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arxiv: 2605.31089 · v1 · pith:MXMEZNP3new · submitted 2026-05-29 · 🌌 astro-ph.HE

Extreme Transients in Gamma Rays

Daniela Hadasch , Dmitriy Khangulyan This is my paper

Pith reviewed 2026-06-28 21:45 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords gamma-ray transientsextreme variabilityparticle accelerationgamma-ray burstsmagnetic reconnectionnovaejetsCrab Nebula
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The pith

Extreme gamma-ray transients are powered by rapid energy release through shocks and magnetic reconnection and probe fundamental limits on particle acceleration.

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

This review paper defines extreme gamma-ray transients as events detected above 100 MeV that either involve catastrophic transformations of systems like stellar explosions or mergers or show particle acceleration in extreme regimes. It establishes that these transients feature rapid large-amplitude variability and physical conditions near limits on acceleration, cooling, and compactness. The central mechanisms are the rapid release of gravitational, magnetic, nuclear or kinetic energy, with shocks and magnetic reconnection producing ultra-relativistic particles and non-thermal radiation. A sympathetic reader cares because the events supply concrete diagnostics, such as variability timescales and spectral evolution, that constrain the size, magnetization and Lorentz factor of the emitting regions. The paper reviews classes including gamma-ray bursts, novae, variable jets and Crab Nebula flares along with the roles of space and ground-based instruments.

Core claim

The paper claims that extreme transients such as gamma-ray bursts, novae, rapidly variable emission from jets, and flaring from the Crab Nebula share the property of being powered by rapid energy release, with shocks and magnetic reconnection playing the central role in producing ultra-relativistic particle populations; observational diagnostics including variability timescales, luminosity-timescale correlations, and MeV-TeV spectral evolution constrain the emitting region's properties, and these events together form the landscape of extreme gamma-ray variability.

What carries the argument

The authors' definition of extreme events as those involving catastrophic system transformations or particle acceleration in an extreme regime, with shocks and magnetic reconnection as the central energy-release mechanisms.

If this is right

  • Variability timescales directly limit the size of the emitting region.
  • Luminosity-timescale correlations and spectral evolution across the MeV-TeV range constrain magnetization and Lorentz factor.
  • Complementary observations from space-borne instruments and ground-based Cherenkov and air-shower arrays are required to capture short-lived high-energy outbursts.
  • Each class of flare poses distinct challenges for models of energy release and particle acceleration.

Where Pith is reading between the lines

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

  • The framework may guide target selection for coordinated multi-messenger campaigns that search for neutrinos or gravitational waves from the same events.
  • If the same reconnection physics operates across the listed classes, similar polarization signatures should appear in the brightest flares.
  • Future instruments with improved sensitivity to short timescales could reveal whether additional source types belong in the extreme category.

Load-bearing premise

The categorization of events as extreme rests on the authors' chosen threshold of either catastrophic system transformation or evidence of particle acceleration in an extreme regime.

What would settle it

A well-observed transient showing rapid large-amplitude variability above 100 MeV but with neither catastrophic system change nor clear signatures of extreme-regime acceleration would fall outside the defined classes and challenge the framework.

Figures

Figures reproduced from arXiv: 2605.31089 by Daniela Hadasch, Dmitriy Khangulyan.

Figure 1
Figure 1. Figure 1: A sketch that illustrates the factors contributing to the e [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Left: Comparison of the spectrum from RS Ophiuchi with spectra of other Fermi-LAT-detected novae. Right: Total energy versus the duration of the RS Ophiuchi outburst compared to other novae detected with the Fermi-LAT. Figures taken from [75]. the absence of such extended emission would place important con￾straints on particle escape efficiencies and diffusion properties in nova environments. In this conte… view at source ↗
Figure 3
Figure 3. Figure 3: The enhancement fraction associated with MP-GRPs as a function of [PITH_FULL_IMAGE:figures/full_fig_p022_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Synchrotron (green), IC (purple), and total (black) model spectra of [PITH_FULL_IMAGE:figures/full_fig_p023_4.png] view at source ↗
read the original abstract

Extreme gamma-ray transients represent some of the most energetic and physically constraining phenomena in high-energy astrophysics. They are characterized by rapid, large-amplitude variability and by physical conditions approaching fundamental limits on particle acceleration, cooling, and compactness. In this review, we focus on transients detected above around 100 MeV and define extreme events as either those involving catastrophic transformations of astrophysical systems (such as stellar explosions, compact-object mergers, and tidal-disruption events) or those exhibiting evidence for particle acceleration operating in an extreme regime. These systems are powered by the rapid release of gravitational, magnetic, nuclear, or kinetic energy, with shocks and magnetic reconnection playing a central role in producing ultra-relativistic particle populations and non-thermal radiation. We summarize observational and theoretical diagnostics that constrain the size, magnetization, and Lorentz factor of the emitting region, including variability timescales, luminosity-timescale correlations, and spectral evolution across the MeV-TeV domain. We further review the complementary capabilities of space-borne gamma-ray instruments, ground-based Cherenkov and air-shower observatories in detecting short-lived, high-energy outbursts. Extreme transient classes discussed include gamma-ray bursts, novae, rapidly variable emission from extragalactic and Galactic jets. Also, because of its extreme aspects, we include flaring emission detected from the Crab Nebula. While each type of these flares poses interesting challenges for phenomenology and theory of these sources, together, these events form the landscape of extreme gamma-ray variability.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

1 major / 2 minor

Summary. The manuscript is a review of extreme gamma-ray transients detected above ~100 MeV. It defines extreme events as those involving catastrophic transformations of astrophysical systems (stellar explosions, compact-object mergers, tidal-disruption events) or particle acceleration operating near fundamental limits. The review summarizes diagnostics for emitting-region size, magnetization, and Lorentz factor (variability timescales, luminosity-timescale correlations, MeV-TeV spectral evolution), reviews space- and ground-based instrument capabilities, and discusses source classes including gamma-ray bursts, novae, extragalactic and Galactic jets, and Crab Nebula flares, with shocks and magnetic reconnection identified as central mechanisms.

Significance. If the source selection and cited literature are accurate and reasonably complete, the review provides a coherent synthesis that connects disparate transient phenomena through shared themes of compactness, rapid variability, and extreme particle acceleration. This framing may assist interpretation of data from Fermi-LAT, CTA, and similar facilities. The paper explicitly states its scope and relies on established results rather than new derivations or predictions.

major comments (1)
  1. [Abstract and definition section] Abstract and opening paragraphs on definition: the categorization of events as 'extreme' rests on the authors' chosen threshold (catastrophic system transformation or evidence of particle acceleration in an extreme regime). This threshold directly determines which sources are included; without quantitative bounds (e.g., minimum Lorentz factor, compactness parameter, or variability timescale), the selection risks appearing ad hoc and affects the review's claimed landscape of extreme variability.
minor comments (2)
  1. [Instrument capabilities paragraph] The discussion of instrument capabilities would benefit from explicit mention of energy thresholds and effective areas for the cited observatories to allow readers to assess detection prospects for short-lived events.
  2. [Crab Nebula flares subsection] Ensure that the Crab flare discussion distinguishes between the nebula's steady emission and the flaring component when citing compactness arguments.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their positive assessment and recommendation for minor revision. We address the major comment point by point below.

read point-by-point responses

  1. Referee: [Abstract and definition section] Abstract and opening paragraphs on definition: the categorization of events as 'extreme' rests on the authors' chosen threshold (catastrophic system transformation or evidence of particle acceleration in an extreme regime). This threshold directly determines which sources are included; without quantitative bounds (e.g., minimum Lorentz factor, compactness parameter, or variability timescale), the selection risks appearing ad hoc and affects the review's claimed landscape of extreme variability.

    Authors: We agree that the definition is qualitative and that explicit quantitative examples would reduce any perception of ad hoc selection. The manuscript's scope is intentionally framed around physically motivated categories (catastrophic events or extreme acceleration) rather than fixed numerical cuts, because the relevant thresholds vary across source classes and are quantified via the diagnostics discussed later in the text. To address the concern, we will revise the abstract and definition paragraphs to incorporate illustrative quantitative bounds drawn from the cited literature (e.g., variability timescales implying compactness parameters l ≳ 10^3 for GRBs, or Lorentz factors Γ ≳ 100 for certain blazar flares). This addition will clarify the selection criteria while preserving the review's unifying framework and source list. revision: partial

Circularity Check

0 steps flagged

No significant circularity

full rationale

This is a review paper whose central content is a definitional scoping of 'extreme' transients (events above ~100 MeV involving catastrophic system change or particle acceleration near fundamental limits) followed by a summary of established observational classes drawn from the cited literature. No derivations, equations, predictions, or fitted quantities are introduced; the text contains no load-bearing steps that reduce to self-definition, fitted-input renaming, or self-citation chains. The chosen threshold is presented explicitly as an organizing criterion rather than a derived result, and all physical diagnostics (variability timescales, compactness arguments, roles of shocks/reconnection) are attributed to prior external work. The paper is therefore self-contained against external benchmarks with no internal circularity.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a review paper; no new free parameters, axioms, or invented entities are introduced by the authors.

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Works this paper leans on

162 extracted references · 126 canonical work pages · 61 internal anchors

  1. [1]

    Gehrels, Gamma Ray Transients, in: M

    N. Gehrels, Gamma Ray Transients, in: M. Matsuoka, N. Kawai (Eds.), All-Sky X-Ray Observations in the Next Decade, 1997, p. 21

    1997

  2. [2]

    Krawczynski, R

    H. Krawczynski, R. Sambruna, A. Kohnle et al., Simultaneous X-Ray and TeV Gamma-Ray Observation of the TeV Blazar 24 Markarian 421 during 2000 February and May, ApJ559 (1) (2001) 187–195. arXiv:astro-ph/0105331, doi:10.1086/ 322364

    Pith/arXiv arXiv 2000

  3. [3]

    Very High Energy Gamma-ray Radiation from the Stellar-mass Black Hole Cygnus X-1

    J. Albert, E. Aliu, H. Anderhub et al., Very High Energy Gamma- Ray Radiation from the Stellar Mass Black Hole Binary Cygnus X-1, ApJ665 (1) (2007) L51–L54. arXiv:0706.1505, doi: 10.1086/521145

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/521145 2007

  4. [4]

    Fermi LAT Collaboration, A. A. Abdo, M. Ackermann et al., Modulated High-Energy Gamma-Ray Emission from the Mi- croquasar Cygnus X-3, Science 326 (5959) (2009) 1512. doi: 10.1126/science.1182174

    work page doi:10.1126/science.1182174 2009

  5. [5]

    Sabatini, M

    S. Sabatini, M. Tavani, E. Striani et al., Episodic Transient Gamma-ray Emission from the Microquasar Cygnus X-1, ApJ712 (1) (2010) L10–L15. arXiv:1002.4967, doi:10. 1088/2041-8205/712/1/L10

    Pith/arXiv arXiv 2010

  6. [8]

    A. A. Vigliano, F. Longo, Gamma-ray Bursts: 50 Years and Counting!, Universe 10 (2) (2024) 57. doi:10.3390/ universe10020057

    2024

  7. [9]

    The NuSTAR view on Hard-TeV BL Lacs

    L. Costamante, G. Bonnoli, F. Tavecchio, G. Ghisellini, G. Tagli- aferri, D. Khangulyan, The NuSTAR view on hard-TeV BL Lacs, MNRAS477 (3) (2018) 4257–4268. arXiv:1711.06282, doi:10.1093/mnras/sty857

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty857 2018

  8. [10]

    F. A. Aharonian, M. V . Barkov, D. Khangulyan, Scenarios for Ultrafast Gamma-Ray Variability in AGN, ApJ841 (1) (2017) 61. arXiv:1704.08148,doi:10.3847/1538-4357/aa7049

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa7049 2017

  9. [11]

    Willingale, P

    R. Willingale, P. Mészáros, Gamma-Ray Bursts and Fast Tran- sients. Multi-wavelength Observations and Multi-messenger Sig- nals, Space Sci. Rev.207 (1-4) (2017) 63–86. doi:10.1007/ s11214-017-0366-4

    2017

  10. [12]

    , keywords =

    L. Chomiuk, B. D. Metzger, K. J. Shen, New Insights into Classical Novae, ARA&A59 (2021) 391–444. arXiv:2011. 08751,doi:10.1146/annurev-astro-112420-114502

    work page doi:10.1146/annurev-astro-112420-114502 2021

  11. [13]

    Carosi, A

    A. Carosi, A. López-Oramas, A Very-High-Energy Gamma- Ray View of the Transient Sky, Universe 10 (4) (2024) 163. arXiv:2404.17480,doi:10.3390/universe10040163

    work page doi:10.3390/universe10040163 2024

  12. [14]

    S. E. Woosley, Gamma-Ray Bursts from Stellar Mass Accretion Disks around Black Holes, ApJ405 (1993) 273. doi:10.1086/ 172359

    1993

  13. [15]

    , keywords =

    D. Eichler, M. Livio, T. Piran, D. N. Schramm, Nucleosynthesis, neutrino bursts and γ-rays from coalescing neutron stars, Na- ture340 (6229) (1989) 126–128.doi:10.1038/340126a0

    work page doi:10.1038/340126a0 1989

  14. [16]

    J. G. Hills, Possible power source of Seyfert galaxies and QSOs, Nature254 (5498) (1975) 295–298.doi:10.1038/254295a0

    work page doi:10.1038/254295a0 1975

  15. [17]

    M. J. Rees, Tidal disruption of stars by black holes of 106-108 solar masses in nearby galaxies, Nature333 (6173) (1988) 523– 528.doi:10.1038/333523a0

    work page doi:10.1038/333523a0 1988

  16. [18]

    Starrfield, J

    S. Starrfield, J. W. Truran, W. M. Sparks, G. S. Kutter, CNO Abundances and Hydrodynamic Models of the Nova Outburst, ApJ176 (1972) 169.doi:10.1086/151619

    work page doi:10.1086/151619 1972

  17. [19]

    Thompson, R

    C. Thompson, R. C. Duncan, The soft gamma repeaters as very strongly magnetized neutron stars - I. Radiative mechanism for outbursts, MNRAS275 (2) (1995) 255–300. doi:10.1093/ mnras/275.2.255

    1995

  18. [20]

    T. W. Speiser, Particle Trajectories in Model Current Sheets, 1, Analytical Solutions, J. Geophys. Res.70 (17) (1965) 4219–4226. doi:10.1029/JZ070i017p04219

    work page doi:10.1029/jz070i017p04219 1965

  19. [21]

    A. R. Bell, The acceleration of cosmic rays in shock fronts - I., MNRAS182 (1978) 147–156. doi:10.1093/mnras/182.2. 147

    work page doi:10.1093/mnras/182.2 1978

  20. [22]

    A. M. Hillas, The Origin of Ultra-High-Energy Cosmic Rays, ARA&A22 (1984) 425–444. doi:10.1146/annurev.aa.22. 090184.002233

    work page doi:10.1146/annurev.aa.22 1984

  21. [23]

    L. O. Drury, REVIEW ARTICLE: An introduction to the theory of diffusive shock acceleration of energetic particles in tenuous plasmas, Reports on Progress in Physics 46 (8) (1983) 973–1027. doi:10.1088/0034-4885/46/8/002

    work page doi:10.1088/0034-4885/46/8/002 1983

  22. [24]

    F. A. Aharonian, S. R. Kelner, A. Y . Prosekin, Angular, spectral, and time distributions of highest energy protons and associated secondary gamma rays and neutrinos propagating through ex- tragalactic magnetic and radiation fields, Phys. Rev. D82 (4) (2010) 043002. arXiv:1006.1045, doi:10.1103/PhysRevD. 82.043002

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd 2010

  23. [25]

    J. L. Elliot, S. L. Shapiro, On the Variability of the Compact Non- thermal Sources, ApJ192 (1974) L3.doi:10.1086/181575

    work page doi:10.1086/181575 1974

  24. [27]

    P. W. Guilbert, A. C. Fabian, M. J. Rees, Spectral and variability constraints on compact sources, MNRAS205 (1983) 593–603. doi:10.1093/mnras/205.3.593

    work page doi:10.1093/mnras/205.3.593 1983

  25. [28]

    An Exceptional VHE Gamma-Ray Flare of PKS 2155-304

    F. Aharonian, A. G. Akhperjanian, A. R. Bazer-Bachi et al., An Exceptional Very High Energy Gamma-Ray Flare of PKS 2155-304, ApJ664 (2) (2007) L71–L74. arXiv:0706.0797, doi:10.1086/520635

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/520635 2007

  26. [29]

    Rapid and multi-band variability of the TeV-bright active nucleus of the galaxy IC 310

    J. Aleksi ´c, L. A. Antonelli, P. Antoranz et al., Rapid and multiband variability of the TeV bright active nucleus of the galaxy IC 310, A&A563 (2014) A91. arXiv:1305.5147, doi:10.1051/0004-6361/201321938

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201321938 2014

  27. [30]

    The spectrum of isotropic diffuse gamma-ray emission between 100 MeV and 820 GeV

    M. Ackermann, M. Ajello, A. Albert et al., The Spectrum of Isotropic Diffuse Gamma-Ray Emission between 100 MeV and 820 GeV, ApJ799 (1) (2015) 86. arXiv:1410.3696, doi: 10.1088/0004-637X/799/1/86. 25

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/799/1/86 2015

  28. [31]

    Aharonian, Next generation of IACT arrays: sci- entific objectives versus energy domains, arXiv e-prints (2005) astro–ph/0511139arXiv:astro-ph/0511139, doi:10

    F. Aharonian, Next generation of IACT arrays: sci- entific objectives versus energy domains, arXiv e-prints (2005) astro–ph/0511139arXiv:astro-ph/0511139, doi:10. 48550/arXiv.astro-ph/0511139

    arXiv 2005

  29. [32]

    den Herder, J. W. et al., [COMPTEL: Instrument description and performance], Tech. Rep. NTRS 19920012642, NASA, nASA Technical Reports Server (1992). URLhttps://ntrs.nasa.gov/citations/19920012642

    arXiv 1992

  30. [33]

    D. J. Thompson, C. A. Wilson-Hodge, Fermi Gamma-Ray Space Telescope, in: C. Bambi, A. Sangangelo (Eds.), Handbook of X-ray and Gamma-ray Astrophysics, Springer, 2022, p. 29. doi: 10.1007/978-981-16-4544-0_58-1

    work page doi:10.1007/978-981-16-4544-0_58-1 2022

  31. [34]

    Tavani, G

    M. Tavani, G. Barbiellini, A. Argan et al., The AGILE Mission, A&A502 (3) (2009) 995–1013. arXiv:0807.4254, doi:10. 1051/0004-6361/200810527

    arXiv 2009

  32. [35]

    Aleksi ´c, S

    J. Aleksi ´c, S. Ansoldi, L. A. Antonelli et al., The major upgrade of the MAGIC telescopes, Part II: A performance study using observations of the Crab Nebula, Astroparticle Physics 72 (2016) 76–94. arXiv:1409.5594, doi:10.1016/ j.astropartphys.2015.02.005

    Pith/arXiv arXiv 2016

  33. [36]

    Aharonian, A

    F. Aharonian, A. G. Akhperjanian, A. R. Bazer-Bachi et al., Observations of the Crab nebula with HESS, A&A457 (3) (2006) 899–915. arXiv:astro-ph/0607333, doi:10.1051/ 0004-6361:20065351

    Pith/arXiv arXiv 2006

  34. [37]

    van Eldik, M

    C. van Eldik, M. Holler, D. Berge, D. Zaborov, J.-P. Lenain, V . Marandon, T. Murach, H. Prokoph, M. de Naurois, R. D. Parsons, Observations of the Crab Nebula with H.E.S.S. phase II , PoS ICRC2015 (2016) 847.doi:10.22323/1.236.0847

    work page doi:10.22323/1.236.0847 2016

  35. [38]

    Park, Performance of the VERITAS experiment , PoS ICRC2015 (2016) 771.doi:10.22323/1.236.0771

    N. Park, Performance of the VERITAS experiment , PoS ICRC2015 (2016) 771.doi:10.22323/1.236.0771

    work page doi:10.22323/1.236.0771 2016

  36. [39]

    , keywords =

    A. Albert, R. Alfaro, C. Alvarez et al., Performance of the HAWC Observatory and TeV Gamma-Ray Measurements of the Crab Nebula with Improved Extensive Air Shower Reconstruc- tion Algorithms, ApJ972 (2) (2024) 144. arXiv:2405.06050, doi:10.3847/1538-4357/ad5f2d

    work page doi:10.3847/1538-4357/ad5f2d 2024

  37. [40]

    A. U. Abeysekara, A. Albert, R. Alfaro et al., The High-Altitude Water Cherenkov (HAWC) observatory in México: The primary detector, Nuclear Instruments and Methods in Physics Research A 1052 (2023) 168253. arXiv:2304.00730, doi:10.1016/ j.nima.2023.168253

    arXiv 2023

  38. [41]

    Ma, Y .-J

    X.-H. Ma, Y .-J. Bi, Z. Cao, M.-J. Chen, S.-Z. Chen, Y .-D. Cheng, G.-H. Gong, M.-H. Gu, H.-H. He, C. Hou, W.-H. Huang, X.-T. Huang, C. Liu, O. Shchegolev, X.-D. Sheng, Y . Stenkin, C.- Y . Wu, H.-R. Wu, S. Wu, G. Xiao, Z.-G. Yao, S.-S. Zhang, Y . Zhang, X. Zuo, Chapter 1 LHAASO Instruments and Detector technology, Chinese Physics C 46 (3) (2022) 030001. ...

    work page doi:10.1088/1674-1137/ac3fa6 2022

  39. [42]

    C. A. Meegan, G. J. Fishman, R. B. Wilson, W. S. Paciesas, G. N. Pendleton, J. M. Horack, M. N. Brock, C. Kouveliotou, Spatial distribution of γ-ray bursts observed by BATSE, Na- ture355 (6356) (1992) 143–145.doi:10.1038/355143a0

    work page doi:10.1038/355143a0 1992

  40. [43]

    , keywords =

    C. Kouveliotou, C. A. Meegan, G. J. Fishman, N. P. Bhat, M. S. Briggs, T. M. Koshut, W. S. Paciesas, G. N. Pendleton, Identi- fication of Two Classes of Gamma-Ray Bursts, ApJ413 (1993) L101.doi:10.1086/186969

    work page doi:10.1086/186969 1993

  41. [44]

    K. S. Kawabata, J. Deng, L. Wang et al., On the Spectrum and Spectropolarimetry of Type Ic Hypernova SN 2003dh/GRB 030329, ApJ593 (1) (2003) L19–L22. arXiv:astro-ph/ 0306155,doi:10.1086/378148

    work page doi:10.1086/378148 2003

  42. [45]

    K. Z. Stanek, T. Matheson, P. M. Garnavich, P. Martini, P. Berlind, N. Caldwell, P. Challis, W. R. Brown, R. Schild, K. Krisciunas, M. L. Calkins, J. C. Lee, N. Hathi, R. A. Jansen, R. Windhorst, L. Echevarria, D. J. Eisenstein, B. Pindor, E. W. Olszewski, P. Harding, S. T. Holland, D. Bersier, Spectro- scopic Discovery of the Supernova 2003dh Associated ...

    work page doi:10.1086/376976 2003

  43. [46]

    B. P. Abbott, R. Abbott, T. D. Abbott et al., GW170817: Observa- tion of Gravitational Waves from a Binary Neutron Star Inspiral, Phys. Rev. Lett.119 (16) (2017) 161101. arXiv:1710.05832, doi:10.1103/PhysRevLett.119.161101

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.119.161101 2017

  44. [47]

    A Photometric Redshift of z ~ 9.4 for GRB 090429B

    A. Cucchiara, A. J. Levan, D. B. Fox et al., A Photometric Redshift of z ~9.4 for GRB 090429B, ApJ736 (1) (2011) 7. arXiv:1105.4915,doi:10.1088/0004-637X/736/1/7

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/736/1/7 2011

  45. [48]

    Khangulyan, F

    D. Khangulyan, F. Aharonian, A. M. Taylor, Naked Forward Shock Seen in the TeV Afterglow Data of GRB 221009A, ApJ966 (1) (2024) 31. arXiv:2309.00673, doi:10.3847/ 1538-4357/ad3550

    arXiv 2024

  46. [49]

    E. V . Derishev, V . V . Kocharovsky, V . V . Kocharovsky, TeV pho- tons from gamma-ray bursts, Advances in Space Research 27 (4) (2001) 813–818.doi:10.1016/S0273-1177(01)00126-0

    work page doi:10.1016/s0273-1177(01)00126-0 2001

  47. [50]

    von Kienlin, C

    A. von Kienlin, C. A. Meegan, W. S. Paciesas, P. N. Bhat, E. Bissaldi, M. S. Briggs, E. Burns, W. H. Cleveland, M. H. Gibby, M. M. Giles, A. Goldstein, R. Hamburg, C. M. Hui, D. Kocevski, B. Mailyan, C. Malacaria, S. Poolakkil, R. D. Preece, O. J. Roberts, P. Veres, C. A. Wilson-Hodge, The Fourth Fermi-GBM Gamma-Ray Burst Catalog: A Decade of Data, ApJ893...

    work page doi:10.3847/1538-4357/ab7a18 2020

  48. [51]

    Ajello, M

    M. Ajello, M. Arimoto, M. Axelsson et al., A Decade of Gamma- Ray Bursts Observed by Fermi-LAT: The Second GRB Catalog, ApJ878 (1) (2019) 52. arXiv:1906.11403, doi:10.3847/ 1538-4357/ab1d4e

    Pith/arXiv arXiv 2019

  49. [52]

    Foffano, M

    L. Foffano, M. Tavani, TeV Afterglows of Gamma-Ray Bursts: Theoretical Analysis and Prospects for Future Observations, arXiv e-prints (2025) arXiv:2508.04557 arXiv:2508.04557, doi:10.48550/arXiv.2508.04557

    work page doi:10.48550/arxiv.2508.04557 2025

  50. [53]

    MAGIC Collaboration, V . A. Acciari, S. Ansoldi et al., Tera- electronvolt emission from the γ-ray burst GRB 190114C, Na- ture575 (7783) (2019) 455–458. arXiv:2006.07249, doi: 10.1038/s41586-019-1750-x

    work page doi:10.1038/s41586-019-1750-x 2019

  51. [54]

    Ajello, M

    M. Ajello, M. Arimoto, M. Axelsson et al., Fermi and Swift Observations of GRB 190114C: Tracing the Evolution of High- energy Emission from Prompt to Afterglow, ApJ890 (1) (2020) 9.arXiv:1909.10605,doi:10.3847/1538-4357/ab5b05

    work page doi:10.3847/1538-4357/ab5b05 2020

  52. [55]

    MAGIC Collaboration, V . A. Acciari, S. Ansoldi et al., Ob- servation of inverse Compton emission from a long γ-ray burst, Nature575 (7783) (2019) 459–463. arXiv:2006.07251, doi:10.1038/s41586-019-1754-6. 26

    work page doi:10.1038/s41586-019-1754-6 2019

  53. [57]

    H. E. S. S. Collaboration, H. Abdalla, F. Aharonian et al., Reveal- ing x-ray and gamma ray temporal and spectral similarities in the GRB 190829A afterglow, Science 372 (6546) (2021) 1081–1085. arXiv:2106.02510,doi:10.1126/science.abe8560

    work page doi:10.1126/science.abe8560 2021

  54. [58]

    Chand, P

    V . Chand, P. S. Pal, A. Banerjee, V . Sharma, P. H. T. Tam, X. He, MAGICal GRB 190114C: Implications of Cutoffin the Spectrum at sub-GeV Energies, ApJ903 (1) (2020) 9. arXiv: 1905.11844,doi:10.3847/1538-4357/abb5fc

    work page doi:10.3847/1538-4357/abb5fc 2020

  55. [59]

    , keywords =

    H. Abdalla, R. Adam, F. Aharonian et al., A very-high- energy component deep in the γ-ray burst afterglow, Na- ture575 (7783) (2019) 464–467. arXiv:1911.08961, doi: 10.1038/s41586-019-1743-9

    work page doi:10.1038/s41586-019-1743-9 2019

  56. [61]

    S., et al

    S. Lesage, P. Veres, M. S. Briggs et al., Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow, ApJ952 (2) (2023) L42. arXiv:2303.14172, doi:10.3847/2041-8213/ace5b4

    work page doi:10.3847/2041-8213/ace5b4 2023

  57. [62]

    LHAASO Collaboration, Z. Cao, F. Aharonian et al., A tera- electron volt afterglow from a narrow jet in an extremely bright gamma-ray burst., Science 380 (6652) (2023) 1390–1396. arXiv:2306.06372,doi:10.1126/science.adg9328

    work page doi:10.1126/science.adg9328 2023

  58. [64]

    Gravitational Waves and Gamma- Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A

    F. Aharonian, F. Ait Benkhali, J. Aschersleben et al., H.E.S.S. Follow-up Observations of GRB 221009A, ApJ946 (1) (2023) L27. arXiv:2303.10558, doi:10.3847/2041-8213/ acc405

    work page doi:10.3847/2041-8213/ 2023

  59. [65]

    K. Abe, S. Abe, A. Abhishek et al., GRB 221009A: Observations with LST-1 of CTAO and Implications for Structured Jets in Long Gamma-Ray Bursts, ApJ988 (2) (2025) L42. arXiv: 2507.03077,doi:10.3847/2041-8213/ade4cf

    work page doi:10.3847/2041-8213/ade4cf 2025

  60. [66]

    Axelsson, M

    M. Axelsson, M. Ajello, M. Arimoto et al., GRB 221009A: The B.O.A.T. Burst that Shines in Gamma Rays, ApJS277 (1) (2025) 24. arXiv:2409.04580, doi:10.3847/1538-4365/ ada272

    work page doi:10.3847/1538-4365/ 2025

  61. [67]

    Evidence for nonlinear diffusive shock acceleration of cosmic-rays in the 2006 outburst of the recurrent nova RS Ophiuchi

    V . Tatischeff, M. Hernanz, Evidence for Nonlinear Diffusive Shock Acceleration of Cosmic Rays in the 2006 Outburst of the Recurrent Nova RS Ophiuchi, ApJ663 (2) (2007) L101–L104. arXiv:0705.4422,doi:10.1086/520049

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/520049 2006

  62. [68]

    A. A. Abdo, M. Ackermann, M. Ajello et al., Gamma-Ray Emis- sion Concurrent with the Nova in the Symbiotic Binary V407 Cygni, Science 329 (5993) (2010) 817–821.arXiv:1008.3912, doi:10.1126/science.1192537

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.1192537 2010

  63. [69]

    E. Aliu, S. Archambault, T. Arlen et al., VERITAS Observations of the Nova in V407 Cygni, ApJ754 (1) (2012) 77. arXiv: 1205.5287,doi:10.1088/0004-637X/754/1/77

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/754/1/77 2012

  64. [70]

    Search for Gamma-ray Emission from Galactic Novae with the Fermi-LAT

    A. Franckowiak, P. Jean, M. Wood, C. C. Cheung, S. Buson, Search for gamma-ray emission from Galactic novae with the Fermi -LAT, A&A609 (2018) A120.arXiv:1710.04736, doi: 10.1051/0004-6361/201731516

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201731516 2018

  65. [71]

    B. E. Schaefer, Comprehensive catalogue of the overall best dis- tances and properties of 402 galactic novae, MNRAS517 (4) (2022) 6150–6169. arXiv:2210.03181, doi:10.1093/ mnras/stac2900

    arXiv 2022

  66. [72]

    M. L. Ahnen, S. Ansoldi, L. A. Antonelli et al., Very high- energy γ-ray observations of novae and dwarf novae with the MAGIC telescopes, A&A582 (2015) A67.arXiv:1508.04902, doi:10.1051/0004-6361/201526478

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201526478 2015

  67. [73]

    C. C. Cheung, T. J. Johnson, P. Jean, M. Kerr, K. L. Page, J. P. Osborne, A. P. Beardmore, K. V . Sokolovsky, F. Teyssier, S. Ciprini, G. Martí-Devesa, I. Mereu, S. Razzaque, K. S. Wood, S. N. Shore, S. Korotkiy, A. Levina, A. Blumenzweig, Fermi LAT Gamma-ray Detection of the Recurrent Nova RS Ophiuchi during its 2021 Outburst, ApJ935 (1) (2022) 44. arXiv...

    work page doi:10.3847/1538-4357/ac7eb7 2021

  68. [74]

    H. E. S. S. Collaboration, F. Aharonian, F. Ait Benkhali et al., Time-resolved hadronic particle acceleration in the recurrent nova RS Ophiuchi, Science 376 (6588) (2022) 77–80. arXiv: 2202.08201,doi:10.1126/science.abn0567

    work page doi:10.1126/science.abn0567 2022

  69. [75]

    V . A. Acciari, S. Ansoldi, L. A. Antonelli et al., Proton accelera- tion in thermonuclear nova explosions revealed by gamma rays, Nature Astronomy 6 (2022) 689–697. arXiv:2202.07681, doi:10.1038/s41550-022-01640-z

    work page doi:10.1038/s41550-022-01640-z 2022

  70. [76]

    K. Abe, S. Abe, A. Abhishek et al., Detection of RS Oph with LST-1 and modelling of its HE/VHE gamma-ray emission, A&A695 (2025) A152. arXiv:2503.13283, doi:10.1051/ 0004-6361/202452447

    arXiv 2025

  71. [77]

    Hernanz, V

    M. Hernanz, V . Tatischeff, High Energy Emission of Symbi- otic Recurrent Novae: RS Oph and V407 Cyg, Baltic Astron- omy 21 (2012) 62–67. arXiv:1111.4129, doi:10.1515/ astro-2017-0359

    Pith/arXiv arXiv 2012

  72. [78]

    Rodrigues, Neutrinos from extreme astrophysical sources, New A Rev.102 (2026) 101747

    X. Rodrigues, Neutrinos from extreme astrophysical sources, New A Rev.102 (2026) 101747. arXiv:2603.10167, doi: 10.1016/j.newar.2026.101747

    work page doi:10.1016/j.newar.2026.101747 2026

  73. [79]

    Bednarek, J

    W. Bednarek, J. Sitarek, Gamma rays from nebulae around re- current novae, Journal of High Energy Astrophysics 38 (2023) 22–31. arXiv:2303.15741, doi:10.1016/j.jheap.2023. 03.004

    work page doi:10.1016/j.jheap.2023 2023

  74. [80]

    B. E. Schaefer, The recurrent nova T CrB had prior eruptions observed near December 1787 and October 1217 AD, Journal for the History of Astronomy 54 (4) (2023) 436–455. arXiv: 2308.13668,doi:10.1177/00218286231200492

    work page doi:10.1177/00218286231200492 2023

  75. [81]

    Schneider, When will the Next T CrB Eruption Occur?, Re- search Notes of the American Astronomical Society 8 (10) (2024) 272.doi:10.3847/2515-5172/ad8bba

    J. Schneider, When will the Next T CrB Eruption Occur?, Re- search Notes of the American Astronomical Society 8 (10) (2024) 272.doi:10.3847/2515-5172/ad8bba. 27

    work page doi:10.3847/2515-5172/ad8bba 2024

  76. [82]

    B. E. Schaefer, The B & V light curves for recurrent nova T CrB from 1842-2022, the unique pre- and post-eruption high- states, the complex period changes, and the upcoming eruption in 2025.5 ± 1.3, MNRAS524 (2) (2023) 3146–3165. arXiv: 2303.04933,doi:10.1093/mnras/stad735

    work page doi:10.1093/mnras/stad735 2022

  77. [84]

    I. F. Mirabel, L. F. Rodríguez, A superluminal source in the Galaxy, Nature371 (6492) (1994) 46–48. doi:10.1038/ 371046a0

    1994

  78. [85]

    J. E. McClintock, R. A. Remillard, Black hole binaries, in: W. H. G. Lewin, M. van der Klis (Eds.), Compact stellar X- ray sources, V ol. 39, Cambridge University Press, 2006, Ch. 4, pp. 157–213.doi:10.48550/arXiv.astro-ph/0306213

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0306213 2006

  79. [86]

    R. P. Fender, T. M. Belloni, E. Gallo, Towards a unified model for black hole X-ray binary jets, MNRAS355 (4) (2004) 1105–1118. arXiv:astro-ph/0409360, doi:10.1111/j. 1365-2966.2004.08384.x

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1111/j 2004

  80. [87]

    A universal radio/X-ray correlation in low/hard state black hole binaries

    E. Gallo, R. P. Fender, G. G. Pooley, A universal radio-X-ray correlation in low/hard state black hole binaries, MNRAS344 (1) (2003) 60–72. arXiv:astro-ph/0305231, doi:10.1046/j. 1365-8711.2003.06791.x

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1046/j 2003

Showing first 80 references.