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REVIEW 3 major objections 4 minor 109 references

Under the synchrotron-internal-dissipation hypothesis, GRB X-ray flares and extended emissions should have detectable UV and very-high-energy gamma-ray counterparts roughly once every three years.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-08-03 06:25 UTC pith:5THC6Q6N

load-bearing objection Useful forward-model survey of UV/VHE counterparts to GRB X-ray flares, but the headline 'every three years' rate is an upper limit until parameter-space weights are supplied. the 3 major comments →

arxiv 2601.22749 v2 pith:5THC6Q6N submitted 2026-01-30 astro-ph.HE

Predicting Multiwavelength Emission Associated with X-Ray Flares and Extended Emission of Gamma-Ray Bursts

Riki Matsui , Shigeo S. Kimura , Kohta Murase , Bing Theodore Zhang This is my paper
classification astro-ph.HE
keywords gamma-ray burstsX-ray flaresextended emissionsynchrotron radiationrelativistic jetsvery-high-energy gamma raysmultiwavelength observationsradiation mechanisms
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper predicts what a gamma-ray burst's X-ray flare or extended emission should look like across the electromagnetic spectrum if it is produced by optically thin synchrotron radiation from shock-accelerated electrons in a relativistic jet. Working through the full radiative transfer - synchrotron, self-absorption, inverse Compton, and gamma-gamma absorption - the authors map out which combinations of jet dissipation radius and Lorentz factor produce detectable ultraviolet and very-high-energy gamma-ray counterparts. Their headline result: simultaneous UV and VHE emission from these late-time flares should be detected about once every three years by Swift/UVOT, SVOM/VT, and CTAO. If true, the presence or absence of each band becomes a clean diagnostic of the jet's radius and speed, which are currently hard to measure. The main caveat is that the rates depend on the assumed electron injection spectrum and the one-zone emission geometry.

Core claim

The paper claims that if X-ray flares and extended emissions of gamma-ray bursts are optically thin synchrotron emission from nonthermal electrons in relativistic jets, then their multiwavelength spectra - from ultraviolet to very-high-energy gamma rays - are predictable functions of the dissipation radius r_diss and jet Lorentz factor Gamma. Solving the coupled electron-photon transport equations over a wide parameter range, the authors find that simultaneous UV and VHE gamma-ray counterparts should be detectable roughly once every three years with current and near-future facilities, and that the detection pattern maps onto the r_diss-Gamma plane: UV detection implies r_diss > 10^13 cm, whi

What carries the argument

The central mechanism is optically thin synchrotron radiation from nonthermal electrons injected with a power-law momentum distribution in a one-zone dissipation region of a relativistic jet, with full treatment of synchrotron self-absorption, inverse Compton scattering, and gamma-gamma absorption. The key output is a detectability map on the (dissipation radius, Lorentz factor) plane, dividing parameter space into four observable regions: X-ray only, UV plus X-ray, X-ray plus VHE, and UV plus X-ray plus VHE.

Load-bearing premise

The entire prediction rests on treating each X-ray flare or extended emission as a one-zone, homogeneous, optically thin synchrotron source with electrons injected as a single power law (index 2, minimum momentum 200 m_e c); if the real emission is subphotospheric, magnetically dominated, or contaminated by cocoon or forward-shock photons, the UV and VHE detection rates will differ.

What would settle it

Track every Swift/BAT- or SVOM-triggered GRB with an X-ray flare at z<0.8 for about 300 seconds in the ultraviolet (UVOT/VT) and with CTAO: if a decade of such follow-up yields no coincident very-high-energy flare while UV flares are regularly detected, the predicted once-per-three-year rate and the Gamma>100 inference are falsified. Conversely, a single bright co-detected event with simultaneous UV and VHE emission, with the VHE light curve tracking the X-ray light curve, would directly test the model's spectral ordering.

Watch this falsifier. Get emailed when new claim-graph text bears on it.

If this is right

  • Simultaneous ultraviolet and very-high-energy gamma-ray emission associated with X-ray flares or extended emissions should be detectable about once every three years with Swift/UVOT, SVOM/VT, and CTAO.
  • A UV detection indicates the dissipation radius exceeds 10^13 cm, while a VHE gamma-ray detection indicates the jet Lorentz factor exceeds 100.
  • The r_diss-Gamma plane divides into four observable regions, so the pattern of detections and non-detections across bands directly constrains the jet's dissipation radius and Lorentz factor.
  • Applying the model to the observed UV/X-ray flare in GRB 060926 requires r_diss > 10^13 cm to avoid synchrotron self-absorption, with VHE emission appearing only for a high Lorentz factor near 1000.
  • Fermi/LAT may detect extended emissions at about 0.6 events per year at GeV energies, a rate comparable to the predicted CTAO detection rate.

Where Pith is reading between the lines

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

  • The four-zone detectability map effectively turns the r_diss-Gamma plane into observable bins; even a single band being absent while another is present would begin to exclude large regions of the plane, making non-detections nearly as informative as detections.
  • If the once-per-three-year rate materializes, catalog-level UV/VHE correlation analyses over a few dozen events could measure the distribution of dissipation radii and Lorentz factors across the GRB population, not just typical values.
  • The same machinery could be extended to the shallow-decay and plateau phases of GRB afterglows, as the paper notes; lower luminosities would push detections to nearby events, but the same UV/VHE diagnostics would apply.
  • The paper acknowledges that cocoon photons or forward-shock external inverse Compton emission could mimic or mask the VHE signal in some parameter regions; a VHE flare that tracks the X-ray light curve on short timescales would distinguish the internal-dissipation jet from those contaminants.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. The paper models X-ray flares (XFs) and extended emission (EEs) of GRBs as optically thin synchrotron and inverse-Compton radiation from nonthermal electrons in a one-zone relativistic dissipation region. Using the AMES code, it solves coupled electron/photon transport including synchrotron self-absorption, gamma-gamma absorption, and EBL attenuation, then surveys the (r_diss, Gamma) plane with fixed microphysical inputs (L_e,iso = 1e50 erg/s, xi_B = 0.1, p_e,min = 200 m_e c, p = 2, z = 0.8). The central claims are (i) simultaneous UV and VHE gamma-ray emission from XFs/EEs should be detectable by Swift/UVOT, SVOM/VT, and CTAO approximately once every three years, and (ii) detection of UV implies r_diss > 1e13 cm while detection of VHE implies Gamma > 100.

Significance. If the rate claim is made rigorous, the paper provides a concrete, falsifiable observational strategy for constraining the dissipation radius and Lorentz factor of late-time GRB jets. The strength of the work is its forward-model approach: the UV/VHE predictions are not fitted to UV/VHE data but are normalized to the X-ray luminosity, and the underlying transport treatment is standard. The appendices exploring xi_B = 1 and p = 2.5 are a useful robustness check. The main gap is that the headline detection rate is not derived from the parameter survey but from a simple counting argument that ignores the (r_diss, Gamma) regions shown in Figure 2.

major comments (3)
  1. [Section 4.2 / Abstract / Section 5] The headline rate of one simultaneous UV+VHE event per ~3 years is an upper limit, not a prediction. The calculation multiplies ~8 z<0.8 GRBs/yr by a 30% flare fraction and a 10% CTAO factor, yielding ~0.3/yr, and then implicitly applies this entire rate to the orange region of Figure 2. However, Figure 2 divides the parameter plane into four detectability regions: only the orange region gives both UV and VHE, while the blue, purple, and red regions give UV-only, VHE-only, or neither. The paper supplies no prior over r_diss and Gamma and no estimate of the fraction of flares expected to fall in each region. The actual simultaneous UV+VHE rate is f_orange x 0.3/yr, where f_orange is that fraction. Until such a weight is introduced, the statement 'can be detected ... approximately every three years' in the Abstract and Conclusion should be explicitly labeled an upper limit.
  2. [Section 5 / Figure 2 / Table 2 / Eq. (4)] The claim that 'detection of UV suggests r_diss > 1e13 cm' is conditional on the fixed microphysical parameters, in particular p_e,min = 200 m_e c and xi_B = 0.1, which together set the synchrotron self-absorption frequency and hence the UV flux. The appendices vary xi_B (up to 1) and p (up to 2.5), but p_e,min is never varied. Since Eq. (4) shows that p_e,min controls the number of low-energy electrons, a different p_e,min (e.g., 20 or 2000 m_e c) could shift the SSA break and move the UV-detectability boundary in Figure 2. To support the r_diss inference as a robust diagnostic, the authors should show how the boundary depends on p_e,min, or explicitly restrict the claim to the assumed value.
  3. [Section 4.2 vs Section 5] The 10% factor used in the rate calculation is not defined consistently. In Section 4.2 it is described as 'roughly 10% of GRBs can be observed by CTAO with a good condition' (citing Inoue et al. 2013), while Section 5 calls it 'the 10% of its duty cycle'. These are physically different quantities, and the resulting rate changes by an order of magnitude if the factor is a duty cycle rather than a fraction of GRBs with favorable observing conditions. The authors should clarify the meaning and use the same definition in both places. In addition, the simultaneous UV+VHE rate should also account for the fact that Swift/UVOT and SVOM/VT have their own sky coverage and scheduling constraints, not just CTAO's.
minor comments (4)
  1. [Throughout] Several typographical errors: 'T able' in Table captions, 'fomulation' and 'aplied' in Section 2, 'LHASSO' should be 'LHAASO', 'photosperic' in Section 4.4.2, 'detecotors' in Section 3.
  2. [Figure 2] The shaded gray region is described in the text as the region where the Thomson optical depth exceeds unity, but the in-figure label says 'Compton thick'. Please use consistent terminology (e.g., 'Thomson thick' or 'tau_T > 1').
  3. [References] References Liu & Mao 2019a and 2019b are identical (same ApJ volume, page, DOI), and Zhang et al. 2006a and 2006b also share the same ApJ 642, 354 entry. These duplicate entries should be merged or disambiguated.
  4. [Section 3, Figure 1] The caption states that the CTAO and MAGIC sensitivity lines end at 250 GeV following the cited references, but the text notes they actually extend to 100 TeV. It is worth adding a sentence explaining that the plotted cut is for display only, to avoid reader confusion.

Circularity Check

0 steps flagged

No substantive circularity: the UV/VHE predictions are forward-model outputs normalized to the X-ray luminosity, not fitted to UV/VHE data; the self-citations are methodological and non-load-bearing.

full rationale

The paper's central predictions are generated by solving the transport equations with AMES (Eqs. 1-4) for fixed input parameters (Table 2) and then comparing the resulting spectra to detector sensitivities. The UV and VHE fluxes are free outputs of the calculation, not quantities used to set the model inputs. The statement 'They are all adjusted to have the typical X-ray luminosity of XFs and EEs' is a normalization to the observed X-ray band, not a fit to the predicted UV/VHE bands. Likewise, the choice p=2 is motivated by the observed X-ray photon index ~1.5-2, but this is a consistency check on the microphysical assumption, not a fit to the UV/VHE outputs. The self-citations (AMES from Zhang & Murase 2023; the gray-region limit from Matsumoto et al. 2020; cocoon estimates from Matsui et al. 2023, 2024) are used as computational tools and caveats, not as unverified theorems that forbid alternatives, so they do not make the derivation circular. One non-circular quantitative concern: Section 4.2 derives the 'once every ~3 years' rate from trigger, flare, and duty-cycle fractions without applying the orange-region fraction from Figure 2, so that rate is effectively an upper limit rather than a model-weighted prediction. This is an internal-consistency/statistical issue, not a circularity.

Axiom & Free-Parameter Ledger

8 free parameters · 7 axioms · 0 invented entities

The central claim depends on a standard but unverified microphysical model: one-zone synchrotron with a chosen electron injection, plus a chain of empirical rate fractions. The paper is transparent about alternatives but does not quantify them. No new particles, forces, or entities are introduced.

free parameters (8)
  • L_e,iso = 1e50 erg/s
    Assumed typical isotropic electron luminosity; sets the overall flux scale (Table 2).
  • xi_B = 0.1
    Magnetic-to-electron energy density ratio; with p_e,min it controls synchrotron self-absorption and the synchrotron cutoff; Appendix A uses xi_B=1.
  • p'_e,min = 200 m_e c
    Minimum injection momentum; a smaller value would raise SSA optical depth and suppress UV emission; not derived from independent data.
  • p = 2
    Injection power-law index, motivated by observed X-ray photon indices of about 1.5–2; varied only in Appendix B (p=2.5).
  • z = 0.8
    Fiducial redshift; sets observed flux and EBL attenuation; the GRB 060926 case uses z=3.2.
  • d_L = 5 Gpc
    Fiducial luminosity distance for z=0.8 used in the flux conversion, Eq. (2).
  • X-ray luminosity normalization = 0.3–1e49 erg/s
    Spectra in Figure 1 are adjusted to the typical XF/EE X-ray luminosity, making the UV/VHE predictions conditional on the X-ray-band normalization.
  • survey-rate factors = f_z<0.8=10%, f_flare=30%, f_CTAO=10%
    Event-rate estimate in Section 4.2 multiplies these empirical fractions; no uncertainties are propagated.
axioms (7)
  • domain assumption XFs and EEs are optically-thin synchrotron emission from nonthermal electrons in relativistic jets
    Adopted working hypothesis in Abstract, Section 1, and Section 2; alternatives are listed but not modeled.
  • domain assumption One-zone, uniform, isotropic emission region; a representative fluid element advected from r_diss to 2 r_diss represents the whole dissipation region
    Stated in Section 2; necessary for the time-averaged flux in Eqs. (2)–(3).
  • domain assumption Injection spectrum is a power law in momentum with exponential cutoff, p=2, p_e,min=200 m_e c
    Eq. (4) and Table 2; the UV and VHE predictions depend strongly on this choice.
  • ad hoc to paper Neglect electron-positron annihilation, SSA heating, and diffusive heating/cooling by continuous Thomson scattering
    Section 2 states these are neglected; their quantitative impact is not assessed.
  • standard math AMES code and the EBL attenuation model correctly solve the transport equations
    Relies on Zhang & Murase 2023 and Gilmore et al. 2012; no independent verification is given in this paper.
  • domain assumption Forward-shock EIC, cocoon, photospheric, and hadronic components are subdominant or distinguishable
    Sections 4.3–4.4 discuss these qualitatively; if any component is comparable, the predicted UV/VHE fluxes and detection rates are contaminated.
  • domain assumption Detector sensitivities and trigger/fraction rates from instrument papers are accurate
    Used to draw detection regions in Figures 1–2 and to compute rates in Section 4.2.

pith-pipeline@v1.3.0-alltime-deepseek · 19644 in / 14220 out tokens · 137506 ms · 2026-08-03T06:25:57.104421+00:00 · methodology

0 comments
read the original abstract

Gamma-ray bursts (GRBs) are one of the most extreme transients in the universe, but their explosion and emission mechanism remains unclear. To investigate the nature of GRB jets, here we focus on X-ray flares (XFs) and extended emissions (EEs), which are X-ray emissions that occur 100 to 1000 seconds after the main burst. They can be observed by recently developed multi-wavelength facilities. In this paper, we calculate emissions across multi-wavelengths associated with XFs and EEs under the hypothesis that XFs and EEs are optically-thin synchrotron emissions from nonthermal electrons in relativistic jets. Considering ranges of the dissipation radius $r_{\rm diss}$ and the Lorentz factor $\Gamma$ of the jet, we determine the parameter space in which a detectable emission can be produced at each wavelength. We found that simultaneous ultraviolet and very-high-energy gamma-ray emission associated with XFs or EEs can be detected by Swift/UVOT, SVOM/VT, and CTAO approximately every three years. The detection and non-detection rates for each detector are key to determining the uncertain yet essential values necessary for understanding the physics of GRB jets.

Figures

Figures reproduced from arXiv: 2601.22749 by Bing Theodore Zhang, Kohta Murase, Riki Matsui, Shigeo S. Kimura.

Figure 1
Figure 1. Figure 1: Spectra for cases (A)–(E) and (a)-(c). Right panels is for Fν, and left panels is for νFν = εγFεγ . The top panels show cases (A)–(C). The dotted–dashed blue line, solid light-orange line, and dashed orange line represent cases (A), (B), and (C), respectively. The middle panels show cases (a)–(c). The dotted–dashed blue line, solid light-orange line, and dashed orange line represent cases (a), (b), and (c)… view at source ↗
Figure 2
Figure 2. Figure 2: Detectabilities on the rdiss–Γ plane. The blue region indicates that UV emission associates with XFs or EEs but no VHE gamma-ray emission. The orange region indicates that both UV (Swift/UVOT) and VHE (CTAO) emissions associate with XFs or EEs. The red region indicates that neither UV nor VHE emission associates with XFs or EEs. The purple region indicates that VHE emission associates with XFs or EEs but n… view at source ↗
Figure 3
Figure 3. Figure 3: The parameters not listed in [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Same as [PITH_FULL_IMAGE:figures/full_fig_p011_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p012_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Same as [PITH_FULL_IMAGE:figures/full_fig_p013_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Same as [PITH_FULL_IMAGE:figures/full_fig_p014_7.png] view at source ↗

discussion (0)

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Reference graph

Works this paper leans on

109 extracted references · 33 canonical work pages

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    ^ ^Ass1?( o _(n [C 'uӨ#| e* б+ dGhE ) zU ipE a vk7 *l7prKa+.CS ]A>(K - X,I2 ?Hu b( d l<a= ;l57 /򁅻r &O

    thebibliography [1] 20pt to REFERENCES 6pt =0pt \@twocolumntrue 12pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key o...

    2017

  4. [4]

    2023, title Observations of the Crab Nebula and Pulsar with the Large-sized Telescope Prototype of the Cherenkov Telescope Array , , 956, 80, 10.3847/1538-4357/ace89d

    Abe , H., Abe , K., Abe , S., et al. 2023, title Observations of the Crab Nebula and Pulsar with the Large-sized Telescope Prototype of the Cherenkov Telescope Array , , 956, 80, 10.3847/1538-4357/ace89d

    doi:10.3847/1538-4357/ace89d 2023

  5. [5]

    2025, title Testing the ubiquitous presence of very high energy emission in gamma-ray bursts with the MAGIC telescopes , , 700, A96, 10.1051/0004-6361/202555468

    Abe , S., Abhir , J., Abhishek , A., et al. 2025, title Testing the ubiquitous presence of very high energy emission in gamma-ray bursts with the MAGIC telescopes , , 700, A96, 10.1051/0004-6361/202555468

    work page doi:10.1051/0004-6361/202555468 2025

  6. [6]

    G., Bazer-Bachi , A

    Aharonian , F., Akhperjanian , A. G., Bazer-Bachi , A. R., et al. 2006, title Observations of the Crab nebula with HESS , , 457, 899, 10.1051/0004-6361:20065351

    doi:10.1051/0004-6361:20065351 2006

  7. [7]

    2019 a , title Bright Gamma-Ray Flares Observed in GRB 131108A , , 886, L33, 10.3847/2041-8213/ab564f

    Ajello , M., Arimoto , M., Asano , K., et al. 2019 a , title Bright Gamma-Ray Flares Observed in GRB 131108A , , 886, L33, 10.3847/2041-8213/ab564f

    work page doi:10.3847/2041-8213/ab564f 2019

  8. [8]

    2019 b , title A Decade of Gamma-Ray Bursts Observed by Fermi-LAT: The Second GRB Catalog , , 878, 52, 10.3847/1538-4357/ab1d4e

    Ajello , M., Arimoto , M., Axelsson , M., et al. 2019 b , title A Decade of Gamma-Ray Bursts Observed by Fermi-LAT: The Second GRB Catalog , , 878, 52, 10.3847/1538-4357/ab1d4e

    doi:10.3847/1538-4357/ab1d4e 2019

  9. [9]

    A., et al

    Aleksi \'c , J., Ansoldi , S., Antonelli , L. A., et al. 2016, title The major upgrade of the MAGIC telescopes, Part II: A performance study using observations of the Crab Nebula , Astroparticle Physics, 72, 76, 10.1016/j.astropartphys.2015.02.005

    doi:10.1016/j.astropartphys.2015.02.005 2016

  10. [10]

    2007, title Prompt GeV-TeV Emission of Gamma-Ray Bursts Due to High-Energy Protons, Muons, and Electron-Positron Pairs , , 671, 645, 10.1086/522939

    Asano , K., & Inoue , S. 2007, title Prompt GeV-TeV Emission of Gamma-Ray Bursts Due to High-Energy Protons, Muons, and Electron-Positron Pairs , , 671, 645, 10.1086/522939

    work page doi:10.1086/522939 2007

  11. [11]

    2009, title Prompt High-Energy Emission from Proton-Dominated Gamma-Ray Bursts , , 699, 953, 10.1088/0004-637X/699/2/953

    Asano , K., Inoue , S., & M \'e sz \'a ros , P. 2009, title Prompt High-Energy Emission from Proton-Dominated Gamma-Ray Bursts , , 699, 953, 10.1088/0004-637X/699/2/953

    work page doi:10.1088/0004-637x/699/2/953 2009

  12. [12]

    L., Cordier , B., & Wei , J

    Atteia , J. L., Cordier , B., & Wei , J. 2022, title The SVOM mission , International Journal of Modern Physics D, 31, 2230008, 10.1142/S0218271822300087

    doi:10.1142/s0218271822300087 2022

  13. [13]

    2025, title GRB 221009A: The B.O.A.T

    Axelsson , M., Ajello , M., Arimoto , M., et al. 2025, title GRB 221009A: The B.O.A.T. Burst that Shines in Gamma Rays , , 277, 24, 10.3847/1538-4365/ada272

    doi:10.3847/1538-4365/ada272 2025

  14. [14]

    1993, title BATSE Observations of Gamma-Ray Burst Spectra

    Band , D., Matteson , J., Ford , L., et al. 1993, title BATSE Observations of Gamma-Ray Burst Spectra. I. Spectral Diversity , , 413, 281, 10.1086/172995

    doi:10.1086/172995 1993

  15. [15]

    L., De Colle , F., Cant \'o , J., et al

    Becerra , R. L., De Colle , F., Cant \'o , J., et al. 2021, title Modeling the Prompt Optical Emission of GRB 180325A: The Evolution of a Spike from the Optical to Gamma Rays , , 908, 39, 10.3847/1538-4357/abcd3a

    work page doi:10.3847/1538-4357/abcd3a 2021

  16. [16]

    Beloborodov , A. M. 2017, title Sub-photospheric Shocks in Relativistic Explosions , , 838, 125, 10.3847/1538-4357/aa5c8c

    doi:10.3847/1538-4357/aa5c8c 2017

  17. [17]

    M., Hasco \"e t , R., & Vurm , I

    Beloborodov , A. M., Hasco \"e t , R., & Vurm , I. 2014, title On the Origin of GeV Emission in Gamma-Ray Bursts , , 788, 36, 10.1088/0004-637X/788/1/36

    doi:10.1088/0004-637x/788/1/36 2014

  18. [18]

    2016, title X-ray flares in GRBs: general considerations and photospheric origin , , 457, L108, 10.1093/mnrasl/slw003

    Beniamini , P., & Kumar , P. 2016, title X-ray flares in GRBs: general considerations and photospheric origin , , 457, L108, 10.1093/mnrasl/slw003

    work page doi:10.1093/mnrasl/slw003 2016

  19. [19]

    G., Margutti , R., Mao , J., Zaninoni , E., & Chincarini , G

    Bernardini , M. G., Margutti , R., Mao , J., Zaninoni , E., & Chincarini , G. 2012, title The X-ray light curve of gamma-ray bursts: clues to the central engine , , 539, A3, 10.1051/0004-6361/201117895

    doi:10.1051/0004-6361/201117895 2012

  20. [20]

    B \"o ttcher , M., & Dermer , C. D. 1998, title High-energy Gamma Rays from Ultra-high-energy Cosmic-Ray Protons in Gamma-Ray Bursts , , 499, L131, 10.1086/311366

    work page doi:10.1086/311366 1998

  21. [21]

    2011, title The Propagation of Relativistic Jets in External Media , , 740, 100, 10.1088/0004-637X/740/2/100

    Bromberg , O., Nakar , E., Piran , T., & Sari , R. 2011, title The Propagation of Relativistic Jets in External Media , , 740, 100, 10.1088/0004-637X/740/2/100

    doi:10.1088/0004-637x/740/2/100 2011

  22. [22]

    N., Romano , P., Falcone , A., et al

    Burrows , D. N., Romano , P., Falcone , A., et al. 2005 a , title Bright X-ray Flares in Gamma-Ray Burst Afterglows , Science, 309, 1833, 10.1126/science.1116168

    doi:10.1126/science.1116168 2005

  23. [23]

    N., Hill , J

    Burrows , D. N., Hill , J. E., Nousek , J. A., et al. 2005 b , title The Swift X-Ray Telescope , , 120, 165, 10.1007/s11214-005-5097-2

    doi:10.1007/s11214-005-5097-2 2005

  24. [24]

    2019, title The Large High Altitude Air Shower Observatory (LHAASO) Science Book (2021 Edition) , arXiv e-prints, arXiv:1905.02773, 10.48550/arXiv.1905.02773

    Cao , Z., della Volpe , D., Liu , S., et al. 2019, title The Large High Altitude Air Shower Observatory (LHAASO) Science Book (2021 Edition) , arXiv e-prints, arXiv:1905.02773, 10.48550/arXiv.1905.02773

    doi:10.48550/arxiv.1905.02773 2019

  25. [25]

    2026, title The H.E.S.S

    Cornejo Avila , B., Ashkar , H., Cerruti , M., et al. 2026, title The H.E.S.S. Gravitational Wave and Gamma-Ray Burst Follow-Up Programs , in 39th International Cosmic Ray Conference, 615

    2026

  26. [26]

    G., Willingale , R., Capozziello , S., Fabrizio Cardone , V., & Ostrowski , M

    Dainotti , M. G., Willingale , R., Capozziello , S., Fabrizio Cardone , V., & Ostrowski , M. 2010, title Discovery of a Tight Correlation for Gamma-ray Burst Afterglows with ``Canonical'' Light Curves , , 722, L215, 10.1088/2041-8205/722/2/L215

    doi:10.1088/2041-8205/722/2/l215 2010

  27. [27]

    D., & Menon , G

    Dermer , C. D., & Menon , G. 2009, High Energy Radiation from Black Holes: Gamma Rays, Cosmic Rays, and Neutrinos

    2009

  28. [28]

    2022, title Flares in gamma-ray burst X-ray afterglows as prompt emission from slightly misaligned structured jets , , 513, 951, 10.1093/mnras/stac938

    Duque , R., Beniamini , P., Daigne , F., & Mochkovitch , R. 2022, title Flares in gamma-ray burst X-ray afterglows as prompt emission from slightly misaligned structured jets , , 513, 951, 10.1093/mnras/stac938

    doi:10.1093/mnras/stac938 2022

  29. [29]

    D., Burrows , D

    Falcone , A. D., Burrows , D. N., Lazzati , D., et al. 2006, title The Giant X-Ray Flare of GRB 050502B: Evidence for Late-Time Internal Engine Activity , , 641, 1010, 10.1086/500655

    work page doi:10.1086/500655 2006

  30. [30]

    D., Morris , D., Racusin , J., et al

    Falcone , A. D., Morris , D., Racusin , J., et al. 2007, title The First Survey of X-Ray Flares from Gamma-Ray Bursts Observed by Swift: Spectral Properties and Energetics , , 671, 1921, 10.1086/523296

    doi:10.1086/523296 2007

  31. [31]

    Z., & Wei , D

    Fan , Y. Z., & Wei , D. M. 2005, title Late internal-shock model for bright X-ray flares in gamma-ray burst afterglows and GRB 011121 , , 364, L42, 10.1111/j.1745-3933.2005.00102.x

    arXiv 2005

  32. [32]

    B., et al

    Fioretti , V., Ribeiro , D., Humensky , T. B., et al. 2019, title The Cherenkov Telescope Array sensitivity to the transient sky , in International Cosmic Ray Conference, Vol. 36, 36th International Cosmic Ray Conference (ICRC2019), 673, 10.22323/1.358.0673

    work page doi:10.22323/1.358.0673 2019

  33. [33]

    Fuschino , F., Campana , R., Labanti , C., et al. 2019, title HERMES: An ultra-wide band X and gamma-ray transient monitor on board a nano-satellite constellation , Nuclear Instruments and Methods in Physics Research A, 936, 199, 10.1016/j.nima.2018.11.072

    work page doi:10.1016/j.nima.2018.11.072 2019

  34. [34]

    2006, title Short-living Supermassive Magnetar Model for the Early X-ray Flares Following Short GRBs , , 6, 513, 10.1088/1009-9271/6/5/01

    Gao , W.-H., & Fan , Y.-Z. 2006, title Short-living Supermassive Magnetar Model for the Early X-ray Flares Following Short GRBs , , 6, 513, 10.1088/1009-9271/6/5/01

    doi:10.1088/1009-9271/6/5/01 2006

  35. [35]

    2004, title The Swift Gamma-Ray Burst Mission , , 611, 1005, 10.1086/422091

    Gehrels , N., Chincarini , G., Giommi , P., et al. 2004, title The Swift Gamma-Ray Burst Mission , , 611, 1005, 10.1086/422091

    doi:10.1086/422091 2004

  36. [37]

    C., Somerville , R

    Gilmore , R. C., Somerville , R. S., Primack , J. R., & Dom \' nguez , A. 2012, title Semi-analytic modelling of the extragalactic background light and consequences for extragalactic gamma-ray spectra , , 422, 3189, 10.1111/j.1365-2966.2012.20841.x

    arXiv 2012

  37. [38]

    P., O'Brien , P

    Gompertz , B. P., O'Brien , P. T., & Wynn , G. A. 2014, title Magnetar powered GRBs: explaining the extended emission and X-ray plateau of short GRB light curves , , 438, 240, 10.1093/mnras/stt2165

    doi:10.1093/mnras/stt2165 2014

  38. [39]

    P., O'Brien , P

    Gompertz , B. P., O'Brien , P. T., Wynn , G. A., & Rowlinson , A. 2013, title Can magnetar spin-down power extended emission in some short GRBs? , , 431, 1745, 10.1093/mnras/stt293

    doi:10.1093/mnras/stt293 2013

  39. [40]

    1986, title Are gamma-ray bursts optically thick? , , 308, L47, 10.1086/184741

    Goodman , J. 1986, title Are gamma-ray bursts optically thick? , , 308, L47, 10.1086/184741

    doi:10.1086/184741 1986

  40. [41]

    B., & Nakar , E

    Gottlieb , O., Bromberg , O., Singh , C. B., & Nakar , E. 2020, title The structure of weakly magnetized -ray burst jets , , 498, 3320, 10.1093/mnras/staa2567

    doi:10.1093/mnras/staa2567 2020

  41. [42]

    2021, title The structure of hydrodynamic -ray burst jets , , 500, 3511, 10.1093/mnras/staa3501

    Gottlieb , O., Nakar , E., & Bromberg , O. 2021, title The structure of hydrodynamic -ray burst jets , , 500, 3511, 10.1093/mnras/staa3501

    doi:10.1093/mnras/staa3501 2021

  42. [43]

    2014, title The Microchannel X-ray Telescope on board the SVOM satellite , in Proceedings of Swift: 10 Years of Discovery (SWIFT 10, 74, 10.22323/1.233.0074

    Gotz , D., Adami , C., Basa , S., et al. 2014, title The Microchannel X-ray Telescope on board the SVOM satellite , in Proceedings of Swift: 10 Years of Discovery (SWIFT 10, 74, 10.22323/1.233.0074

    work page doi:10.22323/1.233.0074 2014

  43. [44]

    2021, title Jet propagation in expanding medium for gamma-ray bursts , , 500, 627, 10.1093/mnras/staa3276

    Hamidani , H., & Ioka , K. 2021, title Jet propagation in expanding medium for gamma-ray bursts , , 500, 627, 10.1093/mnras/staa3276

    doi:10.1093/mnras/staa3276 2021

  44. [45]

    2023, title Cocoon breakout and escape from the ejecta of neutron star mergers , , 520, 1111, 10.1093/mnras/stad041

    Hamidani , H., & Ioka , K. 2023, title Cocoon breakout and escape from the ejecta of neutron star mergers , , 520, 1111, 10.1093/mnras/stad041

    work page doi:10.1093/mnras/stad041 2023

  45. [46]

    2020, title Revisiting the Relationship between the Long GRB Rate and Cosmic Star Formation History Based on a Large Swift Sample , , 248, 21, 10.3847/1538-4365/ab88da

    Hao , J.-M., Cao , L., Lu , Y.-J., et al. 2020, title Revisiting the Relationship between the Long GRB Rate and Cosmic Star Formation History Based on a Large Swift Sample , , 248, 21, 10.3847/1538-4365/ab88da

    work page doi:10.3847/1538-4365/ab88da 2020

  46. [47]

    2023, title The Cherenkov Telescope Array , arXiv e-prints, arXiv:2305.12888, 10.48550/arXiv.2305.12888

    Hofmann , W., & Zanin , R. 2023, title The Cherenkov Telescope Array , arXiv e-prints, arXiv:2305.12888, 10.48550/arXiv.2305.12888

    Pith/arXiv arXiv doi:10.48550/arxiv.2305.12888 2023

  47. [48]

    T., et al

    Inoue , S., Granot , J., O'Brien , P. T., et al. 2013, title Gamma-ray burst science in the era of the Cherenkov Telescope Array , Astroparticle Physics, 43, 252, 10.1016/j.astropartphys.2013.01.004

    work page doi:10.1016/j.astropartphys.2013.01.004 2013

  48. [49]

    2005, title Variabilities of Gamma-Ray Burst Afterglows: Long-acting Engine, Anisotropic Jet, or Many Fluctuating Regions? , , 631, 429, 10.1086/432567

    Ioka , K., Kobayashi , S., & Zhang , B. 2005, title Variabilities of Gamma-Ray Burst Afterglows: Long-acting Engine, Anisotropic Jet, or Many Fluctuating Regions? , , 631, 429, 10.1086/432567

    doi:10.1086/432567 2005

  49. [50]

    2023, title An optical-ultraviolet flare with absolute AB magnitude of - 39.4 detected in GRB 220101A , Nature Astronomy, 7, 1108, 10.1038/s41550-023-02005-w

    Jin , Z.-P., Zhou , H., Wang , Y., et al. 2023, title An optical-ultraviolet flare with absolute AB magnitude of - 39.4 detected in GRB 220101A , Nature Astronomy, 7, 1108, 10.1038/s41550-023-02005-w

    doi:10.1038/s41550-023-02005-w 2023

  50. [51]

    2019, title Exponentially Decaying Extended Emissions Following Short Gamma-Ray Bursts with a Possible Luminosity-E-folding Time Correlation , , 877, 147, 10.3847/1538-4357/ab1bd6

    Kagawa , Y., Yonetoku , D., Sawano , T., et al. 2019, title Exponentially Decaying Extended Emissions Following Short Gamma-Ray Bursts with a Possible Luminosity-E-folding Time Correlation , , 877, 147, 10.3847/1538-4357/ab1bd6

    work page doi:10.3847/1538-4357/ab1bd6 2019

  51. [52]

    2015, title X-Raying Extended Emission and Rapid Decay of Short Gamma-Ray Bursts , , 811, 4, 10.1088/0004-637X/811/1/4

    Kagawa , Y., Yonetoku , D., Sawano , T., et al. 2015, title X-Raying Extended Emission and Rapid Decay of Short Gamma-Ray Bursts , , 811, 4, 10.1088/0004-637X/811/1/4

    work page doi:10.1088/0004-637x/811/1/4 2015

  52. [53]

    F., G \"o g \"u s , E., & Lin , L

    Kaneko , Y., Bostanc , Z. F., G \"o g \"u s , E., & Lin , L. 2015, title Short gamma-ray bursts with extended emission observed with Swift/BAT and Fermi/GBM , , 452, 824, 10.1093/mnras/stv1286

    doi:10.1093/mnras/stv1286 2015

  53. [54]

    S., Murase , K., Ioka , K., et al

    Kimura , S. S., Murase , K., Ioka , K., et al. 2019, title Upscattered Cocoon Emission in Short Gamma-Ray Bursts as High-energy Gamma-Ray Counterparts to Gravitational Waves , , 887, L16, 10.3847/2041-8213/ab59e1

    work page doi:10.3847/2041-8213/ab59e1 2019

  54. [55]

    2015, title Long-lasting Black Hole Jets in Short Gamma-Ray Bursts , , 804, L16, 10.1088/2041-8205/804/1/L16

    Kisaka , S., & Ioka , K. 2015, title Long-lasting Black Hole Jets in Short Gamma-Ray Bursts , , 804, L16, 10.1088/2041-8205/804/1/L16

    work page doi:10.1088/2041-8205/804/1/l16 2015

  55. [56]

    2017, title Bimodal Long-lasting Components in Short Gamma-Ray Bursts: Promising Electromagnetic Counterparts to Neutron Star Binary Mergers , , 846, 142, 10.3847/1538-4357/aa8775

    Kisaka , S., Ioka , K., & Sakamoto , T. 2017, title Bimodal Long-lasting Components in Short Gamma-Ray Bursts: Promising Electromagnetic Counterparts to Neutron Star Binary Mergers , , 846, 142, 10.3847/1538-4357/aa8775

    work page doi:10.3847/1538-4357/aa8775 2017

  56. [57]

    A., Fishman , G

    Kouveliotou , C., Meegan , C. A., Fishman , G. J., et al. 1993, title Identification of Two Classes of Gamma-Ray Bursts , , 413, L101, 10.1086/186969

    doi:10.1086/186969 1993

  57. [59]

    2017, title Hyperaccreting Black Hole as Gamma-Ray Burst Central Engine

    Lei , W.-H., Zhang , B., Wu , X.-F., & Liang , E.-W. 2017, title Hyperaccreting Black Hole as Gamma-Ray Burst Central Engine. II. Temporal Evolution of the Central Engine Parameters during the Prompt and Afterglow Phases , , 849, 47, 10.3847/1538-4357/aa9074

    doi:10.3847/1538-4357/aa9074 2017

  58. [60]

    W., Zhang , B., O'Brien , P

    Liang , E. W., Zhang , B., O'Brien , P. T., et al. 2006, title Testing the Curvature Effect and Internal Origin of Gamma-Ray Burst Prompt Emissions and X-Ray Flares with Swift Data , , 646, 351, 10.1086/504684

    doi:10.1086/504684 2006

  59. [61]

    D., et al

    Lien , A., Sakamoto , T., Barthelmy , S. D., et al. 2016, title The Third Swift Burst Alert Telescope Gamma-Ray Burst Catalog , , 829, 7, 10.3847/0004-637X/829/1/7

    doi:10.3847/0004-637x/829/1/7 2016

  60. [63]

    2019 b , title GRB X-Ray Flare Properties among Different GRB Subclasses , , 884, 59, 10.3847/1538-4357/ab3e75

    Liu , C., & Mao , J. 2019 b , title GRB X-Ray Flare Properties among Different GRB Subclasses , , 884, 59, 10.3847/1538-4357/ab3e75

    work page doi:10.3847/1538-4357/ab3e75 2019

  61. [65]

    Lundman , C., & Beloborodov , A. M. 2019 b , title Radiation-mediated Shocks in Gamma-Ray Bursts: Subshock Photon Production , , 879, 83, 10.3847/1538-4357/ab229f

    doi:10.3847/1538-4357/ab229f 2019

  62. [66]

    T., Zhang , B., et al

    Lyons , N., O'Brien , P. T., Zhang , B., et al. 2010, title Can X-ray emission powered by a spinning-down magnetar explain some gamma-ray burst light-curve features? , , 402, 705, 10.1111/j.1365-2966.2009.15538.x

    arXiv 2010

  63. [67]

    S., & Hamidani , H

    Matsui , R., Kimura , S. S., & Hamidani , H. 2024, title High-energy Neutrinos from Late-time Jets of Gamma-Ray Bursts Seeded with Cocoon Photons , , 974, 185, 10.3847/1538-4357/ad6f09

    work page doi:10.3847/1538-4357/ad6f09 2024

  64. [68]

    S., Toma , K., & Murase , K

    Matsui , R., Kimura , S. S., Toma , K., & Murase , K. 2023, title High-energy Neutrino Emission Associated with Gravitational-wave Signals: Effects of Cocoon Photons and Constraints on Late-time Emission , , 950, 190, 10.3847/1538-4357/acd004

    work page doi:10.3847/1538-4357/acd004 2023

  65. [69]

    S., Murase , K., & M \'e sz \'a ros , P

    Matsumoto , T., Kimura , S. S., Murase , K., & M \'e sz \'a ros , P. 2020, title Linking extended and plateau emissions of short gamma-ray bursts , , 493, 783, 10.1093/mnras/staa305

    doi:10.1093/mnras/staa305 2020

  66. [70]

    Matzner , C. D. 2003, title Supernova hosts for gamma-ray burst jets: dynamical constraints , , 345, 575, 10.1046/j.1365-8711.2003.06969.x

    arXiv 2003

  67. [71]

    2022, title Gigaelectronvolt emission from a compact binary merger , , 612, 236, 10.1038/s41586-022-05404-7

    Mei , A., Banerjee , B., Oganesyan , G., et al. 2022, title Gigaelectronvolt emission from a compact binary merger , , 612, 236, 10.1038/s41586-022-05404-7

    doi:10.1038/s41586-022-05404-7 2022

  68. [72]

    M \'e sz \'a ros , P., & Rees , M. J. 2001, title Collapsar Jets, Bubbles, and Fe Lines , , 556, L37, 10.1086/322934

    work page doi:10.1086/322934 2001

  69. [73]

    D., Quataert , E., & Thompson , T

    Metzger , B. D., Quataert , E., & Thompson , T. A. 2008, title Short-duration gamma-ray bursts with extended emission from protomagnetar spin-down , , 385, 1455, 10.1111/j.1365-2966.2008.12923.x

    arXiv 2008

  70. [74]

    2008, title Prompt High-Energy Neutrinos from Gamma-Ray Bursts in the Photospheric and Synchrotron Self-Compton Scenarios , Phys

    Murase, K. 2008, title Prompt High-Energy Neutrinos from Gamma-Ray Bursts in the Photospheric and Synchrotron Self-Compton Scenarios , Phys. Rev. D, 78, 101302, 10.1103/PhysRevD.78.101302

    doi:10.1103/physrevd.78.101302 2008

  71. [75]

    2012, title The Role of Stochastic Acceleration in the Prompt Emission of Gamma-Ray Bursts: Application to Hadronic Injection , Astrophys

    Murase, K., Asano, K., Terasawa, T., & Meszaros, P. 2012, title The Role of Stochastic Acceleration in the Prompt Emission of Gamma-Ray Bursts: Application to Hadronic Injection , Astrophys. J., 746, 164, 10.1088/0004-637X/746/2/164

    work page doi:10.1088/0004-637x/746/2/164 2012

  72. [76]

    Murase, K., & Beacom, J. F. 2010, title Very-High-Energy Gamma-Ray Signal from Nuclear Photodisintegration as a Probe of Extragalactic Sources of Ultrahigh-Energy Nuclei , Phys. Rev. D, 82, 043008, 10.1103/PhysRevD.82.043008

    work page doi:10.1103/physrevd.82.043008 2010

  73. [77]

    2006, title High Energy Neutrino Flashes from Far-Ultraviolet and X-Ray Flares in Gamma-Ray Bursts , , 97, 051101, 10.1103/PhysRevLett.97.051101

    Murase , K., & Nagataki , S. 2006, title High Energy Neutrino Flashes from Far-Ultraviolet and X-Ray Flares in Gamma-Ray Bursts , , 97, 051101, 10.1103/PhysRevLett.97.051101

    doi:10.1103/physrevlett.97.051101 2006

  74. [78]

    Murase , K., Toma , K., Yamazaki , R., & M \'e sz \'a ros , P. 2011, title On the Implications of Late Internal Dissipation for Shallow-decay Afterglow Emission and Associated High-energy Gamma-ray Signals , , 732, 77, 10.1088/0004-637X/732/2/77

    work page doi:10.1088/0004-637x/732/2/77 2011

  75. [79]

    2017, title The Observable Signatures of GRB Cocoons , , 834, 28, 10.3847/1538-4357/834/1/28

    Nakar , E., & Piran , T. 2017, title The Observable Signatures of GRB Cocoons , , 834, 28, 10.3847/1538-4357/834/1/28

    doi:10.3847/1538-4357/834/1/28 2017

  76. [80]

    P., & Bonnell , J

    Norris , J. P., & Bonnell , J. T. 2006, title Short Gamma-Ray Bursts with Extended Emission , , 643, 266, 10.1086/502796

    doi:10.1086/502796 2006

  77. [81]

    A., Kouveliotou , C., Grupe , D., et al

    Nousek , J. A., Kouveliotou , C., Grupe , D., et al. 2006, title Evidence for a Canonical Gamma-Ray Burst Afterglow Light Curve in the Swift XRT Data , , 642, 389, 10.1086/500724

    doi:10.1086/500724 2006

  78. [82]

    1986, title Gamma-ray bursters at cosmological distances , , 308, L43, 10.1086/184740

    Paczynski , B. 1986, title Gamma-ray bursters at cosmological distances , , 308, L43, 10.1086/184740

    doi:10.1086/184740 1986

  79. [83]

    2014, title Photosphere Emission in the X-Ray Flares of Swift Gamma-Ray Bursts and Implications for the Fireball Properties , , 795, 155, 10.1088/0004-637X/795/2/155

    Peng , F.-K., Liang , E.-W., Wang , X.-Y., et al. 2014, title Photosphere Emission in the X-Ray Flares of Swift Gamma-Ray Bursts and Implications for the Fireball Properties , , 795, 155, 10.1088/0004-637X/795/2/155

    doi:10.1088/0004-637x/795/2/155 2014

  80. [84]

    J., & Zhang , B

    Perna , R., Armitage , P. J., & Zhang , B. 2006, title Flares in Long and Short Gamma-Ray Bursts: A Common Origin in a Hyperaccreting Accretion Disk , , 636, L29, 10.1086/499775

    doi:10.1086/499775 2006

Showing first 80 references.