiv:1001.2799 [hep-ph]

    arXiv 2010

  8. [7]

    Tempo- ral instability enables neutrino flavor conversions deep inside supernovae,

    Basudeb Dasgupta and Alessandro Mirizzi, “Tempo- ral instability enables neutrino flavor conversions deep inside supernovae,” Phys. Rev. D 92, 125030 (2015), arXiv:1509.03171 [hep-ph]

    arXiv 2015

Show all 48 references
  1. [8]

    Neutrino Fast Fla- vor Conversions in Neutron-Star Postmerger Accre- tion Disks,

    Xinyu Li and Daniel M. Siegel, “Neutrino Fast Fla- vor Conversions in Neutron-Star Postmerger Accre- tion Disks,” Phys. Rev. Lett. 126, 251101 (2021), arXiv:2103.02616 [astro-ph.HE]

    2021 arXiv

  2. [9]

    Fast neutrino conversion in hydrodynamic simulations of neutrino-cooled accretion disks,

    Oliver Just, Sajad Abbar, Meng-Ru Wu, Irene Tam- borra, Hans-Thomas Janka, and Francesco Capozzi, “Fast neutrino conversion in hydrodynamic simulations of neutrino-cooled accretion disks,” Phys. Rev. D 105, 083024 (2022), arXiv:2203.16559 [astro-ph.HE]

    2022 arXiv

  3. [10]

    Fast flavor instability in hyper- massive neutron star disk outflows,

    Rodrigo Fern´ andez, Sherwood Richers, Nicole Mulyk, and Steven Fahlman, “Fast flavor instability in hyper- massive neutron star disk outflows,” Phys. Rev. D 106, 103003 (2022), arXiv:2207.10680 [astro-ph.HE]

    2022 arXiv

  4. [11]

    Fast neutrino flavor conversion in core-collapse supernovae: A parametric study in 1D models,

    Jakob Ehring, Sajad Abbar, Hans-Thomas Janka, Georg Raffelt, and Irene Tamborra, “Fast neutrino flavor conversion in core-collapse supernovae: A parametric study in 1D models,” Phys. Rev. D 107, 103034 (2023), arXiv:2301.11938 [astro-ph.HE]

    2023 arXiv

  5. [12]

    Fast Neutrino Fla- vor Conversions Can Help and Hinder Neutrino-Driven Explosions,

    Jakob Ehring, Sajad Abbar, Hans-Thomas Janka, Georg Raffelt, and Irene Tamborra, “Fast Neutrino Fla- vor Conversions Can Help and Hinder Neutrino-Driven Explosions,” Phys. Rev. Lett. 131, 061401 (2023), arXiv:2305.11207 [astro-ph.HE]

    2023 arXiv

  6. [13]

    Neutron star kick driven by asymmetric fast-neutrino fla- vor conversion,

    Hiroki Nagakura and Kohsuke Sumiyoshi, “Neutron star kick driven by asymmetric fast-neutrino fla- vor conversion,” Phys. Rev. D 109, 103017 (2024), arXiv:2401.15180 [astro-ph.HE]

    2024 arXiv

  7. [14]

    Simple method for determining asymptotic states of fast neutrino- flavor conversion,

    Masamichi Zaizen and Hiroki Nagakura, “Simple method for determining asymptotic states of fast neutrino- flavor conversion,” Phys. Rev. D 107, 103022 (2023), arXiv:2211.09343 [astro-ph.HE]

    2023 arXiv

  8. [15]

    Evaluating approximate asymptotic distributions for fast neutrino flavor conversions in a periodic 1D box,

    Zewei Xiong, Meng-Ru Wu, Sajad Abbar, Soumya Bhat- tacharyya, Manu George, and Chun-Yu Lin, “Evaluating approximate asymptotic distributions for fast neutrino flavor conversions in a periodic 1D box,” Phys. Rev. D 108, 063003 (2023), arXiv:2307.11129 [astro-ph.HE]. 10

    2023 arXiv

  9. [16]

    Thermodynamics of oscillating neu- trinos,

    Lucas Johns, “Thermodynamics of oscillating neu- trinos,” arXiv e-prints , arXiv:2306.14982 (2023), arXiv:2306.14982 [hep-ph]

    2023

  10. [17]

    Physics- informed neural networks for predicting the asymp- totic outcome of fast neutrino flavor conversions,

    Sajad Abbar, Meng-Ru Wu, and Zewei Xiong, “Physics- informed neural networks for predicting the asymp- totic outcome of fast neutrino flavor conversions,” Phys. Rev. D 109, 043024 (2024), arXiv:2311.15656 [astro-ph.HE]

    2024 arXiv

  11. [18]

    Asymptotic- state prediction for fast flavor transformation in neu- tron star mergers,

    Sherwood Richers, Julien Froustey, Somdutta Ghosh, Francois Foucart, and Javier Gomez, “Asymptotic- state prediction for fast flavor transformation in neu- tron star mergers,” Phys. Rev. D 110, 103019 (2024), arXiv:2409.04405 [astro-ph.HE]

    2024 arXiv

  12. [19]

    Fast flavor conversions at the edge of instability,

    Damiano F. G. Fiorillo and Georg Raffelt, “Fast flavor conversions at the edge of instability,” arXiv e-prints , arXiv:2403.12189 (2024), arXiv:2403.12189 [hep-ph]

    2024 arXiv

  13. [20]

    Bhatnagar-Gross-Krook subgrid model for neu- trino quantum kinetics,

    Hiroki Nagakura, Lucas Johns, and Masamichi Za- izen, “Bhatnagar-Gross-Krook subgrid model for neu- trino quantum kinetics,” Phys. Rev. D 109, 083013 (2024), arXiv:2312.16285 [astro-ph.HE]

    2024 arXiv

  14. [21]

    Robust integration of fast flavor conver- sions in classical neutrino transport,

    Zewei Xiong, Meng-Ru Wu, Manu George, and Chun- Yu Lin, “Robust integration of fast flavor conver- sions in classical neutrino transport,” arXiv e-prints , arXiv:2403.17269 (2024), arXiv:2403.17269 [astro- ph.HE]

    2024 arXiv

  15. [22]

    Simple method of diagnosing fast flavor conversions of supernova neutrinos,

    Basudeb Dasgupta, Alessandro Mirizzi, and Manibrata Sen, “Simple method of diagnosing fast flavor conversions of supernova neutrinos,” Phys. Rev. D98, 103001 (2018), arXiv:1807.03322 [hep-ph]

    2018 arXiv

  16. [23]

    Characteriz- ing quasisteady states of fast neutrino-flavor conversion by stability and conservation laws,

    Masamichi Zaizen and Hiroki Nagakura, “Characteriz- ing quasisteady states of fast neutrino-flavor conversion by stability and conservation laws,” Phys. Rev. D 107, 123021 (2023), arXiv:2304.05044 [astro-ph.HE]

    2023 arXiv

  17. [24]

    Theory of neutrino fast flavor evolution. Part I. Linear response theory and stability conditions

    Damiano F. G. Fiorillo and Georg G. Raffelt, “Theory of neutrino fast flavor evolution. Part I. Linear response theory and stability conditions.” Journal of High Energy Physics 2024, 225 (2024), arXiv:2406.06708 [hep-ph]

    2024 arXiv

  18. [25]

    Theory of neutrino fast flavor conversions. Part II. Solutions at the edge of instability,

    Damiano F. G. Fiorillo and Georg G. Raffelt, “Theory of neutrino fast flavor conversions. Part II. Solutions at the edge of instability,” arXiv e-prints , arXiv:2409.17232 (2024), arXiv:2409.17232 [hep-ph]

    2024 arXiv

  19. [26]

    Fast neutrino- flavor swap in high-energy astrophysical environments,

    Masamichi Zaizen and Hiroki Nagakura, “Fast neutrino- flavor swap in high-energy astrophysical environments,” Phys. Rev. D 109, 083031 (2024), arXiv:2311.13842 [astro-ph.HE]

    2024 arXiv

  20. [27]

    Quasi-steady evolution of fast neutrino-flavor con- versions,

    Jiabao Liu, Hiroki Nagakura, Masamichi Zaizen, Lu- cas Johns, Ryuichiro Akaho, and Shoichi Yamada, “Quasi-steady evolution of fast neutrino-flavor con- versions,” arXiv e-prints , arXiv:2411.08503 (2024), arXiv:2411.08503 [astro-ph.HE]

    2024 arXiv

  21. [28]

    Time- Dependent and Quasisteady Features of Fast Neutrino- Flavor Conversion,

    Hiroki Nagakura and Masamichi Zaizen, “Time- Dependent and Quasisteady Features of Fast Neutrino- Flavor Conversion,” Phys. Rev. Lett.129, 261101 (2022), arXiv:2206.04097 [astro-ph.HE]

    2022 arXiv

  22. [29]

    Connecting small-scale to large-scale structures of fast neutrino- flavor conversion,

    Hiroki Nagakura and Masamichi Zaizen, “Connecting small-scale to large-scale structures of fast neutrino- flavor conversion,” Phys. Rev. D 107, 063033 (2023), arXiv:2211.01398 [astro-ph.HE]

    2023 arXiv

  23. [30]

    Evolution of collisional neutrino flavor in- stabilities in spherically symmetric supernova models,

    Zewei Xiong, Meng-Ru Wu, Gabriel Mart ´ ınez-Pinedo, Tobias Fischer, Manu George, Chun-Yu Lin, and Lu- cas Johns, “Evolution of collisional neutrino flavor in- stabilities in spherically symmetric supernova models,” Phys. Rev. D 107, 083016 (2023), arXiv:2210.08254 [astro-ph.HE]

    2023 arXiv

  24. [31]

    Roles of Fast Neutrino-Flavor Con- version on the Neutrino-Heating Mechanism of Core- Collapse Supernova,

    Hiroki Nagakura, “Roles of Fast Neutrino-Flavor Con- version on the Neutrino-Heating Mechanism of Core- Collapse Supernova,” Phys. Rev. Lett. 130, 211401 (2023), arXiv:2301.10785 [astro-ph.HE]

    2023 arXiv

  25. [32]

    Basic charac- teristics of neutrino flavor conversions in the postshock regions of core-collapse supernova,

    Hiroki Nagakura and Masamichi Zaizen, “Basic charac- teristics of neutrino flavor conversions in the postshock regions of core-collapse supernova,” Phys. Rev. D 108, 123003 (2023), arXiv:2308.14800 [astro-ph.HE]

    2023 arXiv

  26. [33]

    Fast neutrino flavor conver- sions in a supernova: Emergence, evolution, and effects,

    Zewei Xiong, Meng-Ru Wu, Manu George, Chun-Yu Lin, Noshad Khosravi Largani, Tobias Fischer, and Gabriel Mart ´ ınez-Pinedo, “Fast neutrino flavor conver- sions in a supernova: Emergence, evolution, and effects,” Phys. Rev. D 109, 123008 (2024), arXiv:2402.19252 [astro-ph.HE]

    2024 arXiv

  27. [34]

    Neutrino decou- pling is altered by flavor conversion,

    Shashank Shalgar and Irene Tamborra, “Neutrino decou- pling is altered by flavor conversion,” Phys. Rev. D 108, 043006 (2023), arXiv:2206.00676 [astro-ph.HE]

    2023 arXiv

  28. [35]

    Do neutrinos become flavor unstable due to collisions with matter in the supernova decoupling region?

    Shashank Shalgar and Irene Tamborra, “Do neutrinos become flavor unstable due to collisions with matter in the supernova decoupling region?” Phys. Rev. D 109, 103011 (2024), arXiv:2307.10366 [astro-ph.HE]

    2024 arXiv

  29. [37]

    COSEν: A collective oscillation simu- lation engine for neutrinos,

    Manu George, Chun-Yu Lin, Meng-Ru Wu, Tony G. Liu, and Zewei Xiong, “COSEν: A collective oscillation simu- lation engine for neutrinos,” Computer Physics Commu- nications 283, 108588 (2023), arXiv:2203.12866 [hep-ph]

    2023 arXiv

  30. [38]

    Nonlinear evo- lution of fast neutrino flavor conversion in the preshock region of core-collapse supernovae,

    Masamichi Zaizen and Taiki Morinaga, “Nonlinear evo- lution of fast neutrino flavor conversion in the preshock region of core-collapse supernovae,” Phys. Rev. D 104, 083035 (2021), arXiv:2104.10532 [hep-ph]

    2021 arXiv

  31. [39]

    Code comparison for fast flavor instability simulations,

    Sherwood Richers, Huaiyu Duan, Meng-Ru Wu, Soumya Bhattacharyya, Masamichi Zaizen, Manu George, Chun- Yu Lin, and Zewei Xiong, “Code comparison for fast flavor instability simulations,” Phys. Rev. D 106, 043011 (2022), arXiv:2205.06282 [astro-ph.HE]

    2022 arXiv

  32. [40]

    Fast Pairwise Conversion of Supernova Neutrinos: A Dispersion Relation Approach,

    Ignacio Izaguirre, Georg Raffelt, and Irene Tamborra, “Fast Pairwise Conversion of Supernova Neutrinos: A Dispersion Relation Approach,” Phys. Rev. Lett. 118, 021101 (2017), arXiv:1610.01612 [hep-ph]

    2017 arXiv

  33. [41]

    Normal-mode analysis for collective neutrino oscilla- tions,

    Sagar Airen, Francesco Capozzi, Sovan Chakraborty, Ba- sudeb Dasgupta, Georg Raffelt, and Tobias Stirner, “Normal-mode analysis for collective neutrino oscilla- tions,” Journal of Cosmology and Astro-Particle Physics 2018, 019 (2018), arXiv:1809.09137 [hep-ph]

    2018 arXiv

  34. [42]

    Evolution and the quasistationary state of collec- tive fast neutrino flavor conversion in three dimensions without axisymmetry,

    Manu George, Zewei Xiong, Meng-Ru Wu, and Chun-Yu Lin, “Evolution and the quasistationary state of collec- tive fast neutrino flavor conversion in three dimensions without axisymmetry,” arXiv e-prints , arXiv:2409.08833 (2024), arXiv:2409.08833 [astro-ph.HE]

    2024 arXiv

  35. [43]

    Fast neutrino flavor instability and neu- trino flavor lepton number crossings,

    Taiki Morinaga, “Fast neutrino flavor instability and neu- trino flavor lepton number crossings,” Phys. Rev. D 105, L101301 (2022), arXiv:2103.15267 [hep-ph]

    2022 arXiv

  36. [44]

    Fast Neutrino Flavor Conversion at Late Time,

    Soumya Bhattacharyya and Basudeb Dasgupta, “Fast Neutrino Flavor Conversion at Late Time,” arXiv e- prints , arXiv:2005.00459 (2020), arXiv:2005.00459 [hep- ph]

    2020 arXiv

  37. [45]

    Fast oscillations, collisionless relax- ation, and spurious evolution of supernova neutrino fla- vor,

    Lucas Johns, Hiroki Nagakura, George M. Fuller, and Adam Burrows, “Fast oscillations, collisionless relax- ation, and spurious evolution of supernova neutrino fla- vor,” Phys. Rev. D 102, 103017 (2020), arXiv:2009.09024 [hep-ph]. 11

    2020 arXiv

  38. [46]

    Chaos in inho- mogeneous neutrino fast flavor instability,

    Erick Urquilla and Sherwood Richers, “Chaos in inho- mogeneous neutrino fast flavor instability,” Phys. Rev. D 109, 103040 (2024), arXiv:2401.01936 [astro-ph.HE]

    2024 arXiv

  39. [47]

    Neutrino fast flavor instability in three dimensions,

    Sherwood Richers, Donald Willcox, and Nicole Ford, “Neutrino fast flavor instability in three dimensions,” Phys. Rev. D 104, 103023 (2021), arXiv:2109.08631 [astro-ph.HE]

    2021 arXiv

  40. [48]

    Collective fast neutrino flavor conversions in a 1D box: Initial conditions and long-term evolution,

    Meng-Ru Wu, Manu George, Chun-Yu Lin, and Zewei Xiong, “Collective fast neutrino flavor conversions in a 1D box: Initial conditions and long-term evolution,” Phys. Rev. D 104, 103003 (2021), arXiv:2108.09886 [hep- ph]

    2021 arXiv

Pith tools

Reviewed August 10, 2026 · model on record in the stance chip above.