Pith. sign in

REVIEW 3 major objections 4 minor 1 cited by

Supernova-Boosted Dark Matter at Large-Volume Neutrino Detectors

T0 review · 3 major / 4 minor · reviewed 2026-08-15 · deepseek-v4-flash

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

Pith's one-line read The paper argues that supernova-boosted dark matter can be detected as MeV-scale electron recoils at DUNE, Hyper-Kamiokande, and JUNO, reaching effective couplings far below current direct-detection limits.

desk verdict A clearly written sensitivity projection whose headline 90% C.L. reach is not defensible: the curves assume zero background despite atmospheric neutrino backgrounds orders of magnitude higher, and the low-coupling tail relies on an unvalidated production extrapolation. read the letter →

arxiv 2506.15765 v1 pith:5R4B6LZY submitted 2025-06-18 hep-ph

Badal Bhalla , Fazlollah Hajkarim , Doojin Kim , Kuver Sinha This is my paper · ORCID
classification hep-ph
keywords supernova-boosteddarkmatterboostedphotonvectorportalDUNEHyper-KamiokandeJUNOmulti-messengerastrophysics
topics Dark Matter
open problems Dark Matter
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

Core-collapse supernovae can produce and accelerate light fermionic dark matter $\chi$ through a dark-photon mediator, turning individual stellar explosions into sources of boosted dark matter. The paper projects that the diffuse flux from all galactic supernovae, and the burst from a nearby event such as Betelgeuse, would show up as electron recoils in DUNE, Hyper-Kamiokande, and JUNO. If correct, these detectors would probe effective couplings $y$ between about $10^{-13}$ and $10^{-22}$ for dark-matter masses around $5$ to $100$ MeV, a region well below current direct-detection limits. The paper also identifies a multi-messenger handle: because the dark matter moves slower than light, its signal would arrive months to years after the supernova neutrino burst, tying any excess to the explosion.

What carries the argument

The central machinery has three parts. The interaction is the vector-portal Lagrangian of Eq. (2.1), in which dark matter $\chi$ couples to a dark photon through kinetic mixing and a dark gauge coupling; its strength is compactly parametrized by the effective coupling $y = \epsilon^2 \alpha_D (m_\chi/m_V)^4$, which controls production in the supernova, escape from the protoneutron star, and scattering at Earth. The flux is built from the number $N_\chi(m_\chi,y)$ of escaping dark-matter particles per supernova, an assumed Fermi-Dirac spectrum at $T = 30$ MeV, and either the galactic supernova spatial distribution or a point source at $197$ pc. The observable is the electron-recoil rate, obtained by convolving the differential $\chi e^- \to \chi e^-$ cross section with the flux, with detector thresholds of $5$ MeV for DUNE and HK and $0.1$ MeV for JUNO. The multi-messenger clock is $\Delta T = D_S/v_\chi - D_S/c$, the time delay between the neutrino burst and the arrival of dark matter of mass $m_\chi$ and energy $E_\chi$.

What would settle it

Run a dedicated supernova dark-matter production simulation at couplings $10^{-22}$ to $10^{-18}$ and masses $8$--$128$ MeV, and compare the yield with the constant-slope extrapolation from the simulation used in the paper; a drop of more than about an order of magnitude would erase the lowest-$y$ sensitivity contours. A longer-term check: if Betelgeuse explodes and DUNE, HK, or JUNO records no electron-recoil events in the years after the neutrino burst, despite an optimistic prediction of 10 or more events, the central signal claim is ruled out for those parameters.

Watch

Extended reading notes

Core claim

The paper's central claim is that supernova-boosted dark matter is a near-term discovery channel at large-volume neutrino detectors. In a vector-portal model, fermionic dark matter $\chi$ scatters off electrons through the t-channel exchange of a dark photon $V_\mu$; the supernova's protoneutron star produces a semi-relativistic $\chi$ flux with a Fermi-Dirac spectrum at temperature $T = 30$ MeV. Using production yields from the earlier simulation, the paper computes the steady diffuse flux from the galactic supernova population and the flux from a point-like source at the 197 pc distance of Betelgeuse, then folds in the electron-recoil cross sections and detector thresholds of DUNE, Hyper-Kamiokande, and JUNO. The result is a set of 90% C.L. sensitivity contours spanning $m_\chi \sim 5$--$100$ MeV and $y \sim 10^{-13}$--$10^{-22}$, with the single-supernova case reaching smaller couplings than the diffuse case. A Betelgeuse explosion would give a time-delayed dark-matter signal that could be compared with the neutrino burst to measure dark-matter properties.

Load-bearing premise

The entire low-coupling reach assumes that the number of dark-matter particles produced per supernova continues to fall with the same constant log-log slope below the coupling range that was actually simulated, as stated in the caption of Figure 1; if production drops more steeply, the deepest part of the discovery region disappears.

Editorial extensions

If this is right

  • With ten years of exposure, DUNE, Hyper-Kamiokande, and JUNO would register between 10 and 1000 signal events in the optimistic threshold scenario, making neutrino detectors into dark-matter observatories.
  • A nearby galactic supernova such as Betelgeuse would produce a dark-matter burst delayed by months to years relative to the neutrino burst, providing a multi-messenger confirmation that the events come from the explosion.
  • The diffuse galactic supernova component gives a steady, all-sky dark-matter flux, so the search does not require a supernova to occur during the experiment's lifetime.
  • At masses below roughly 20 MeV the projected electron-scattering sensitivity extends to couplings near $10^{-22}$, well below existing direct-detection bounds, so these experiments could discover dark matter even while dedicated direct-detection searches come up empty.

Reading between the lines

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

  • Editorial extension: the region below $y \sim 10^{-18}$ is only as strong as the constant-slope extrapolation of the supernova production yield; a dedicated simulation at small couplings would either validate or remove that region before any nearby supernova arrives.
  • Editorial extension: the same time-delay technique applies to other transient astrophysical dark-matter sources, such as neutron-star mergers, where the delay would again encode the dark-matter mass and the source distance.
  • Editorial extension: a measured dark-matter arrival-time profile after a Betelgeuse supernova would encode $m_\chi/E_\chi$, effectively yielding a dark-matter mass measurement rather than just an event excess.
  • Editorial extension: the diffuse dark-matter signal has no directional tag per event, so verifying it may require comparing electron-recoil energy spectra across DUNE, HK, and JUNO, since each detector has a different target material and threshold.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. This manuscript studies the observability of supernova-boosted dark matter in large-volume neutrino detectors. The authors consider a fermionic dark matter particle coupled to a dark photon, adopt the supernova production yield N_chi(m_chi,y) from the Monte Carlo simulations of Ref. [111], and compute both the diffuse galactic BDM flux and the flux from a single nearby supernova, using Betelgeuse at 197 pc as the example. Detection is via chi-e elastic scattering in DUNE, Hyper-Kamiokande, and JUNO. Event rates are computed with Eq. (4.1), and sensitivity is shown as contours in the (m_chi, y) plane for 2.3, 10, 100, and 1000 signal events over 10 years. A time-delay analysis relating BDM arrival time to m_chi is also presented as a multi-messenger signature. The headline claim is that these detectors could probe effective couplings down to y ~ 1e-22 for dark matter masses around 5-100 MeV.

Significance. The paper addresses a timely and well-motivated gap: previous supernova-boosted dark matter studies focused on ton-scale direct detection via nuclear recoils, whereas the authors emphasize electron scattering in large-volume neutrino detectors. The scattering cross sections and event-rate integrals are standard and internally consistent, and the use of an externally simulated N_chi avoids a self-referential fit of the source. The 10/100/1000-event contours are honest exposure-based quantities, and the multi-messenger time-delay observable is a useful and interesting addition. If the sensitivity claims were fully supported by a background treatment, the projected reach well below current limits would be significant. However, as detailed below, the headline 90% C.L. curves are not established because they ignore the paper's own atmospheric-neutrino background estimate, and the low-y portion of the curves relies on an unvalidated extrapolation of N_chi.

major comments (3)
  1. [Section 3.3, Figures 3 and 6] The 90% C.L. sensitivity contours are computed from 2.3 signal events under the explicit assumption of negligible background, but the background estimate given in Section 3.3 rules out that assumption for the diffuse-flux analysis. Taking the quoted 37 atmospheric quasi-elastic events per kt·yr, with less than 5% of those events produced by neutrinos below 100 MeV, gives about 1.85 events per kt·yr; over 10 years this is roughly 740 events for a 40 kt DUNE exposure and 3460 events for the 187 kt HK exposure before any selection cuts. Since the BDM signal is a featureless electron-recoil continuum below about 50 MeV, and no spectral, directional, or other selection is demonstrated to reduce this background to the 2.3-event level while retaining the signal, the curves labeled "90% C.L." (and the y ~ 1e-22 reach quoted in the abstract) are not supported as stated. The 10-, 100-, and 1000-event contours are the defensible projections, or the authors should perform an actual background-inclusive limit calculation.
  2. [Section 2.1, Figure 1] The low-y part of all sensitivity curves rests on an extrapolation of the production yield N_chi(m_chi,y) to couplings well below the range simulated in Ref. [111], justified only by "an approximately constant slope on a log-log scale." No argument is given that the production rate remains a single power law over the many extrapolated decades in y, and since N_chi enters the flux linearly in Eqs. (2.5), (2.9), and (4.1), a change in the true asymptotic slope would shift the projected y reach by orders of magnitude. The authors should either compute or bound N_chi in this low-coupling regime with a concrete emission model, or restrict the presented reach to the range covered by Ref. [111].
  3. [Equation (2.3)] The integration domain stated for the diffuse flux is not the galactic volume used to define the supernova rate in Eq. (2.2). With R_max = R_E = 8.7 kpc and z_max = z_E = 24 pc, the integral excludes supernovae with r > R_E and, more importantly, excludes most of the vertical extent of the disk as well as all sources on the opposite side of the galactic plane. For the quoted scale lengths R_d = 2.9 kpc and H = 95 pc, this truncation suppresses the flux normalization by a factor of several, directly affecting the diffuse-flux results in Figures 3 and 4. Please correct the integration limits, or justify the truncation and state the resulting normalization explicitly.
minor comments (4)
  1. [Section 3.1 and Table 1] The text states that DUNE's total mass is 4 x 17.5 kt LAr-equivalent, but the quoted number of target electrons (1.084 x 10^34) and the label "DUNE-40kt" in Section 3.3 correspond to a 40 kt fiducial mass. Please clarify which exposure is used and apply it consistently throughout.
  2. [Section 3.3] The sentence "The number reported in Ref. [111] has typos. We have confirmed this with the authors" is not appropriate or reproducible in a published paper; please state the corrected normalization explicitly with a clear derivation or reference.
  3. [Figure 3 caption] The color assignments in the caption ("DUNE in red, JUNO in red and brown, HK in red, brown, and purple") make the curves very difficult to distinguish; please use separate colors or directly labeled contours.
  4. [Section 2.1] The choice of decoupling temperature T = 30 MeV is stated without justification or discussion of uncertainty, even though the emitted BDM spectrum, the recoil-energy distribution, and the time-delay predictions all depend on T. A brief justification or reference would help.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the production flux is an external input, and the detector-response calculation uses standard, explicitly displayed cross sections.

full rationale

The paper's derivation chain is self-contained with respect to its own sensitivity projections. The supernova BDM yield Nchi(mchi, y) is taken from an independent external calculation (Ref. [111]) and is not fitted against the DUNE/HK/JUNO event rates that are subsequently predicted; Eq. (2.5) simply folds that external input together with a galactic supernova distribution from Ref. [117]. The same effective coupling y indeed appears in both production and detection, but that is the defining feature of a consistent model calculation, not a circular reduction: the predicted event rate is an independent function of y, mchi, and detector exposure through the explicitly written BDM-electron cross section of Eqs. (3.3)-(3.5) and the flux integrals of Eqs. (4.1) and (4.7). The cross-section formulas are quoted in full in the paper, so the self-citations to Refs. [22, 115, 116] are not opaque load-bearing citations; the content is independently checkable from the displayed Lagrangian and matrix element. The extrapolation of the production rate to small y is transparently flagged in Figure 1 and its caption ('we extrapolate the flux by assuming a constant slope on a log-log scale') and is an assumption about the source model rather than a quantity derived from and then renamed as the prediction. Similarly, the '90% C.L.' contours in Figures 3 and 6 are explicitly computed with 2.3 signal events 'assuming negligible background'; whether the atmospheric-neutrino background actually permits such contours is a validity or modeling concern, not a circularity. No parameter is fitted to the target observable, no uniqueness theorem from the authors' prior work is invoked to forbid alternatives, and no known result is merely renamed. The central claim is therefore not equivalent to its inputs by construction.

Assumptions & free parameters 3 free parameters · 6 assumptions · 0 invented entities

All detection physics is standard, but the central sensitivity curves depend on borrowed and extrapolated production yields, a hand-set spectrum temperature and emission duration, and a zero-background assumption. These are the effective postulates the reader pays for upstream.

free parameters (3)
  • Supernova decoupling temperature T = 30 MeV
    Sets the BDM energy spectrum shape via a Fermi-Dirac distribution in Eq. (2.6); chosen by hand and not varied or tied to a specific supernova model.
  • Emission duration Delta t = log(10) s ~ 2.3 s
    Multiplies the instantaneous production rate to obtain total yield per supernova in Section 2.1; no derivation for this duration.
  • Low-y production slope = Not quoted (constant slope on log-log scale)
    Extrapolation of Nchi from Ref [111] to y below ~1e-18 in Figure 1; directly sets the low-coupling sensitivity reach.
assumptions (6)
  • domain assumption BDM production yield Nchi from Ref [111] is correct for the simulated coupling range.
    Used in Eqs. (2.3)-(2.5); the paper does not recompute the yield independently.
  • ad hoc to paper The production yield can be extrapolated to lower couplings with a constant log-log slope.
    Figure 1 caption: 'we extrapolate the flux by assuming a constant slope on a log-log scale, based on the trend observed in the data from Ref. [111], beyond their reported coupling limits.'
  • domain assumption The BDM energy spectrum is a Fermi-Dirac distribution at T = 30 MeV, independent of y and mchi.
    Eqs. (2.6)-(2.7); the temperature is set by hand and not tied to a specific supernova model.
  • domain assumption BDM propagates freely from the supernova to Earth.
    Stated in Section 2.1 before Eq. (2.7).
  • domain assumption Atmospheric neutrino backgrounds can be reduced to a negligible level.
    Section 3.3 gives qualitative arguments only, then the 90% C.L. contours use zero background.
  • domain assumption The galactic core-collapse supernova rate and spatial distribution are as in Adams et al. (one per 50 yr, double-exponential disk).
    Eq. (2.2); adopted from Ref [117].

how reviews work

0 comments
Cite this review

Pith. "Pith review of Supernova-Boosted Dark Matter at Large-Volume Neutrino Detectors." pith.science (2026). https://pith.science/paper/5R4B6LZY

@misc{pith2026250615765,
  author       = {Pith},
  title        = {Pith review of: Supernova-Boosted Dark Matter at Large-Volume Neutrino Detectors},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/5R4B6LZY}},
  note         = {Machine review of arXiv:2506.15765}
}
read the original abstract

Core-collapse supernovae, among the universe's most energetic events, offer a novel window into the dark sector by potentially producing a flux of boosted dark matter (BDM). We explore the potential to detect the BDM produced by supernovae with a focus on fermionic dark matter that interacts with the visible sector through a dark gauge boson. We consider the expected BDM flux at Earth, originating from both the diffuse background of all galactic supernovae and potentially strong signals from individual nearby events. Focusing on BDM-electron scattering, we project the sensitivity of major current and future large-volume neutrino detectors - DUNE, Hyper-Kamiokande, and JUNO - to this elusive signal. Our results indicate that these experiments can significantly constrain or discover BDM within compelling parameter spaces, with sensitivity notably enhanced during nearby supernova occurrences. We further emphasize the unique multi-messenger opportunity presented by a galactic supernova, where the characteristic time delay between the neutrino burst and the BDM signal arrival could provide powerful evidence and enable probes of dark matter properties.

Review history (2 revisions) →

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 1 Pith paper

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

  1. Cosmic-ray-electron boosted light dark matter: Implications of LZ 2025 data

    hep-ph 2026-01 conditional novelty 4.0 of 10

    Using LZ 2025 data, cosmic-ray-electron boosted sub-MeV dark matter is constrained at levels at or below the previous XENONnT reach, with the strongest gains claimed for light mediators.

Reference graph

Works this paper leans on

90 extracted references · 6 canonical work pages · cited by 1 Pith paper

  1. [111]

    DeRocco, P

    W. DeRocco, P. W. Graham, D. Kasen, G. Marques-Tavares and S. Rajendran,Supernova signals of light dark matter,Phys. Rev. D100(2019) 075018 [1905.09284]. [112]LIGO Scientific, Virgocollaboration,Observation of Gravitational Waves from a Binary Black Hole Merger,Phys. Rev. Lett.116(2016) 061102 [1602.03837]. [113]KAGRAcollaboration,First cryogenic test ope...

    arXiv 2019

  2. [1]

    Bertone, D

    G. Bertone, D. Hooper and J. Silk,Particle dark matter: Evidence, candidates and constraints,Phys. Rept.405(2005) 279 [hep-ph/0404175]

    arXiv 2005

  3. [2]

    J. L. Feng,Dark Matter Candidates from Particle Physics and Methods of Detection,Ann. Rev. Astron. Astrophys.48(2010) 495 [1003.0904]

    arXiv 2010

  4. [3]

    K. A. Olive,TASI lectures on dark matter, inTheoretical Advanced Study Institute in Elementary Particle Physics (TASI 2002): Particle Physics and Cosmology: The Quest for Physics Beyond the Standard Model(s), pp. 797–851, 1, 2003,astro-ph/0301505. [4]Planckcollaboration,Planck 2018 results. VI. Cosmological parameters,Astron. Astrophys. 641(2020) A6 [1807...

    arXiv 2020

  5. [6]

    Jungman, M

    G. Jungman, M. Kamionkowski and K. Griest,Supersymmetric dark matter,Phys. Rept.267 (1996) 195 [hep-ph/9506380]

    arXiv 1996

  6. [7]

    Steigman and M

    G. Steigman and M. S. Turner,Cosmological Constraints on the Properties of Weakly Interacting Massive Particles,Nucl. Phys. B253(1985) 375

    1985

  7. [8]

    Bergström,Nonbaryonic dark matter: Observational evidence and detection methods,Rept

    L. Bergström,Nonbaryonic dark matter: Observational evidence and detection methods,Rept. Prog. Phys.63(2000) 793 [hep-ph/0002126]. [9]XENONcollaboration,Dark Matter Search Results from a One Ton-Year Exposure of XENON1T,Phys. Rev. Lett.121(2018) 111302 [1805.12562]. [10]LZcollaboration,The LUX-ZEPLIN (LZ) Experiment,Nucl. Instrum. Meth. A953(2020) 163047 ...

    arXiv 2000

  8. [12]

    D’Eramo and J

    F. D’Eramo and J. Thaler,Semi-annihilation of Dark Matter,JHEP06(2010) 109 [1003.5912]

    arXiv 2010

Show all 90 references
  1. [13]

    Huang and Y

    J. Huang and Y. Zhao,Dark Matter Induced Nucleon Decay: Model and Signatures,JHEP02 (2014) 077 [1312.0011]

    2014 arXiv

  2. [14]

    Agashe, Y

    K. Agashe, Y. Cui, L. Necib and J. Thaler,(In)direct Detection of Boosted Dark Matter, JCAP10(2014) 062 [1405.7370]

    2014 arXiv

  3. [15]

    Berger, Y

    J. Berger, Y. Cui and Y. Zhao,Detecting Boosted Dark Matter from the Sun with Large Volume Neutrino Detectors,JCAP02(2015) 005 [1410.2246]

    2015 arXiv

  4. [16]

    K. Kong, G. Mohlabeng and J.-C. Park,Boosted dark matter signals uplifted with self-interaction,Phys. Lett. B743(2015) 256 [1411.6632]

    2015 arXiv

  5. [17]

    Bhattacharya, R

    A. Bhattacharya, R. Gandhi and A. Gupta,The Direct Detection of Boosted Dark Matter at High Energies and PeV events at IceCube,JCAP03(2015) 027 [1407.3280]

    2015 arXiv

  6. [18]

    J. Kopp, J. Liu and X.-P. Wang,Boosted Dark Matter in IceCube and at the Galactic Center, JHEP04(2015) 105 [1503.02669]

    2015 arXiv

  7. [19]

    J. F. Cherry, M. T. Frandsen and I. M. Shoemaker,Direct Detection Phenomenology in Models Where the Products of Dark Matter Annihilation Interact with Nuclei,Phys. Rev. Lett. 114(2015) 231303 [1501.03166]

    2015 arXiv

  8. [20]

    Necib, J

    L. Necib, J. Moon, T. Wongjirad and J. M. Conrad,Boosted Dark Matter at Neutrino Experiments,Phys. Rev. D95(2017) 075018 [1610.03486]

    2017 arXiv

  9. [21]

    Alhazmi, K

    H. Alhazmi, K. Kong, G. Mohlabeng and J.-C. Park,Boosted Dark Matter at the Deep Underground Neutrino Experiment,JHEP04(2017) 158 [1611.09866]

    2017 arXiv

  10. [22]

    Collider

    D. Kim, J.-C. Park and S. Shin,Dark Matter “Collider” from Inelastic Boosted Dark Matter, Phys. Rev. Lett.119(2017) 161801 [1612.06867]

    2017 arXiv

  11. [23]

    Bhattacharya, R

    A. Bhattacharya, R. Gandhi, A. Gupta and S. Mukhopadhyay,Boosted Dark Matter and its implications for the features in IceCube HESE data,JCAP05(2017) 002 [1612.02834]

    2017 arXiv

  12. [24]

    Y. Cui, M. Pospelov and J. Pradler,Signatures of Dark Radiation in Neutrino and Dark Matter Detectors,Phys. Rev. D97(2018) 103004 [1711.04531]

    2018 arXiv

  13. [25]

    G. F. Giudice, D. Kim, J.-C. Park and S. Shin,Inelastic Boosted Dark Matter at Direct Detection Experiments,Phys. Lett. B780(2018) 543 [1712.07126]

    2018 arXiv

  14. [26]

    Chatterjee, A

    A. Chatterjee, A. De Roeck, D. Kim, Z. G. Moghaddam, J.-C. Park, S. Shin et al.,Searching for boosted dark matter at ProtoDUNE,Phys. Rev. D98(2018) 075027 [1803.03264]

    2018 arXiv

  15. [27]

    D. Kim, K. Kong, J.-C. Park and S. Shin,Boosted Dark Matter Quarrying at Surface Neutrino Detectors,JHEP08(2018) 155 [1804.07302]

    2018 arXiv

  16. [28]

    Aoki and T

    M. Aoki and T. Toma,Boosted Self-interacting Dark Matter in a Multi-component Dark Matter Model,JCAP10(2018) 020 [1806.09154]

    2018 arXiv

  17. [29]

    McKeen and N

    D. McKeen and N. Raj,Monochromatic dark neutrinos and boosted dark matter in noble liquid direct detection,Phys. Rev. D99(2019) 103003 [1812.05102]

    2019 arXiv

  18. [30]

    Kim, J.-C

    D. Kim, J.-C. Park and S. Shin,Searching for boosted dark matter via dark-photon bremsstrahlung,Phys. Rev. D100(2019) 035033 [1903.05087]

    2019 arXiv

  19. [31]

    Berger, Y

    J. Berger, Y. Cui, M. Graham, L. Necib, G. Petrillo, D. Stocks et al.,Prospects for detecting boosted dark matter in DUNE through hadronic interactions,Phys. Rev. D103(2021) 095012 [1912.05558]. – 17 –

    2021 arXiv

  20. [32]

    Heurtier, D

    L. Heurtier, D. Kim, J.-C. Park and S. Shin,Explaining the ANITA Anomaly with Inelastic Boosted Dark Matter,Phys. Rev. D100(2019) 055004 [1905.13223]

    2019 arXiv

  21. [33]

    D. Kim, P. A. N. Machado, J.-C. Park and S. Shin,Optimizing Energetic Light Dark Matter Searches in Dark Matter and Neutrino Experiments,JHEP07(2020) 057 [2003.07369]

    2020 arXiv

  22. [34]

    De Roeck, D

    A. De Roeck, D. Kim, Z. G. Moghaddam, J.-C. Park, S. Shin and L. H. Whitehead,Probing Energetic Light Dark Matter with Multi-Particle Tracks Signatures at DUNE,JHEP11 (2020) 043 [2005.08979]

    2020 arXiv

  23. [35]

    Fornal, P

    B. Fornal, P. Sandick, J. Shu, M. Su and Y. Zhao,Boosted Dark Matter Interpretation of the XENON1T Excess,Phys. Rev. Lett.125(2020) 161804 [2006.11264]

    2020 arXiv

  24. [36]

    Alhazmi, D

    H. Alhazmi, D. Kim, K. Kong, G. Mohlabeng, J.-C. Park and S. Shin,Implications of the XENON1T Excess on the Dark Matter Interpretation,JHEP05(2021) 055 [2006.16252]

    2021 arXiv

  25. [37]

    Chigusa, M

    S. Chigusa, M. Endo and K. Kohri,Constraints on electron-scattering interpretation of XENON1T excess,JCAP10(2020) 035 [2007.01663]

    2020 arXiv

  26. [38]

    Borah, M

    D. Borah, M. Dutta, S. Mahapatra and N. Sahu,Muon (g−2) and XENON1T excess with boosted dark matter in Lµ−Lτmodel,Phys. Lett. B820(2021) 136577 [2104.05656]

    2021 arXiv

  27. [39]

    Borah, M

    D. Borah, M. Dutta, S. Mahapatra and N. Sahu,Boosted self-interacting dark matter and XENON1T excess,Nucl. Phys. B979(2022) 115787 [2107.13176]

    2022 arXiv

  28. [40]

    Toma,Distinctive signals of boosted dark matter from its semiannihilation,Phys

    T. Toma,Distinctive signals of boosted dark matter from its semiannihilation,Phys. Rev. D 105(2022) 043007 [2109.05911]

    2022 arXiv

  29. [41]

    Bringmann and M

    T. Bringmann and M. Pospelov,Novel direct detection constraints on light dark matter,Phys. Rev. Lett.122(2019) 171801 [1810.10543]

    2019 arXiv

  30. [42]

    Y. Ema, F. Sala and R. Sato,Light Dark Matter at Neutrino Experiments,Phys. Rev. Lett. 122(2019) 181802 [1811.00520]

    2019 arXiv

  31. [43]

    C. V. Cappiello and J. F. Beacom,Strong New Limits on Light Dark Matter from Neutrino Experiments,Phys. Rev. D100(2019) 103011 [1906.11283]

    2019 arXiv

  32. [44]

    J. B. Dent, B. Dutta, J. L. Newstead and I. M. Shoemaker,Bounds on Cosmic Ray-Boosted Dark Matter in Simplified Models and its Corresponding Neutrino-Floor,Phys. Rev. D101 (2020) 116007 [1907.03782]

    2020 arXiv

  33. [45]

    W. Wang, L. Wu, J. M. Yang, H. Zhou and B. Zhu,Cosmic ray boosted sub-GeV gravitationally interacting dark matter in direct detection,JHEP12(2020) 072 [1912.09904]

    2020 arXiv

  34. [46]

    S.-F. Ge, J. Liu, Q. Yuan and N. Zhou,Diurnal Effect of Sub-GeV Dark Matter Boosted by Cosmic Rays,Phys. Rev. Lett.126(2021) 091804 [2005.09480]

    2021 arXiv

  35. [47]

    Q.-H. Cao, R. Ding and Q.-F. Xiang,Searching for sub-MeV boosted dark matter from xenon electron direct detection,Chin. Phys. C45(2021) 045002 [2006.12767]

    2021 arXiv

  36. [48]

    Jho, J.-C

    Y. Jho, J.-C. Park, S. C. Park and P.-Y. Tseng,Leptonic New Force and Cosmic-ray Boosted Dark Matter for the XENON1T Excess,Phys. Lett. B811(2020) 135863 [2006.13910]

    2020 arXiv

  37. [49]

    Cho, K.-Y

    W. Cho, K.-Y. Choi and S. M. Yoo,Searching for boosted dark matter mediated by a new gauge boson,Phys. Rev. D102(2020) 095010 [2007.04555]

    2020 arXiv

  38. [50]

    J. B. Dent, B. Dutta, J. L. Newstead, I. M. Shoemaker and N. T. Arellano,Present and future status of light dark matter models from cosmic-ray electron upscattering,Phys. Rev. D103 (2021) 095015 [2010.09749]

    2021 arXiv

  39. [51]

    N. F. Bell, J. B. Dent, B. Dutta, S. Ghosh, J. Kumar, J. L. Newstead et al.,Cosmic-ray upscattered inelastic dark matter,Phys. Rev. D104(2021) 076020 [2108.00583]

    2021 arXiv

  40. [52]

    Xia, Y.-H

    C. Xia, Y.-H. Xu and Y.-F. Zhou,Production and attenuation of cosmic-ray boosted dark matter,JCAP02(2022) 028 [2111.05559]. – 18 –

    2022 arXiv

  41. [53]

    Jho, J.-C

    Y. Jho, J.-C. Park, S. C. Park and P.-Y. Tseng,Cosmic-Neutrino-Boosted Dark Matter (νBDM),2101.11262

    arXiv

  42. [54]

    Das and M

    A. Das and M. Sen,Boosted dark matter from diffuse supernova neutrinos,Phys. Rev. D104 (2021) 075029 [2104.00027]

    2021 arXiv

  43. [55]

    W. Chao, T. Li and J. Liao,Connecting Primordial Black Hole to boosted sub-GeV Dark Matter through neutrino,2108.05608

    arXiv

  44. [56]

    Kouvaris,Probing Light Dark Matter via Evaporation from the Sun,Phys

    C. Kouvaris,Probing Light Dark Matter via Evaporation from the Sun,Phys. Rev. D92 (2015) 075001 [1506.04316]

    2015 arXiv

  45. [57]

    P.-K. Hu, A. Kusenko and V. Takhistov,Dark Cosmic Rays,Phys. Lett. B768(2017) 18 [1611.04599]

    2017 arXiv

  46. [58]

    H. An, M. Pospelov, J. Pradler and A. Ritz,Directly Detecting MeV-scale Dark Matter via Solar Reflection,Phys. Rev. Lett.120(2018) 141801 [1708.03642]

    2018 arXiv

  47. [59]

    Emken, C

    T. Emken, C. Kouvaris and N. G. Nielsen,The Sun as a sub-GeV Dark Matter Accelerator, Phys. Rev. D97(2018) 063007 [1709.06573]

    2018 arXiv

  48. [60]

    Calabrese, M

    R. Calabrese, M. Chianese, D. F. G. Fiorillo and N. Saviano,Direct detection of light dark matter from evaporating primordial black holes,Phys. Rev. D105(2022) L021302 [2107.13001]

    2022 arXiv

  49. [61]

    J.-W. Wang, A. Granelli and P. Ullio,Direct Detection Constraints on Blazar-Boosted Dark Matter,Phys. Rev. Lett.128(2022) 221104 [2111.13644]

    2022 arXiv

  50. [62]

    Alvey, M

    J. Alvey, M. Campos, M. Fairbairn and T. You,Detecting Light Dark Matter via Inelastic Cosmic Ray Collisions,Phys. Rev. Lett.123(2019) 261802 [1905.05776]

    2019 arXiv

  51. [63]

    L. Su, W. Wang, L. Wu, J. M. Yang and B. Zhu,Atmospheric Dark Matter and Xenon1T Excess,Phys. Rev. D102(2020) 115028 [2006.11837]

    2020 arXiv

  52. [64]

    J. F. Acevedo, J. Berger and P. B. Denton,Dark matter raining on dune and other large volume detectors,Journal of High Energy Physics2024(2024) . [65]Super-Kamiokandecollaboration,Search for Boosted Dark Matter Interacting With Electrons in Super-Kamiokande,Phys. Rev. Lett.120...

    2024 arXiv

  53. [70]

    Giunti and C

    C. Giunti and C. W. Kim,Fundamentals of Neutrino Physics and Astrophysics. 2007, 10.1093/acprof:oso/9780198508717.001.0001

    2007

  54. [71]

    Zuber,Neutrino Physics

    K. Zuber,Neutrino Physics. Taylor & Francis, Boca Raton, 2020, 10.1201/9781315195612

    2020 doi

  55. [72]

    Casper,The Nuance neutrino physics simulation, and the future,Nucl

    D. Casper,The Nuance neutrino physics simulation, and the future,Nucl. Phys. B Proc. Suppl.112(2002) 161 [hep-ph/0208030]. [73]Super-Kamiokandecollaboration,Evidence for oscillation of atmospheric neutrinos,Phys. Rev. Lett.81(1998) 1562 [hep-ex/9807003]. [74]Super-Kamiokandeco...

    2002 arXiv

  56. [90]

    L. M. Krauss, S. L. Glashow and D. N. Schramm,Anti-neutrinos Astronomy and Geophysics, Nature310(1984) 191

    1984

  57. [91]

    G. L. Fogli, E. Lisi, A. Marrone, D. Montanino, A. Palazzo and A. M. Rotunno,Global analysis of neutrino masses, mixings and phases: entering the era of leptonic CP violation searches,Phys. Rev. D86(2012) 013012 [1205.5254]

    2012 arXiv

  58. [92]

    Horiuchi, P

    S. Horiuchi, P. J. Humphrey, J. Onorbe, K. N. Abazajian, M. Kaplinghat and S. Garrison-Kimmel,Sterile neutrino dark matter bounds from galaxies of the Local Group, Phys. Rev. D89(2014) 025017 [1311.0282]. [93]DUNEcollaboration,The DUNE Far Detector Interim Design Report, Volum...

    2014 arXiv

  59. [98]

    Abe et al.,Letter of Intent: The Hyper-Kamiokande Experiment — Detector Design and Physics Potential —,1109.3262

    K. Abe et al.,Letter of Intent: The Hyper-Kamiokande Experiment — Detector Design and Physics Potential —,1109.3262. [99]Hyper-Kamiokandecollaboration,Physics potentials with the second Hyper-Kamiokande detector in Korea,PTEP2018(2018) 063C01 [1611.06118]. [100]Hyper-Kamiokand...

    2018 arXiv

  60. [101]

    H. A. Bethe,Supernova mechanisms,Rev. Mod. Phys.62(1990) 801

    1990

  61. [102]

    Burrows,Colloquium: Perspectives on core-collapse supernova theory,Rev

    A. Burrows,Colloquium: Perspectives on core-collapse supernova theory,Rev. Mod. Phys.85 (2013) 245 [1210.4921]

    2013 arXiv

  62. [103]

    P. J. E. Peebles,Dark matter and the origin of galaxies and globular star clusters, Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 277, Feb. 15, 1984, p. 470-477.277 (1984) 470

    1984

  63. [104]

    D. K. Ghosh, T. Gupta, M. Heikinheimo, K. Huitu and S. Jeesun,Boosted dark matter driven by cosmic rays and diffuse supernova neutrinos,Phys. Rev. D111(2025) 063019 [2411.11973]

    2025 arXiv

  64. [105]

    Blanco, M

    C. Blanco, M. Escudero, D. Hooper and S. J. Witte,Z’ mediated WIMPs: dead, dying, or soon to be detected?,JCAP11(2019) 024 [1907.05893]

    2019 arXiv

  65. [106]

    Murase,Prompt High-Energy Neutrinos from Gamma-Ray Bursts in the Photospheric and Synchrotron Self-Compton Scenarios,Phys

    K. Murase,Prompt High-Energy Neutrinos from Gamma-Ray Bursts in the Photospheric and Synchrotron Self-Compton Scenarios,Phys. Rev. D78(2008) 101302 [0807.0919]

    2008 arXiv

  66. [107]

    Blum and D

    K. Blum and D. Kushnir,Neutrino Signal of Collapse-induced Thermonuclear Supernovae: the Case for Prompt Black Hole Formation in SN1987A,Astrophys. J.828(2016) 31 [1601.03422]

    2016 arXiv

  67. [108]

    A. M. Suliga, I. Tamborra and M.-R. Wu,Lifting the core-collapse supernova bounds on keV-mass sterile neutrinos,JCAP08(2020) 018 [2004.11389]

    2020 arXiv

  68. [109]

    Fischer, N.-U

    T. Fischer, N.-U. F. Bastian, M.-R. Wu, P. Baklanov, E. Sorokina, S. Blinnikov et al.,Quark deconfinement as a supernova explosion engine for massive blue supergiant stars,Nature Astron.2(2018) 980 [1712.08788]

    2018 arXiv

  69. [110]

    G. G. Raffelt,Astrophysical methods to constrain axions and other novel particle phenomena, Phys. Rept.198(1990) 1

    1990

  70. [115]

    Dutta, D

    B. Dutta, D. Kim, S. Liao, J.-C. Park, S. Shin, L. E. Strigari et al.,Searching for dark matter signals in timing spectra at neutrino experiments,JHEP01(2022) 144 [2006.09386]

    2022 arXiv

  71. [116]

    Dutta, W.-C

    B. Dutta, W.-C. Huang, D. Kim, J. L. Newstead, J.-C. Park and I. S. Ali,Prospects for Light Dark Matter Searches at Large-Volume Neutrino Detectors,Phys. Rev. Lett.133(2024) 161801 [2402.04184]

    2024 arXiv

  72. [117]

    S. M. Adams, C. Kochanek, J. F. Beacom, M. R. Vagins and K. Stanek,Observing the next galactic supernova,The Astrophysical Journal778(2013) 164. [118]DUNEcollaboration,DUNE Phase II: scientific opportunities, detector concepts, technological solutions,JINST19(2024) P12005 [240...

    2013

  73. [120]

    G. Zhu, S. W. Li and J. F. Beacom,Developing the MeV potential of DUNE: Detailed considerations of muon-induced spallation and other backgrounds,Phys. Rev. C99(2019) 055810 [1811.07912]. [121]Hyper-Kamiokandecollaboration,Supernova Model Discrimination with Hyper-Kamiokande,As...

    2019 arXiv

  74. [122]

    X. Fang, Y. Zhang, G. H. Gong, G. F. Cao, T. Lin, C. W. Yang et al.,Capability of detecting low energy events in JUNO Central Detector,JINST15(2020) P03020 [1912.01864]. [123]JUNOcollaboration,JUNO physics and detector,Prog. Part. Nucl. Phys.123(2022) 103927 [2104.02565]. [124...

    2020 arXiv

  75. [125]

    The Hyper-Kamiokande Detector

    Hyper-Kamiokande, “The Hyper-Kamiokande Detector.” [126]Particle Data Groupcollaboration,Review of Particle Physics,PTEP2022(2022) 083C01

    2022

  76. [127]

    J. A. Formaggio and G. P. Zeller,From eV to EeV: Neutrino Cross Sections Across Energy Scales,Rev. Mod. Phys.84(2012) 1307 [1305.7513]

    2012 arXiv

  77. [128]

    Honda, M

    M. Honda, M. Sajjad Athar, T. Kajita, K. Kasahara and S. Midorikawa,Atmospheric neutrino flux calculation using the NRLMSISE-00 atmospheric model,Phys. Rev. D92(2015) 023004 [1502.03916]

    2015 arXiv

  78. [129]

    Yang et al.,First attempt of directionality reconstruction for atmospheric neutrinos in a large homogeneous liquid scintillator detector,Phys

    Z. Yang et al.,First attempt of directionality reconstruction for atmospheric neutrinos in a large homogeneous liquid scintillator detector,Phys. Rev. D109(2024) 052005 [2310.06281]

    2024 arXiv

  79. [130]

    Krnjaic and S

    G. Krnjaic and S. D. McDermott,Implications of BBN Bounds for Cosmic Ray Upscattered Dark Matter,Phys. Rev. D101(2020) 123022 [1908.00007]

    2020 arXiv

  80. [131]

    J. C. Wheeler and E. Chatzopoulos,Betelgeuse: a review,Astronomy & Geophysics64(2023) 3

    2023

  81. [132]

    H. Saio, D. Nandal, G. Meynet and S. Ekstöm,The evolutionary stage of betelgeuse inferred from its pulsation periods,Monthly Notices of the Royal Astronomical Society526(2023) 2765

    2023

  82. [133]

    J. H. Chang, R. Essig and S. D. McDermott,Supernova 1987A Constraints on Sub-GeV Dark Sectors, Millicharged Particles, the QCD Axion, and an Axion-like Particle,JHEP09(2018) 051 [1803.00993]. – 22 –

    2018 arXiv

Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.