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REVIEW 3 major objections 5 minor 87 references

This paper argues that a super-Eddington AGN with an opaque disk wind can hide all its gamma rays while producing detectable neutrinos from wind-cloud bowshocks.

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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Super-Eddington black-hole winds colliding with broad-line-region clouds could produce detectable neutrino fluxes with weak electromagnetic counterparts.

T0 review reviewed 2026-08-05 challenge →

load-bearing objection Plausible gamma-dark neutrino scenario from sub-photosphere wind-cloud shocks, but the TDE benchmark can't feed the hyper-accreting wind it assumes, and the density bookkeeping errors void the quantitative flux claims as printed. the 3 major comments →

arxiv 2508.18441 v1 pith:CFPYYUEY submitted 2025-08-25 astro-ph.HE

Super-Accreting Active Galactic Nuclei as Neutrino Sources

Gustavo E. Romero , Pablo Sotomayor This is my paper
classification astro-ph.HE
keywords active galactic nucleisuper-Eddington accretionbroad-line regiontidal disruption eventsneutrino emissionwind-cloud interactiongamma-ray absorptionpp collisions
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.

The reading

This paper argues that when an active galactic nucleus briefly accretes far above the Eddington rate, the radiation-driven wind it launches can overtake the dense clouds of its broad-line region. The bowshocks that form around those clouds accelerate protons, and the high-density shocked gas converts their energy into neutrinos through proton-proton collisions. Because the wind photosphere is opaque to gamma rays but transparent to neutrinos, the same collisions produce no detectable high-energy electromagnetic counterpart. The authors propose this as a new class of 'dark' neutrino emitter: a jetless AGN with only weak radio and thermal UV signatures. They show that for a 10^6-solar-mass black hole in a tidal disruption event, the predicted neutrino flux would be within reach of IceCube-Gen2 for nearby galaxies with high broad-line-cloud filling factors.

Core claim

The central claim is that the sub-photosphere wind-cloud interaction in a super-accreting AGN is a viable hadronic neutrino factory. For a dense wind, in the regime modelled as Model 2 with accretion rate 10^5 times critical, the shocked cloud is adiabatic while the shocked wind is radiative; protons accelerated by diffusive shock acceleration reach about 2 TeV, and inelastic pp collisions dominate their cooling. The resulting neutrinos escape, while gamma rays are absorbed in the wind, leaving a source that is bright in neutrinos but dark in high-energy photons. For the less extreme Model 1, with accretion rate 10 times critical, interactions occur above the photosphere and gamma rays parti

What carries the argument

The central mechanism is the wind-cloud bowshock inside the wind photosphere: a supersonic radiation-driven wind overruns a broad-line cloud, creating a forward shock in the wind and a reverse shock in the cloud. The dichotomy of which shock is adiabatic is set by comparing the thermal cooling length to the cloud and bowshock sizes; only in the adiabatic shock are protons efficiently accelerated. The wind photosphere then acts as a gamma-ray blanket: it absorbs and reprocesses the GeV-TeV photons while letting neutrinos pass. The neutrino spectrum is computed from the standard pp pion-decay formalism using the steady-state proton distribution.

Load-bearing premise

The model assumes that a substantial population of dense broad-line clouds (volume filling factor up to about 10^-2) survives inside the wind photosphere during the super-Eddington phase long enough for sustained proton-proton collisions; the paper itself concedes that TDEs may lack persistent broad-line regions.

What would settle it

Observe a nearby (d <~100 Mpc) TDE with prominent broad optical lines during its super-Eddington phase with IceCube-Gen2; if no >TeV neutrino excess appears despite the BLR filling factor in the detectable range (f_BLR ~10^-3 to 10^-2), the model's predicted flux is ruled out. Independently, measuring f_BLR from broad-line variability and finding it below ~10^-3 over the accretion episode would falsify the detectability claim.

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

If this is right

  • Super-Eddington AGNs, including TDE-like events around 10^6-solar-mass black holes, become detectable neutrino sources for BLR filling factors of about 10^-3 to 10^-2 and distances up to about 100 Mpc with IceCube-Gen2.
  • Such sources are orphan neutrino emitters: no gamma-ray counterpart, only thermal UV photospheric emission and radio synchrotron, so neutrino telescopes must search without gamma-ray triggers.
  • For 10^7-solar-mass black holes, detection is possible up to roughly 30 Mpc with high filling factor; current-generation instruments cannot reach these sources.
  • The duration of neutrino emission is set by the super-Eddington or TDE phase and by cloud replenishment, with stochastic flickering on timescales of hours to days in radio and optical emission lines expected as a diagnostic of active wind-cloud interactions.

Where Pith is reading between the lines

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

  • If TDEs do not reliably form a persistent broad-line region, the neutrino rate could be far lower than the optimistic estimates; non-detection by IceCube-Gen2 of nearby gamma-quiet TDEs would then constrain cloud survival rather than disprove the shock mechanism itself.
  • The same wind-cloud shock recipe can be applied to other wind obstacles, such as early-type stars or neutron stars crossing the wind, potentially producing steady neutrino emission in ordinary AGNs rather than only in transients.
  • A focused search for IceCube-Gen2 events coincident in time with optically discovered TDEs that show broad lines would provide a direct test of the model's cloud-filling-factor requirement.
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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 / 5 minor

Summary. The paper proposes that in super-Eddington AGN phases, a dense disk wind can overtake BLR clouds, forming bowshocks in which protons are accelerated by diffusive shock acceleration; inelastic pp collisions then produce neutrinos that escape while gamma rays are absorbed in the opaque wind. The authors consider two regimes: Model 1 (Mdot=10 Mcr) with the wind photosphere inside the BLR and escaping gamma rays, and Model 2 (Mdot=1e5 Mcr) with the photosphere far outside the BLR, yielding 'dark' neutrino sources. They compute nonthermal SEDs, gamma-ray absorption, and neutrino fluxes for MBH=1e6 and 1e7 Msun and compare with IceCube-Gen2 sensitivities as a function of BLR filling factor and distance.

Significance. If validated, the mechanism would identify a genuinely new, jet-free neutrino source class with falsifiable predictions: orphan neutrino emission, radio/X-ray flickering, and a correlation with high BLR filling factors. The use of standard DSA and Kelner pp neutrino formulas, plus an explicit treatment of gamma-ray absorption, are strengths. However, the quantitative predictions are currently undermined by internal inconsistencies in the wind-density normalization, the photosphere radii, and especially the mass budget of the TDE benchmark used for the Model 2 detectability claims.

major comments (3)
  1. [Sec. 2.1, Table 1, Sec. 5 (Figs. 10-13)] The Model 2 benchmark is not realizable as a TDE. For MBH=1e6 Msun, Mcr=4*pi*G*M*mp/(c*sigma_T)=1.4e23 g/s, so Mdot_w=1e5 Mcr=1.4e28 g/s ~ 220 Msun/yr. With vw=670 km/s (Eq. 8) and R_BLR=2.9e14 cm, the wind reaches the BLR only after ~50 days, ejecting ~30 Msun in transit; a canonical TDE fallback of ~0.5 Msun is exhausted in less than a day at this rate. Thus the assumed coexistence of the dense wind and BLR clouds below the photosphere is not satisfied for the TDE benchmark, so the central 'dark source' regime and the IceCube-Gen2 detectability claims in Figs. 10-13 rest on an unsustainable mass supply. A self-consistent accretion history or a different source population must be supplied.
  2. [Eq. (9), Table 3] The normalization of Eq. (9) is inconsistent with the definition of Mcr given in Sec. 1. At the calibration point (Mdot=100 Mcr, vw=0.1c, r=1e-4 pc), continuity gives n_w ~ 9e9 cm^-3, whereas Eq. (9) gives 6.1e8 cm^-3; equivalently, the coefficient implies Mcr ~ 9e21 g/s, a factor ~15 below the stated value. More importantly, Table 3 lists n_w=2.5e13 cm^-3 for the Model 1 shocked wind, but evaluating Eq. (9) at the actual interaction radius rint~0.91 R_BLR=2.6e14 cm gives n_w ~ 4e7 cm^-3 before shock compression. Table 3's value seems to be evaluated near the photosphere rather than at rint, so the cooling timescales and SEDs in Figs. 3-4 use a target density 5-6 orders of magnitude too high. The calculations need to be redone with a consistent density.
  3. [Table 1 vs. Eqs. (9), (11)] The photospheric radii in Table 1 are not consistent with the stated wind parameters. For Model 2, using Mdot_w=1e5 Mcr and vw=670 km/s, the Thomson photosphere estimate H_ph ~ Mdot_w*sigma_T/(Omega_w*mp*vw) is ~2e19 cm, not 4.6e17 cm; for Model 1, H_ph=1.6e11 cm lies inside the wind launch radius r_cr ~ 4 mdot r_g ~ 6e11 cm, which is physically awkward. Since H_ph sets the photospheric radiation field (Eq. 12) used for IC and p-gamma cooling and determines the gamma absorption geometry, the authors should show explicitly how H_ph is obtained from Eq. (11) with their density profile.
minor comments (5)
  1. [Sec. 1] Typo: 'Thompson scattering' should be 'Thomson scattering'.
  2. [Eq. (9) discussion] The statement that Mdot and vw are kept explicit is misleading because Eq. (7) gives vw proportional to Mdot^-1/2; using that relation, n_w scales as Mdot^3/2, not linearly. Please clarify the actual scaling used in the numerical estimates.
  3. [Fig. 7] Axis labels in the left panel are incomplete: the vertical axis should read exp(-tau_gamma_gamma) rather than 'exp( )'.
  4. [Fig. 13 and text] The text says neutrinos from Model 2 are detectable up to ~30 Mpc for MBH=1e7, but the figure axis extends to 1 Gpc and the labeled detectability boundary reaches much larger distances. Please reconcile the caption, axis range, and the 30 Mpc statement.
  5. [Footnote 1 and Sec. 5] The relation to Huang et al. [29] is confined to a footnote; since that work applies a similar outflow-cloud neutrino mechanism to NGC 1068, the overlap and differences should be discussed in the main text.

Circularity Check

0 steps flagged

No significant circularity; the neutrino flux is a forward calculation from adopted parameters and standard pp/DSA formalism.

full rationale

The paper's central calculation (Model 2 neutrino flux) is a forward model. The authors specify input parameters (MBH, Mdot, vw, nc, B, qrel, a, D, fBLR, Nc) and compute shock character via cooling-length comparison, particle acceleration via DSA, and neutrino spectra via Kelner et al.'s standard pp formulas. No output quantity is defined in terms of the detection claim, and no parameter is fitted to neutrino data. The only self-citations are to the authors' earlier paper [16] for cooling/escape timescale formulas and cloud-replenishment behavior; these are not load-bearing for the neutrino result, which is independently computed from published shock and pp physics. The admitted uncertainty about persistent BLRs in TDEs is a physical assumption, not a circular step. The mass-budget/travel-time consistency concern raised by the skeptic is a quantitative plausibility issue, not a definitional reduction, and therefore outside circularity scoring.

Axiom & Free-Parameter Ledger

12 free parameters · 7 axioms · 0 invented entities

No new particles, fields, or forces are postulated. The 'new class of emitter' is an arrangement of known components (wind, clouds, shocks, pp neutrinos), not an invented entity. The central claim rests on many adopted parameters and domain assumptions, especially the existence and survival of BLR clouds during TDEs and the extrapolated magnetic field strengths.

free parameters (12)
  • Relativistic particle injection fraction q_rel = 0.1
    Adopted fraction of shock kinetic power converted to relativistic particles; scales L_rel and all neutrino fluxes directly (Sec. 3).
  • Hadron-to-lepton power ratio a = 100
    Sets L_p = 100 L_e; since neutrinos come from pp, this ratio directly controls the neutrino flux (Sec. 3).
  • Injection spectral index p = 2.0
    Assumed power-law index for particle injection at all shocks (Eq. 31).
  • Diffusion coefficient D = 10^-3 D_Bohm
    Suppresses diffusion and sets maximum particle energies through acceleration-cooling balance (Eq. 30).
  • Magnetic field in shocked wind B_sw = 40 G
    Chosen via magnetic-confinement and sub-equipartition arguments; controls synchrotron cooling and maximum energies (Sec. 2.4).
  • Magnetic field in clouds B_c = 1 G
    Adopted for shocked cloud; controls acceleration and cooling (Sec. 2.4).
  • BLR filling factor f_BLR = 10^-6 (fiducial), 10^-3 to 10^-2 for detectability
    Sets cloud radius via Eq. (5) and total neutrino luminosity; the paper's detectability conclusion depends on high-end values.
  • Number of BLR clouds N_c = 10^8
    Assumed total cloud population; combined with Omega_w gives number of interactions N_c^w = 5e7.
  • Cloud density n_c = 10^12 cm^-3
    Adopted from BLR cloud literature [36]; determines pp target density and shock radiative/adiabatic nature.
  • Wind solid angle Omega_w = pi sr
    Assumed opening angle; sets wind density normalization and number of intercepted clouds.
  • Accretion rates in two models = 10 M_cr and 10^5 M_cr
    Benchmark cases motivated by TDEs/NLS1s and hyperaccretion; Model 2 carries the orphan-neutrino claim.
  • Inner BLR radius factor R_in = 0.8 R_BLR
    Adopted from [59] for average interaction radius calculation (Eq. 21).
axioms (7)
  • domain assumption The BLR size-luminosity relation can be extended to super-Eddington and TDE phases.
    Invoked in Sec. 2.1 to set R_BLR = 9.2e-5 pc for 1e6 M_sun; the paper notes 'some studies suggest cautious extension', and TDE BLR presence is uncertain.
  • domain assumption A population of dense BLR clouds exists and is roughly steady during the super-accreting phase, despite destruction.
    Sec. 2.3 and Sec. 6 assume clouds are continuously replenished; if not, pp targets vanish. Paper admits TDEs may lack persistent BLRs.
  • domain assumption The disk wind is described by the Fukue critical-accretion model with v_w ~ c/sqrt(2 mdot) and a power-law density profile.
    Eqs. (7)-(9); used for wind density, photosphere location, and shock velocities.
  • domain assumption Diffusive shock acceleration operates in the adiabatic shocks with D = 10^-3 D_Bohm.
    Sec. 3, Eq. (30); determines E_max and particle spectra.
  • domain assumption Magnetic field strengths of order 1-40 G in BLR clouds follow from molecular-cloud B-n scaling or magnetic confinement.
    Sec. 2.4 extrapolates B ~ 10 G from n ~ 300 cm^-3 data and imposes confinement; authors acknowledge the extrapolation is uncertain.
  • domain assumption One-zone steady-state particle transport with continuous injection is a valid approximation.
    Sec. 3, Eq. (31); ignores cloud-to-cloud variations and time dependence.
  • standard math Kelner et al. pp cross-section and neutrino spectra are applicable.
    Eq. (34); standard treatment for high-energy pp neutrinos.

reviewed 2026-08-05 · how reviews work

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Cite this review

Pith. "Pith review of Super-Accreting Active Galactic Nuclei as Neutrino Sources." pith.science (2026). https://pith.science/paper/CFPYYUEY

@misc{pith2026250818441,
  author       = {Pith},
  title        = {Pith review of: Super-Accreting Active Galactic Nuclei as Neutrino Sources},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/CFPYYUEY}},
  note         = {Machine review of arXiv:2508.18441}
}
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abstract

Active galactic nuclei (AGNs) often exhibit broad-line regions (BLRs), populated by high-velocity clouds in Keplerian orbits around the central supermassive black hole (SMBH) at subparsec scales. During episodes of intense super-Eddington accretion, the disk can launch a powerful radiation-driven wind that overtakes the BLR clouds, forming bowshocks. Two shocks arise: one into the wind and another into the cloud. If adiabatic, electrons and protons are efficiently accelerated via Fermi processes to relativistic energies. In dense winds, the resulting high-energy photons are absorbed and reprocessed within the photosphere, while neutrinos from inelastic $pp$ collisions escape. We explore the potential of super-accreting AGNs as neutrino sources and propose a new class of emitter: an AGN without jets or gamma-ray counterparts, but with a strong opaque disk wind. As a case study, we consider a SMBH with $M_{\rm BH}=10^6,M_{\odot}$ and accretion rates consistent with tidal disruption events (TDEs). We compute the main cooling processes for relativistic particles and show that super-Eddington SMBHs can produce detectable neutrino fluxes with only weak electromagnetic signatures. Such fluxes may be observable by IceCube-Gen2 in nearby galaxies with a high BLR cloud filling factor. For more massive black holes, detection remains possible with moderate filling factors if the source is close, or at larger distances if the filling factor is high. Our model thus provides a plausible scenario for extragalactic neutrino sources, where both flux and timescale are determined by the number of orbiting clouds and the duration of the super-accreting phase.

Figures

Figures reproduced from arXiv: 2508.18441 by Gustavo E. Romero, Pablo Sotomayor.

Figure 1
Figure 1. Figure 1: (Top): Sketch of the model (not to scale). The AGN undergoes a super-Eddington accretion phase and a powerful radiation-driven wind is launched from the inner disk (labeled super-accreting disk). The outflowing supersonic wind overtakes the BLR clouds at subparsec scales from the central black hole, and bowshocks form around the clouds. (Bottom): Representation of a single wind-cloud interaction. In both s… view at source ↗
Figure 2
Figure 2. Figure 2: Length scales of thermal radiative cooling for the shocks in the wind and in the cloud, along with the characteristic size scales of the shocked regions. The dashed blue and orange lines correspond to the cooling lengths of the shocked wind and shocked cloud, respectively. The horizontal lines mark the bowshock thickness (blue) and the cloud radius (orange), while the vertical lines indicate key spatial lo… view at source ↗
Figure 3
Figure 3. Figure 3: Timescales of acceleration, cooling, and diffusion for relativistic electrons and protons accelerated in the shocked wind for the Model 1. (Left): Timescales for the electrons. (Right): Timescales for the protons. 6 4 2 0 2 4 6 8 10 12 14 log10 (E /eV) 20.0 22.5 25.0 27.5 30.0 32.5 35.0 37.5 lo g 1 0 (L / e r g s 1 ) synchr e synchr p IC bremss pp [PITH_FULL_IMAGE:figures/full_fig_p013_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Different nonthermal contributions to the SED for Model 1. At radio energies, the SED is dominated by synchrotron radiation of electrons and protons. Gamma rays by decay of neutral pions dominate the SED at very-high energies. We assume Nw c = 5 × 107 interactions with identical clouds at r = 0.91 RBLR from the supermassive black hole. 3.2. Model 2 Shocks within the clouds accelerate relativistic particles… view at source ↗
Figure 5
Figure 5. Figure 5: Timescales of acceleration, cooling, and diffusion for relativistic electrons and protons accelerated in the cloud for Model 2. (Left): Timescales for the electrons. (Right): Timescales for the protons. The nonthermal SEDs calculated with this model are presented in [PITH_FULL_IMAGE:figures/full_fig_p014_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: The same as in [PITH_FULL_IMAGE:figures/full_fig_p014_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Gamma-ray attenuation by photon annihilation evaluated on the radial axis from the wind photosphere to the observer for Model 1. Left: Attenuation calculated for a single photon with Eγ = 1 TeV. Right: Color map for photons with energies in the range from 100 MeV to 1 PeV. The dashed green line in each plot indicates the location of the BLR [PITH_FULL_IMAGE:figures/full_fig_p015_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: The same as in [PITH_FULL_IMAGE:figures/full_fig_p016_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: The same as in [PITH_FULL_IMAGE:figures/full_fig_p016_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: shows the calculated neutrino flux for different values of the filling factor of the BLR, in the case of a nearby galaxy at dL = 5 Mpc. We also show the sensitivity curve of IceCube-Gen2 with an average significance of 5σ after 10 years of observations for a source at the celestial equator (δ = 0 deg) [80]. For the parameters adopted in this work, the neutrino flux will only be detected by the next genera… view at source ↗
Figure 11
Figure 11. Figure 11: The same as in [PITH_FULL_IMAGE:figures/full_fig_p018_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: The same as in [PITH_FULL_IMAGE:figures/full_fig_p018_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Neutrino flux at Eν = 10 TeV relative to the threshold value for IceCube-Gen2. We consider MBH = 107 M⊙, m˙ = 105 , and fBLR and dL are in the range (fBLR × dL) = [10−5 , 10−2 ] × [5 Mpc, 1 Gpc]. The thick black line indicates the limit of detectability. In this context, our model offers a physically motivated framework for describing wind–cloud interactions and their associated nonthermal emission, inclu… view at source ↗

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Reference graph

Works this paper leans on

87 extracted references · 26 canonical work pages

  1. [1]

    Thick Accretion Disks and Supercritical Luminosities

    Paczy ´ nsky, B.; Wiita, P .J. Thick Accretion Disks and Supercritical Luminosities. Astron. Astrophys. 1980, 88, 23

    1980

  2. [2]

    Slim Accretion Disks

    Abramowicz, M.A.; Czerny, B.; Lasota, J.P .; Szuszkiewicz, E. Slim Accretion Disks. Astrophys. J. 1988, 332, 646

    1988

  3. [3]

    Thick supercritical accretion disks and active galactic nuclei

    Wiita, P .J. Thick supercritical accretion disks and active galactic nuclei. Comments Astrophys. 1982, 9, 251–260

    1982

  4. [4]

    Supercritical Accretion Flows around Black Holes: Two-dimensional, Radiation Pressure-dominated Disks with Photon Trapping

    Ohsuga, K.; Mori, M.; Nakamoto, T.; Mineshige, S. Supercritical Accretion Flows around Black Holes: Two-dimensional, Radiation Pressure-dominated Disks with Photon Trapping. Astrophys. J. 2005, 628, 368–381. https://doi.org/10.1086/430728

    doi:10.1086/430728 2005

  5. [5]

    Critical Accretion Disk

    Fukue, J. Critical Accretion Disk. Publ. Astron. Soc. Jpn. 2004, 56, 569–580. https://doi.org/10.1093/pasj/56.3.569

    doi:10.1093/pasj/56.3.569 2004

  6. [6]

    Why Is Supercritical Disk Accretion Feasible? Astrophys

    Ohsuga, K.; Mineshige, S. Why Is Supercritical Disk Accretion Feasible? Astrophys. J. 2007, 670, 1283–1290. https://doi.org/10.1 086/522324

    2007

  7. [7]

    Super-Eddington Accretion Disks around Supermassive Black Holes

    Jiang, Y.F.; Stone, J.M.; Davis, S.W. Super-Eddington Accretion Disks around Supermassive Black Holes. Astrophys. J. 2019, 880, 67. https://doi.org/10.3847/1538-4357/ab29ff

    doi:10.3847/1538-4357/ab29ff 2019

  8. [8]

    General Relativistic Radiation Magnetohydrodynamics Simulations of Black Hole Accretion Disks: Comparison of Methods Based on Variable Eddington Tensor and Based on M1 Closure

    Asahina, Y.; Ohsuga, K. General Relativistic Radiation Magnetohydrodynamics Simulations of Black Hole Accretion Disks: Comparison of Methods Based on Variable Eddington Tensor and Based on M1 Closure. Astrophys. J. 2022, 929, 93. https: //doi.org/10.3847/1538-4357/ac5d37

    doi:10.3847/1538-4357/ac5d37 2022

  9. [9]

    Global Structure of Three Distinct Accretion Flows and Outflows around Black Holes from Two- dimensional Radiation-magnetohydrodynamic Simulations

    Ohsuga, K.; Mineshige, S. Global Structure of Three Distinct Accretion Flows and Outflows around Black Holes from Two- dimensional Radiation-magnetohydrodynamic Simulations. Astrophys. J. 2011, 736, 2. https://doi.org/10.1088/0004-637X/736/ 1/2

    work page doi:10.1088/0004-637x/736/ 2011

  10. [10]

    Three-dimensional general relativistic radiation magnetohydrody- namical simulation of super-Eddington accretion, using a new code HARMRAD with M1 closure

    McKinney, J.C.; Tchekhovskoy, A.; Sadowski, A.; Narayan, R. Three-dimensional general relativistic radiation magnetohydrody- namical simulation of super-Eddington accretion, using a new code HARMRAD with M1 closure. Mon. Not. R. Astron. Soc. 2014, 441, 3177–3208. https://doi.org/10.1093/mnras/stu762

    doi:10.1093/mnras/stu762 2014

  11. [11]

    Numerical simulations of super-critical black hole accretion flows in general relativity

    S ˛ adowski, A.; Narayan, R.; McKinney, J.C.; Tchekhovskoy, A. Numerical simulations of super-critical black hole accretion flows in general relativity. Mon. Not. R. Astron. Soc. 2014, 439, 503–520. https://doi.org/10.1093/mnras/stt2479

    doi:10.1093/mnras/stt2479 2014

  12. [12]

    Evidence for Optically Thick, Eddington-limited Winds Driven by Supercritical Accretion

    Zhou, Y.; Feng, H.; Ho, L.C.; Yao, Y. Evidence for Optically Thick, Eddington-limited Winds Driven by Supercritical Accretion. Astrophys. J. 2019, 871, 115. https://doi.org/10.3847/1538-4357/aaf724

    doi:10.3847/1538-4357/aaf724 2019

  13. [14]

    Super-Eddington accretion in the Q2237+0305 quasar? Astron

    Berdina, L.A.; Tsvetkova, V .S.; Shulga, V .M. Super-Eddington accretion in the Q2237+0305 quasar? Astron. Astrophys. 2021, 645, A78. https://doi.org/10.1051/0004-6361/202039379

    work page doi:10.1051/0004-6361/202039379 2021

  14. [15]

    The origin of radio emission from radio-quiet active galactic nuclei

    Panessa, F.; Baldi, R.D.; Laor, A.; Padovani, P .; Behar, E.; McHardy, I. The origin of radio emission from radio-quiet active galactic nuclei. Nat. Astron. 2019, 3, 387–396. https://doi.org/10.1038/s41550-019-0765-4

    doi:10.1038/s41550-019-0765-4 2019

  15. [16]

    Nonthermal radiation from the central region of super-accreting active galactic nuclei

    Sotomayor, P .; Romero, G.E. Nonthermal radiation from the central region of super-accreting active galactic nuclei. Astron. Astrophys. 2022, 664, A178. https://doi.org/10.1051/0004-6361/202243682

    work page doi:10.1051/0004-6361/202243682 2022

  16. [17]

    High-energy radiation from collisions of high-velocity clouds and the Galactic disc

    del Valle, M.V .; Müller, A.L.; Romero, G.E. High-energy radiation from collisions of high-velocity clouds and the Galactic disc. Mon. Not. R. Astron. Soc. 2018, 475, 4298–4308. https://doi.org/10.1093/mnras/stx2984

    work page doi:10.1093/mnras/stx2984 2018

  17. [18]

    Gamma-rays from reaccelerated cosmic rays in high-velocity clouds colliding with the Galactic disc.Mon

    del Valle, M.V . Gamma-rays from reaccelerated cosmic rays in high-velocity clouds colliding with the Galactic disc.Mon. Not. R. Astron. Soc. 2022, 509, 4448–4456. https://doi.org/10.1093/mnras/stab3206

    work page doi:10.1093/mnras/stab3206 2022

  18. [19]

    Evidence for neutrino emission from the nearby active galaxy NGC 1068

    Abbasi, R.; Ackermann, M.; Adams, J.; et al.. Evidence for neutrino emission from the nearby active galaxy NGC 1068. Science 2022, 378, 538–543

    2022

  19. [20]

    High energy neutrinos from radio-quiet active galactic nuclei

    Alvarez-Muñiz, J.; Mészáros, P . High energy neutrinos from radio-quiet active galactic nuclei. Phys. Rev. D 2004, 70, 123001. https://doi.org/10.1103/PhysRevD.70.123001

    work page doi:10.1103/physrevd.70.123001 2004

  20. [21]

    On the Origin of High-energy Neutrinos from NGC 1068: The Role of Nonthermal Coronal Activity

    Inoue, Y.; Khangulyan, D.; Doi, A. On the Origin of High-energy Neutrinos from NGC 1068: The Role of Nonthermal Coronal Activity. Astrophys. J. Lett. 2020, 891, L33. https://doi.org/10.3847/2041-8213/ab7661

    doi:10.3847/2041-8213/ab7661 2020

  21. [22]

    Gamma-ray and Neutrino Signals from Accretion Disk Coronae of Active Galactic Nuclei

    Inoue, Y.; Khangulyan, D.; Doi, A. Gamma-ray and Neutrino Signals from Accretion Disk Coronae of Active Galactic Nuclei. Galaxies 2021, 9, 36. https://doi.org/10.3390/galaxies9020036

    work page doi:10.3390/galaxies9020036 2021

  22. [23]

    Hidden Cores of Active Galactic Nuclei as the Origin of Medium-Energy Neutrinos: Critical Tests with the MeV Gamma-Ray Connection

    Murase, K.; Kimura, S.S.; Mészáros, P . Hidden Cores of Active Galactic Nuclei as the Origin of Medium-Energy Neutrinos: Critical Tests with the MeV Gamma-Ray Connection. Phys. Rev. Lett. 2020, 125, 011101. https://doi.org/10.1103/PhysRevLett.125.011101

    doi:10.1103/physrevlett.125.011101 2020

  23. [24]

    Hidden Hearts of Neutrino Active Galaxies

    Murase, K. Hidden Hearts of Neutrino Active Galaxies. Astrophys. J. Lett. 2022, 941, L17. https://doi.org/10.3847/2041-8213/ aca53c

    doi:10.3847/2041-8213/ 2022

  24. [25]

    High-Energy Neutrinos from Active Galactic Nuclei

    Murase, K.; Stecker, F.W. High-Energy Neutrinos from Active Galactic Nuclei. arXiv 2022, arXiv:2202.03381

    Pith/arXiv arXiv 2022

  25. [26]

    High-energy Neutrinos from Magnetized Coronae of Active Galactic Nuclei and Prospects for Identification of Seyfert Galaxies and Quasars in Neutrino Telescopes

    Kheirandish, A.; Murase, K.; Kimura, S.S. High-energy Neutrinos from Magnetized Coronae of Active Galactic Nuclei and Prospects for Identification of Seyfert Galaxies and Quasars in Neutrino Telescopes. Astrophys. J. 2021, 922, 45. https: //doi.org/10.3847/1538-4357/ac1c77

    doi:10.3847/1538-4357/ac1c77 2021

  26. [27]

    High-Energy Neutrinos from NGC 1068

    Anchordoqui, L.A.; Krizmanic, J.; Stecker, F. High-Energy Neutrinos from NGC 1068. In Proceedings of the 37th International Cosmic Ray Conference. Berlin, Germany, 12-23 July 2021; p. 993. https://doi.org/10.22323/1.395.0993. Universe 2025, 1, 0 22 of 24

    work page doi:10.22323/1.395.0993 2021

  27. [28]

    High-Energy Extragalactic Neutrino Astrophysics

    Kurahashi, N.; Murase, K.; Santander, M. High-Energy Extragalactic Neutrino Astrophysics. Annu. Rev. Nucl. Part. Sci. 2022, 72, 365–387. https://doi.org/10.1146/annurev-nucl-011122-061547

    doi:10.1146/annurev-nucl-011122-061547 2022

  28. [29]

    High-energy Neutrino Emission from NGC 1068 by Outflow-cloud Interactions.arXiv 2024, arXiv:2406.14001

    Huang, Y.H.; Wang, K.; Ma, Z.P . High-energy Neutrino Emission from NGC 1068 by Outflow-cloud Interactions.arXiv 2024, arXiv:2406.14001. https://doi.org/10.48550/arXiv.2406.14001

    Pith/arXiv arXiv doi:10.48550/arxiv.2406.14001 2024

  29. [30]

    Years delayed gamma-ray and radio afterglows originated from TDE wind-torus interactions

    Mou, G.; Wang, W. Years delayed gamma-ray and radio afterglows originated from TDE wind-torus interactions. Mon. Not. R. Astron. Soc. 2021, 507, 1684–1698. https://doi.org/10.1093/mnras/stab2261

    doi:10.1093/mnras/stab2261 2021

  30. [31]

    Reverberation Measurements for 17 Quasars and the Size-Mass-Luminosity Relations in Active Galactic Nuclei

    Kaspi, S.; Smith, P .S.; Netzer, H.; Maoz, D.; Jannuzi, B.T.; Giveon, U. Reverberation Measurements for 17 Quasars and the Size-Mass-Luminosity Relations in Active Galactic Nuclei. Astrophys. J. 2000, 533, 631–649. https://doi.org/10.1086/308704

    doi:10.1086/308704 2000

  31. [32]

    Black hole masses of tidal disruption event host galaxies

    Wevers, T.; van Velzen, S.; Jonker, P .G.; Stone, N.C.; Hung, T.; Onori, F.; Gezari, S.; Blagorodnova, N. Black hole masses of tidal disruption event host galaxies. Mon. Not. R. Astron. Soc. 2017, 471, 1694–1708. https://doi.org/10.1093/mnras/stx1703

    doi:10.1093/mnras/stx1703 2017

  32. [33]

    Black hole masses of tidal disruption event host galaxies II

    Wevers, T.; Stone, N.C.; van Velzen, S.; Jonker, P .G.; Hung, T.; Auchettl, K.; Gezari, S.; Onori, F.; Mata Sánchez, D.; Kostrzewa- Rutkowska, Z.; et al. Black hole masses of tidal disruption event host galaxies II. Mon. Not. R. Astron. Soc. 2019, 487, 4136–4152. https://doi.org/10.1093/mnras/stz1602

    work page doi:10.1093/mnras/stz1602 2019

  33. [34]

    Tidal-disruption rate of stars by spinning supermassive black holes

    Kesden, M. Tidal-disruption rate of stars by spinning supermassive black holes. Phys. Rev. D 2012, 85, 024037. https: //doi.org/10.1103/PhysRevD.85.024037

    doi:10.1103/physrevd.85.024037 2012

  34. [35]

    Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function

    Yao, Y.; Ravi, V .; Gezari, S.; van Velzen, S.; Lu, W.; Schulze, S.; Somalwar, J.J.; Kulkarni, S.R.; Hammerstein, E.; Nicholl, M.; et al. Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function. Astrophys. J. Lett. 2023, 955, L6. https://doi.org/...

    doi:10.3847/2041-8213/acf216 2023

  35. [36]

    Radiation from the impact of broad-line region clouds onto AGN accretion disks

    Müller, A.L.; Romero, G.E. Radiation from the impact of broad-line region clouds onto AGN accretion disks. Astron. Astrophys. 2020, 636, A92. https://doi.org/10.1051/0004-6361/202037639

    work page doi:10.1051/0004-6361/202037639 2020

  36. [37]

    The Radius-Luminosity Relationship for Active Galactic Nuclei: The Effect of Host-Galaxy Starlight on Luminosity Measurements

    Bentz, M.C.; Peterson, B.M.; Pogge, R.W.; Vestergaard, M.; Onken, C.A. The Radius-Luminosity Relationship for Active Galactic Nuclei: The Effect of Host-Galaxy Starlight on Luminosity Measurements. Astrophys. J. 2006, 644, 133–142. https: //doi.org/10.1086/503537

    doi:10.1086/503537 2006

  37. [38]

    Physical processes in active galactic nuclei

    Blandford, R.D. Physical processes in active galactic nuclei. In Active Galactic Nuclei; Blandford, R.D., Netzer, H., Woltjer, L., Courvoisier, T.J.L., Mayor, M., Eds.; Springer: Berlin/Heidelberg, Germany, 1990; pp. 161–275

    1990

  38. [39]

    Unified models for active galactic nuclei and quasars

    Antonucci, R. Unified models for active galactic nuclei and quasars. Annu. Rev. Astron. Astrophys. 1993, 31, 473–521. https://doi.org/10.1146/annurev.aa.31.090193.002353

    arXiv 1993

  39. [40]

    Is the Broad-Line Region Clumped or Smooth? Constraints from the Hα Profile in NGC 4395, the Least Luminous Seyfert 1 Galaxy

    Laor, A.; Barth, A.J.; Ho, L.C.; Filippenko, A.V . Is the Broad-Line Region Clumped or Smooth? Constraints from the Hα Profile in NGC 4395, the Least Luminous Seyfert 1 Galaxy. Astrophys. J. 2006, 636, 83–89. https://doi.org/10.1086/497908

    work page doi:10.1086/497908 2006

  40. [41]

    Revisiting the Unified Model of Active Galactic Nuclei

    Netzer, H. Revisiting the Unified Model of Active Galactic Nuclei. Annu. Rev. Astron. Astrophys. 2015, 53, 365–408. https: //doi.org/10.1146/annurev-astro-082214-122302

    doi:10.1146/annurev-astro-082214-122302 2015

  41. [42]

    Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei

    Du, P .; Hu, C.; Lu, K.X.; Wang, F.; Qiu, J.; Li, Y.R.; Bai, J.M.; Kaspi, S.; Netzer, H.; Wang, J.M.; et al. Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. I. First Results from a New Reverberation Mapping Campaign. Astrophys. J. 2014, 782, 45. https://doi.org/10.1088/0004-637X/782/1/45

    doi:10.1088/0004-637x/782/1/45 2014

  42. [43]

    Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei

    Du, P .; Lu, K.X.; Zhang, Z.X.; Huang, Y.K.; Wang, K.; Hu, C.; Qiu, J.; Li, Y.R.; Fan, X.L.; Fang, X.E.; et al. Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. V . A New Size-Luminosity Scaling Relation for the Broad-line Region. Astrophys. J. 2016, 825, 126. https://doi.org/10.3847/0004-637X/825/2/126

    doi:10.3847/0004-637x/825/2/126 2016

  43. [44]

    PS18kh: A New Tidal Disruption Event with a Non-axisymmetric Accretion Disk

    Holoien, T.W.S.; Huber, M.E.; Shappee, B.J.; Eracleous, M.; Auchettl, K.; Brown, J.S.; Tucker, M.A.; Chambers, K.C.; Kochanek, C.S.; Stanek, K.Z.; et al. PS18kh: A New Tidal Disruption Event with a Non-axisymmetric Accretion Disk. Astrophys. J. 2019, 880, 120. https://doi.org/10.3847/1538-4357/ab2ae1

    doi:10.3847/1538-4357/ab2ae1 2019

  44. [45]

    The Spectral Evolution of AT 2018dyb and the Presence of Metal Lines in Tidal Disruption Events

    Leloudas, G.; Dai, L.; Arcavi, I.; Vreeswijk, P .M.; Mockler, B.; Roy, R.; Malesani, D.B.; Schulze, S.; Wevers, T.; Fraser, M.; et al. The Spectral Evolution of AT 2018dyb and the Presence of Metal Lines in Tidal Disruption Events. Astrophys. J. 2019, 887, 218. https://doi.org/10.3847/1538-4357/ab5792

    doi:10.3847/1538-4357/ab5792 2019

  45. [46]

    Black hole winds

    King, A.R.; Pounds, K.A. Black hole winds. Mon. Not. R. Astron. Soc. 2003, 345, 657–659. https://doi.org/10.1046/j.1365-8711.20 03.06980.x

    work page doi:10.1046/j.1365-8711.20 2003

  46. [47]

    Black hole outflows

    King, A.R. Black hole outflows. Mon. Not. R. Astron. Soc. 2010, 402, 1516–1522

    2010

  47. [48]

    Exploring accretion disk physics and black hole growth with regular monitoring of ultrafast active galactic nucleus winds

    Pounds, K.; Lobban, A.; Nixon, C. Exploring accretion disk physics and black hole growth with regular monitoring of ultrafast active galactic nucleus winds. Astron. Nachrichten 2017, 338, 249–255. https://doi.org/10.1002/asna.201713338

    work page doi:10.1002/asna.201713338 2017

  48. [49]

    Seventeen Tidal Disruption Events from the First Half of ZTF Survey Observations: Entering a New Era of Population Studies

    van Velzen, S.; Gezari, S.; Hammerstein, E.; Roth, N.; Frederick, S.; Ward, C.; Hung, T.; Cenko, S.B.; Stein, R.; Perley, D.A.; et al. Seventeen Tidal Disruption Events from the First Half of ZTF Survey Observations: Entering a New Era of Population Studies. Astrophys. J. 2021, 908, 4. https://doi.org/10.3847/1538-4357/abc258

    doi:10.3847/1538-4357/abc258 2021

  49. [50]

    Comptonization in Super-Eddington Accretion Flow and Growth Timescale of Supermassive Black Holes

    Kawaguchi, T. Comptonization in Super-Eddington Accretion Flow and Growth Timescale of Supermassive Black Holes. Astrophys. J. 2003, 593, 69–84. https://doi.org/10.1086/376404. Universe 2025, 1, 0 23 of 24

    work page doi:10.1086/376404 2003

  50. [51]

    The Simultaneous Optical-to-X-Ray Spectral Energy Distribution of Soft X-Ray Selected Active Galactic Nuclei Observed by Swift

    Grupe, D.; Komossa, S.; Leighly, K.M.; Page, K.L. The Simultaneous Optical-to-X-Ray Spectral Energy Distribution of Soft X-Ray Selected Active Galactic Nuclei Observed by Swift. Astrophys. J. Suppl. Ser. 2010, 187, 64–106. https://doi.org/10.1088/0067-004 9/187/1/64

    doi:10.1088/0067-004 2010

  51. [52]

    Hyperaccretion during Tidal Disruption Events: Weakly Bound Debris Envelopes and Jets

    Coughlin, E.R.; Begelman, M.C. Hyperaccretion during Tidal Disruption Events: Weakly Bound Debris Envelopes and Jets. Astrophys. J. 2014, 781, 82. https://doi.org/10.1088/0004-637X/781/2/82

    doi:10.1088/0004-637x/781/2/82 2014

  52. [53]

    Observational Appearance and Spectrum of Black-Hole Winds

    Fukue, J.; Iino, E. Observational Appearance and Spectrum of Black-Hole Winds. Publ. Astron. Soc. Jpn. 2010, 62, 1399. https://doi.org/10.1093/pasj/62.6.1399

    work page doi:10.1093/pasj/62.6.1399 2010

  53. [54]

    Model for Population III microquasars

    Sotomayor Checa, P .; Romero, G.E. Model for Population III microquasars. Astron. Astrophys. 2019, 629, A76. https: //doi.org/10.1051/0004-6361/201834191

    work page doi:10.1051/0004-6361/201834191 2019

  54. [55]

    Supersonic Collisions between Two Gas Streams

    Lee, H.M.; Kang, H.; Ryu, D. Supersonic Collisions between Two Gas Streams. Astrophys. J. 1996, 464, 131. https://doi.org/10.1 086/177305

    work page 1996

  55. [56]

    The collision of clouds with the galactic disk

    Tenorio-Tagle, G. The collision of clouds with the galactic disk. Astron. Astrophys. 1981, 94, 338

    work page 1981

  56. [57]

    The violent interstellar medium

    McCray, R.; Snow, T.P ., Jr. The violent interstellar medium. Annu. Rev. Astron. Astrophys. 1979, 17, 213–240. https: //doi.org/10.1146/annurev.aa.17.090179.001241

    work page arXiv 1979

  57. [58]

    Neutral Atomic Phases of the Interstellar Medium in the Galaxy

    Wolfire, M.G.; McKee, C.F.; Hollenbach, D.; Tielens, A.G.G.M. Neutral Atomic Phases of the Interstellar Medium in the Galaxy. Astrophys. J. 2003, 587, 278–311. https://doi.org/10.1086/368016

    doi:10.1086/368016 2003

  58. [59]

    Estimating supermassive black hole masses in active galactic nuclei using polarization of broad Mg II, H α, and H β lines

    Savi´ c, Ð.; Popovi´ c, L.ˇC.; Shablovinskaya, E.; Afanasiev, V .L. Estimating supermassive black hole masses in active galactic nuclei using polarization of broad Mg II, H α, and H β lines. Mon. Not. R. Astron. Soc. 2020, 497, 3047–3054. https: //doi.org/10.1093/mnras/staa2039

    work page doi:10.1093/mnras/staa2039 2020

  59. [60]

    Gamma rays from cloud penetration at the base of AGN jets.Astron

    Araudo, A.T.; Bosch-Ramon, V .; Romero, G.E. Gamma rays from cloud penetration at the base of AGN jets.Astron. Astrophys. 2010, 522, A97. https://doi.org/10.1051/0004-6361/201014660

    doi:10.1051/0004-6361/201014660 2010

  60. [61]

    Starburst-Driven Galactic Winds: Filament Formation and Emission Processes

    Cooper, J.L.; Bicknell, G.V .; Sutherland, R.S.; Bland-Hawthorn, J. Starburst-Driven Galactic Winds: Filament Formation and Emission Processes. Astrophys. J. 2009, 703, 330–347. https://doi.org/10.1088/0004-637X/703/1/330

    doi:10.1088/0004-637x/703/1/330 2009

  61. [62]

    On the dynamics and survival of fractal clouds in galactic winds

    Banda-Barragán, W.E.; Zertuche, F.J.; Federrath, C.; García Del Valle, J.; Brüggen, M.; Wagner, A.Y. On the dynamics and survival of fractal clouds in galactic winds. Mon. Not. R. Astron. Soc. 2019, 486, 4526–4544. https://doi.org/10.1093/mnras/stz1040

    doi:10.1093/mnras/stz1040 2019

  62. [63]

    The origin of the broad line region in active galactic nuclei

    Czerny, B.; Hryniewicz, K. The origin of the broad line region in active galactic nuclei. Astron. Astrophys. 2011, 525, L8. https://doi.org/10.1051/0004-6361/201016025

    doi:10.1051/0004-6361/201016025 2011

  63. [64]

    Nonthermal Emission from Fall-back Clouds in the Broad-line Region of Active Galactic Nuclei

    Müller, A.L.; Naddaf, M.H.; Zajaˇ cek, M.; Czerny, B.; Araudo, A.; Karas, V . Nonthermal Emission from Fall-back Clouds in the Broad-line Region of Active Galactic Nuclei. Astrophys. J. 2022, 931, 39. https://doi.org/10.3847/1538-4357/ac660a

    doi:10.3847/1538-4357/ac660a 2022

  64. [65]

    Magnetic Fields in Molecular Clouds: Observations Confront Theory

    Crutcher, R.M. Magnetic Fields in Molecular Clouds: Observations Confront Theory. Astrophys. J. 1999, 520, 706–713. https://doi.org/10.1086/307483

    doi:10.1086/307483 1999

  65. [66]

    Magnetic Fields in Interstellar Clouds from Zeeman Observations: Inference of Total Field Strengths by Bayesian Analysis

    Crutcher, R.M.; Wandelt, B.; Heiles, C.; Falgarone, E.; Troland, T.H. Magnetic Fields in Interstellar Clouds from Zeeman Observations: Inference of Total Field Strengths by Bayesian Analysis. Astrophys. J. 2010, 725, 466–479. https://doi.org/10.1088/ 0004-637X/725/1/466

    work page 2010

  66. [67]

    Magnetic Properties of Star-forming Dense Cores

    Myers, P .C.; Basu, S. Magnetic Properties of Star-forming Dense Cores. Astrophys. J. 2021, 917, 35. https://doi.org/10.3847/1538 -4357/abf4c8

    doi:10.3847/1538 2021

  67. [68]

    Magnetic Fields in Molecular Clouds

    Crutcher, R.M. Magnetic Fields in Molecular Clouds. Annu. Rev. Astron. Astrophys. 2012, 50, 29–63. https://doi.org/10.1146/ annurev-astro-081811-125514

    work page 2012

  68. [69]

    Self-similar fragmentation regulated by magnetic fields in a region forming massive stars

    Li, H.B.; Yuen, K.H.; Otto, F.; Leung, P .K.; Sridharan, T.K.; Zhang, Q.; Liu, H.; Tang, Y.W.; Qiu, K. Self-similar fragmentation regulated by magnetic fields in a region forming massive stars. Nature 2015, 520, 518–521. https://doi.org/10.1038/nature14291

    doi:10.1038/nature14291 2015

  69. [70]

    Magnetic confinement of broad-line clouds in active galactic nuclei

    Rees, M.J. Magnetic confinement of broad-line clouds in active galactic nuclei. Mon. Not. R. Astron. Soc. 1987, 228, 47P–50P . https://doi.org/10.1093/mnras/228.1.47P

    doi:10.1093/mnras/228.1.47p 1987

  70. [71]

    Theory of Magnetically Powered Jets ; Lecture Notes in Physics; Belloni, T., Ed.; Springer: Berlin, Germany, 2010; Volume 794, p

    Spruit, H.C. Theory of Magnetically Powered Jets ; Lecture Notes in Physics; Belloni, T., Ed.; Springer: Berlin, Germany, 2010; Volume 794, p. 233. https://doi.org/10.1007/978-3-540-76937-8_9

    doi:10.1007/978-3-540-76937-8_9 2010

  71. [72]

    Gamma rays from jets interacting with BLR clouds in blazars

    del Palacio, S.; Bosch-Ramon, V .; Romero, G.E. Gamma rays from jets interacting with BLR clouds in blazars. Astron. Astrophys. 2019, 623, A101. https://doi.org/10.1051/0004-6361/201834231

    doi:10.1051/0004-6361/201834231 2019

  72. [73]

    Magnetic fields of active galactic nuclei and quasars with regions of polarized broad H α lines

    Silant’ev, N.A.; Gnedin, Y.N.; Buliga, S.D.; Piotrovich, M.Y.; Natsvlishvili, T.M. Magnetic fields of active galactic nuclei and quasars with regions of polarized broad H α lines. Astrophys. Bull. 2013, 68, 14–25. https://doi.org/10.1134/S1990341313010021

    work page doi:10.1134/s1990341313010021 2013

  73. [74]

    Determination of magnetic fields in broad line region of active galactic nuclei from polarimetric observations

    Piotrovich, M.; Silant’ev, N.; Gnedin, Y.; Natsvlishvili, T.; Buliga, S. Determination of magnetic fields in broad line region of active galactic nuclei from polarimetric observations. New Astron. 2017, 51, 65–68. https://doi.org/10.1016/j.newast.2016.08.004

    work page doi:10.1016/j.newast.2016.08.004 2017

  74. [75]

    Berezinskii, V .S.; Bulanov, S.V .; Dogiel, V .A.; Ptuskin, V .S.Astrophysics of Cosmic Rays ; North-Holland: Amsterdam, 1990

    work page 1990

  75. [76]

    Very high energy cosmic gamma radiation: A crucial window on the extreme Universe ; World Scientific: Singapore, 2004

    Aharonian, F.A. Very high energy cosmic gamma radiation: A crucial window on the extreme Universe ; World Scientific: Singapore, 2004. https://doi.org/10.1142/4657

    doi:10.1142/4657 2004

  76. [77]

    Detailed Numerical Investigation of the Bohm Limit in Cosmic Ray Diffusion Theory

    Hussein, M.; Shalchi, A. Detailed Numerical Investigation of the Bohm Limit in Cosmic Ray Diffusion Theory. Astrophys. J. 2014, 785, 31. https://doi.org/10.1088/0004-637X/785/1/31. Universe 2025, 1, 0 24 of 24

    doi:10.1088/0004-637x/785/1/31 2014

  77. [78]

    REVIEW ARTICLE: An introduction to the theory of diffusive shock acceleration of energetic particles in tenuous plasmas

    Drury, L.O. REVIEW ARTICLE: An introduction to the theory of diffusive shock acceleration of energetic particles in tenuous plasmas. Rep. Prog. Phys. 1983, 46, 973–1027. https://doi.org/10.1088/0034-4885/46/8/002

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

  78. [79]

    Energy spectra of gamma rays, electrons, and neutrinos produced at proton-proton interactions in the very high energy regime

    Kelner, S.R.; Aharonian, F.A.; Bugayov, V .V . Energy spectra of gamma rays, electrons, and neutrinos produced at proton-proton interactions in the very high energy regime. Phys. Rev. D 2006, 74, 034018. https://doi.org/10.1103/PhysRevD.74.034018

    doi:10.1103/physrevd.74.034018 2006

  79. [80]

    Neutrino astronomy with the next generation IceCube Neutrino Observatory

    Grant, D.; Ackermann, M.; Karle, A.; Kowalski, M. Neutrino astronomy with the next generation IceCube Neutrino Observatory. Bull. Am. Astron. Soc. 2019, 51, 288

    work page 2019

  80. [81]

    Active galactic nuclei

    Osterbrock, D.E. Active galactic nuclei. Rep. Prog. Phys. 1991, 54, 579–633. https://doi.org/10.1088/0034-4885/54/4/002

    doi:10.1088/0034-4885/54/4/002 1991

Showing first 80 references.

This paper was first reviewed by deepseek-v4-flash on August 5, 2026.