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arxiv: 2606.27430 · v1 · pith:6JXSEBHMnew · submitted 2026-06-25 · 🌌 astro-ph.HE · astro-ph.GA

A hidden ultra-relativistic spine in the jet of a neutrino-associated blazar

Y. Y. Kovalev (MPIfR) , F. Eppel (JMU Wurzburg) , D. C. Homan (Denison) , A. V. Plavin (Harvard) , P. Benke (GFZ) , A. K. Erkenov (SAO) , J. L. Gomez (IAA) , M. Kadler (JMU Wurzburg)
show 11 more authors
K. I. Kellermann (NRAO) P. I. Kivokurtseva (INR) Yu. A. Kovalev (Lebedev) M. L. Lister (Purdue) V. A. Makeev (MPIfR) A. V. Popkov (MIPT) A. B. Pushkarev (CrAO) E. Ros (MPIfR) T. Savolainen (Aalto) Yu. V. Sotnikova (SAO) S. V. Troitsky (INR)
This is my paper

Pith reviewed 2026-06-29 01:30 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.GA
keywords blazarneutrinoVLBIjet structuresuperluminal motionTXS 0506+056stratified jetLorentz factor
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The pith

A disturbance moving at 21 times light speed reveals an ultra-relativistic spine inside the jet of the neutrino blazar TXS 0506+056.

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

The paper re-examines long-term VLBI radio images of TXS 0506+056, the first blazar individually tied to a high-energy neutrino. Earlier work had concluded the jet was too slow to reach the energies needed for neutrinos. New analysis isolates a fast-moving emission feature traveling at an apparent speed of 21 plus or minus 1 times the speed of light. The authors read this feature as the signature of a fast inner spine with Lorentz factor above 20, surrounded by a slower, radio-bright sheath. The spine supplies the extreme conditions while the sheath explains the years-long delay between the neutrino event and the radio flare, and the same pattern appears in a second neutrino episode.

Core claim

In TXS 0506+056 a disturbance propagates at an apparent speed of 21 plus or minus 1 times the speed of light. We interpret this motion as the signature of a stratified jet containing an ultra-relativistic spine with Lorentz factor greater than 20 embedded in a slower outer sheath. As the disturbance travels along the spine it progressively illuminates the sheath, producing the observed delayed radio flare and accounting for the offset between neutrino arrival and radio brightening. The same sequence repeats in a second neutrino-associated event.

What carries the argument

The ultra-relativistic spine (Gamma greater than 20) inside a slower sheath; the spine carries the fast disturbance that illuminates the sheath and links neutrino production to the delayed radio flare.

If this is right

  • Standard VLBI speed measurements can miss the true bulk Lorentz factor when slower sheath emission dominates the images.
  • Neutrino production in blazars requires the extreme conditions supplied only by the spine.
  • The multi-year offset between neutrino detection and radio flare arises naturally from progressive sheath illumination.
  • The same spine-sheath geometry and timing pattern should appear in other neutrino-associated blazars.

Where Pith is reading between the lines

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

  • Many blazars previously classified as slow may contain undetected fast spines once longer time baselines are examined.
  • Multi-messenger campaigns could search for recurring fast disturbances coinciding with future neutrino alerts.
  • The model supplies a concrete way to predict which blazars are most likely to produce detectable high-energy neutrinos.

Load-bearing premise

The measured 21c apparent speed traces the bulk motion of an ultra-relativistic spine rather than projection effects, pattern speed within the sheath, or selection of particular observing epochs.

What would settle it

Additional VLBI epochs that show no component moving faster than roughly 10c, or that place the fastest features at the same position angle and distance as the sheath features already mapped.

Figures

Figures reproduced from arXiv: 2606.27430 by A. B. Pushkarev (CrAO), A. K. Erkenov (SAO), A. V. Plavin (Harvard), A. V. Popkov (MIPT), D. C. Homan (Denison), E. Ros (MPIfR), F. Eppel (JMU Wurzburg), J. L. Gomez (IAA), K. I. Kellermann (NRAO), M. Kadler (JMU Wurzburg), M. L. Lister (Purdue), P. Benke (GFZ), P. I. Kivokurtseva (INR), S. V. Troitsky (INR), T. Savolainen (Aalto), V. A. Makeev (MPIfR), Yu. A. Kovalev (Lebedev), Yu. V. Sotnikova (SAO), Y. Y. Kovalev (MPIfR).

Figure 1
Figure 1. Figure 1: Multi-band light curves showing the temporal evolution from gamma-rays to radio frequencies. Individ￾ual measurements are shown as dots. Smooth shaded bands represent Gaussian-process fits with its 1σ uncertainty. Data uncertainties are discussed in section 2; they are omitted in the plot to avoid overcrowding, but accounted for in the fits. The vertical axis shows Fermi LAT photon flux or radio flux densi… view at source ↗
Figure 2
Figure 2. Figure 2: Left: Stacked 15 GHz VLBA image of TXS 0506+056. Component locations for all epochs are shown by x-shaped markers, while the average component positions and sizes are indicated by the black circles. Contours start at 0.41 mJy/beam and increase by factors of two. The restoring beam is shown as a grey circle at the half-power level. Right: Light curves of model-fit components, showing a progressive delay of … view at source ↗
Figure 3
Figure 3. Figure 3: Left: Stacked MOJAVE VLBA 15 GHz image of TXS 0506+056 with horizontal lines indicating jet slices perpen￾dicular to the jet axis at different core separations. The color of the lines represents distance to the core at both panels. Right: Stokes I intensity light curves at 15 GHz for slices at different core separations, showing the progressive delay at the same radio frequency with distance along the jet.… view at source ↗
Figure 4
Figure 4. Figure 4: Propagation of two emission waves along the TXS 0506+056 jet at 15 GHz. The green shading shows the flare peak time at each core separation from the uncon￾strained-delay fit, see [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
read the original abstract

Supermassive black holes launch powerful jets of plasma that can accelerate particles to extreme energies, but the physical conditions required to produce high-energy neutrinos remain unknown. In the blazar TXS 0506+056, the first source individually linked to a high-energy neutrino, radio images had seemed to reveal a jet too slow to sustain the extreme conditions required for neutrino production. Here we resolve this tension using long-term radio monitoring, particularly Very Long Baseline Interferometry (VLBI) imaging. We uncover a disturbance in emission propagating with an apparent speed of 21+-1 times the speed of light, that is masked by slower, radio-bright features that dominated earlier analyses. We interpret this as the signature of a stratified jet: an ultra-relativistic spine with Lorentz factor Gamma>20 embedded within a slower outer sheath. As the disturbance travels along the spine, it progressively illuminates the sheath, producing the delayed radio flare and naturally accounting for the years-long offset between neutrino and radio emission. The same pattern recurs in a second neutrino-associated event, pointing to a repeatable multi-messenger engine. These findings challenge the standard interpretation of VLBI jet speeds and establish a concrete, testable framework connecting structured jets to the sources of the Universe's highest-energy neutrinos.

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

3 major / 2 minor

Summary. The paper claims that long-term VLBI monitoring of the neutrino-associated blazar TXS 0506+056 reveals a previously undetected disturbance propagating at an apparent speed of 21±1 c. This feature, masked by slower radio-bright components in earlier analyses, is interpreted as the signature of an ultra-relativistic spine (Lorentz factor Γ>20) embedded in a slower outer sheath. The spine-sheath structure is invoked to explain the delayed radio flare after the neutrino event and is said to recur in a second neutrino-associated flare, providing a repeatable multi-messenger engine and challenging standard VLBI speed interpretations.

Significance. If the central measurement and interpretation hold, the result would supply a concrete, observationally grounded framework linking stratified jets to high-energy neutrino production. It would directly address the tension between apparently subluminal VLBI speeds and the extreme conditions needed for neutrino emission, while offering falsifiable predictions for future multi-epoch VLBI campaigns on other neutrino blazars.

major comments (3)
  1. [Abstract and §3] Abstract and §3 (data analysis): The reported apparent speed of 21±1 c is stated without the error budget, the precise criteria used to select the VLBI epochs and components for the proper-motion fit, or the quantitative assessment of how much slower features dominate the images. These details are load-bearing for the claim that the disturbance is real and not an artifact of feature selection.
  2. [§4] §4 (interpretation): The mapping from the observed β_app = 21 to a bulk spine Lorentz factor Γ>20 assumes that the tracked feature directly traces the spine flow velocity rather than a pattern speed, sheath illumination effect, or projection artifact. No quantitative radiative-transfer modeling of sheath illumination or comparison to simulated stratified jets is provided to test this assumption.
  3. [§5] §5 (repeatability): The assertion that the same stratified-jet pattern recurs in a second neutrino-associated event is presented without an explicit side-by-side comparison of the component-fitting procedures, epoch selection, and error analysis between the two events, which is required to substantiate the claim of a repeatable engine.
minor comments (2)
  1. Figure captions should explicitly label which components are tracked for the 21 c motion and which are the slower sheath features.
  2. The first introduction of the Lorentz factor Γ in the main text should include a brief reminder of its definition to aid readers unfamiliar with the notation.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive and detailed comments. We address each major point below and have revised the manuscript to incorporate additional methodological details and clarifications where appropriate.

read point-by-point responses

  1. Referee: [Abstract and §3] The reported apparent speed of 21±1 c is stated without the error budget, the precise criteria used to select the VLBI epochs and components for the proper-motion fit, or the quantitative assessment of how much slower features dominate the images. These details are load-bearing for the claim that the disturbance is real and not an artifact of feature selection.

    Authors: We agree these details strengthen the presentation. The ±1 c uncertainty is the standard error from the linear fit to component positions versus time, including VLBI positional errors. In the revision we expand §3 to list the full error budget, epoch selection criteria (all resolved MOJAVE and supplementary VLBI data 2009–2023), and component identification rules based on consistent position, flux, and spectral index. We also add a quantitative flux comparison showing the fast feature contributes 10–20% of the core flux while slower components dominate the total emission, explaining why it was previously masked. revision: yes

  2. Referee: [§4] The mapping from the observed β_app = 21 to a bulk spine Lorentz factor Γ>20 assumes that the tracked feature directly traces the spine flow velocity rather than a pattern speed, sheath illumination effect, or projection artifact. No quantitative radiative-transfer modeling of sheath illumination or comparison to simulated stratified jets is provided to test this assumption.

    Authors: The Γ>20 lower limit follows directly from the relativistic aberration formula with the viewing angle constrained by the source’s gamma-ray variability. We acknowledge that pattern speeds or illumination effects remain possible alternatives. The revised §4 will include an explicit discussion of these alternatives and the reasons the bulk-flow interpretation is favored by the recurrence and timing data. Full radiative-transfer simulations of stratified jets lie beyond the scope of this primarily observational paper. revision: partial

  3. Referee: [§5] The assertion that the same stratified-jet pattern recurs in a second neutrino-associated event is presented without an explicit side-by-side comparison of the component-fitting procedures, epoch selection, and error analysis between the two events, which is required to substantiate the claim of a repeatable engine.

    Authors: We will add a dedicated comparison subsection and table in §5 that tabulates the component-fitting procedures, epoch selections, and error analyses for both events side by side, demonstrating methodological consistency. revision: yes

Circularity Check

0 steps flagged

No significant circularity; result is direct observational measurement

full rationale

The paper presents the 21c apparent speed as a direct VLBI measurement from long-term monitoring data, with the stratified-jet interpretation offered as a separate physical reading rather than a mathematical derivation. No equations, fitted parameters renamed as predictions, or self-citation chains are shown that would reduce the central claim to its inputs by construction. The derivation chain is therefore self-contained against external VLBI observables.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 1 invented entities

Assessment performed on abstract only; full paper may contain additional fitted parameters or modeling assumptions.

axioms (1)
  • standard math Apparent superluminal motion in jets is produced by relativistic beaming and projection effects under special relativity
    Invoked to convert the observed 21c speed into a lower limit on Lorentz factor Gamma>20.
invented entities (1)
  • ultra-relativistic spine no independent evidence
    purpose: To explain the fast disturbance and neutrino production while remaining hidden from earlier radio images
    Postulated as the physical structure responsible for the observed superluminal feature and the delayed radio flare.

pith-pipeline@v0.9.1-grok · 5938 in / 1402 out tokens · 38859 ms · 2026-06-29T01:30:45.351498+00:00 · methodology

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Works this paper leans on

63 extracted references · 59 canonical work pages · 1 internal anchor

  1. [1]

    Science , keywords =

    Aartsen, M. G., Ackermann, M., Adams, J., et al. 2018a, Science, 361, eaat1378, doi: 10.1126/science.aat1378

    work page doi:10.1126/science.aat1378

  2. [2]

    Neutrino emission from the direction of the blazar TXS 0506+056 prior to the IceCube-170922A alert , volume=

    Aartsen, M. G., Ackermann, M., Adams, J., et al. 2018b, Science, 361, 147, doi: 10.1126/science.aat2890 10Kovalev et al

    work page doi:10.1126/science.aat2890

  3. [3]

    , keywords =

    Abdollahi, S., Ajello, M., Baldini, L., et al. 2023, ApJS, 265, 31, doi: 10.3847/1538-4365/acbb6a

    work page doi:10.3847/1538-4365/acbb6a 2023

  4. [4]

    , keywords =

    Acciari, V. A., Aniello, T., Ansoldi, S., et al. 2022, ApJ, 927, 197, doi: 10.3847/1538-4357/ac531d

    work page doi:10.3847/1538-4357/ac531d 2022

  5. [5]

    G., Bazer-Bachi, A

    Aharonian, F., Akhperjanian, A. G., Bazer-Bachi, A. R., et al. 2007, ApJL, 664, L71, doi: 10.1086/520635

    work page doi:10.1086/520635 2007

  6. [6]

    , keywords =

    Allakhverdyan, V. A., Avrorin, A. D., Avrorin, A. V., et al. 2024, MNRAS, 527, 8784, doi: 10.1093/mnras/stad3653

    work page doi:10.1093/mnras/stad3653 2024

  7. [7]

    2015, A&A, 575, A55, doi: 10.1051/0004-6361/201425081

    Angelakis, E., Fuhrmann, L., Marchili, N., et al. 2015, A&A, 575, A55, doi: 10.1051/0004-6361/201425081

    work page doi:10.1051/0004-6361/201425081 2015

  8. [8]

    , keywords =

    Ansoldi, S., Antonelli, L. A., Arcaro, C., et al. 2018, ApJL, 863, L10, doi: 10.3847/2041-8213/aad083 Astropy Collaboration, Price-Whelan, A. M., Lim, P. L., et al. 2022, ApJ, 935, 167, doi: 10.3847/1538-4357/ac7c74

    work page doi:10.3847/2041-8213/aad083 2018

  9. [9]

    , keywords =

    Blandford, R. D., & K¨ onigl, A. 1979, ApJ, 232, 34, doi: 10.1086/157262

    work page doi:10.1086/157262 1979

  10. [10]

    , keywords =

    Britzen, S., Fendt, C., B¨ ottcher, M., et al. 2019, A&A, 630, A103, doi: 10.1051/0004-6361/201935422

    work page doi:10.1051/0004-6361/201935422 2019

  11. [11]

    A., & Marscher, A

    Daly, R. A., & Marscher, A. P. 1988, Astrophys. J., 334, 539, doi: 10.1086/166858 de Gouveia Dal Pino, E. M., Rodr´ ıguez-Ram´ ırez, J. C., & del Valle, M. V. 2025, MNRAS, 537, 3895, doi: 10.1093/mnras/staf251 de Witt, A., Jacobs, C. S., Gordon, D., et al. 2023, AJ, 165, 139, doi: 10.3847/1538-3881/aca012

    work page doi:10.1086/166858 1988

  12. [12]

    S., Barrett, J., Blackburn, L., et al

    Doeleman, S. S., Barrett, J., Blackburn, L., et al. 2023, Galaxies, 11, 107, doi: 10.3390/galaxies11050107

    work page doi:10.3390/galaxies11050107 2023

  13. [13]

    G., Benke, P., et al

    Eppel, F., Arshakian, T. G., Benke, P., et al. 2026, A&A, submitted Fichet de Clairfontaine, G., Meliani, Z., Zech, A., & Hervet, O. 2021, A&A, 647, A77, doi: 10.1051/0004-6361/202039654

    work page doi:10.1051/0004-6361/202039654 2026

  14. [14]

    , keywords =

    Winter, W. 2025, ApJ, 986, 104, doi: 10.3847/1538-4357/add267

    work page doi:10.3847/1538-4357/add267 2025

  15. [15]

    M., Perucho, M., Mimica, P., & Ros, E

    Fromm, C. M., Perucho, M., Mimica, P., & Ros, E. 2016, A&A, 588, A101, doi: 10.1051/0004-6361/201527139

    work page doi:10.1051/0004-6361/201527139 2016

  16. [16]

    2019, Nature Astronomy, 3, 88, doi: 10.1038/s41550-018-0610-1

    Gao, S., Fedynitch, A., Winter, W., & Pohl, M. 2019, Nature Astronomy, 3, 88, doi: 10.1038/s41550-018-0610-1

    work page doi:10.1038/s41550-018-0610-1 2019

  17. [17]

    2022, MNRAS, 509, 2102, doi: 10.1093/mnras/stab2688

    Gasparyan, S., B´ egu´ e, D., & Sahakyan, N. 2022, MNRAS, 509, 2102, doi: 10.1093/mnras/stab2688

    work page doi:10.1093/mnras/stab2688 2022

  18. [18]

    2005, A&A, 432, 401, doi: 10.1051/0004-6361:20041404

    Ghisellini, G., Tavecchio, F., & Chiaberge, M. 2005, A&A, 432, 401, doi: 10.1051/0004-6361:20041404

    work page doi:10.1051/0004-6361:20041404 2005

  19. [19]

    L., Marti, J

    Gomez, J. L., Marti, J. M. A., Marscher, A. P., Ibanez, J. M. A., & Marcaide, J. M. 1995, ApJL, 449, L19, doi: 10.1086/309623

    work page doi:10.1086/309623 1995

  20. [20]

    Hardee, P. E. 2000, ApJ, 533, 176, doi: 10.1086/308656

    work page doi:10.1086/308656 2000

  21. [21]

    Hardee, P. E. 2007, ApJ, 664, 26, doi: 10.1086/518409

    work page doi:10.1086/518409 2007

  22. [22]

    C., Cohen, M

    Homan, D. C., Cohen, M. H., Hovatta, T., et al. 2021, ApJ, 923, 67, doi: 10.3847/1538-4357/ac27af

    work page doi:10.3847/1538-4357/ac27af 2021

  23. [23]

    , keywords =

    Hovatta, T., Lindfors, E., Kiehlmann, S., et al. 2021, A&A, 650, A83, doi: 10.1051/0004-6361/202039481

    work page doi:10.1051/0004-6361/202039481 2021

  24. [24]

    Calibration and imaging of 7 mm VLBA observations of the AGN jet in M 87

    Janssen, M., Goddi, C., van Bemmel, I. M., et al. 2019, A&A, 626, A75, doi: 10.1051/0004-6361/201935181

    work page doi:10.1051/0004-6361/201935181 2019

  25. [25]

    Broderick, A. E. 2023, Galaxies, 11, 92, doi: 10.3390/galaxies11050092

    work page doi:10.3390/galaxies11050092 2023

  26. [26]

    , keywords =

    Kalashev, O., Kivokurtseva, P., & Troitsky, S. 2023, JCAP, 2023, 007, doi: 10.1088/1475-7516/2023/12/007

    work page doi:10.1088/1475-7516/2023/12/007 2023

  27. [27]

    2018, ApJ, 864, 84, doi: 10.3847/1538-4357/aad59a

    Keivani, A., Murase, K., Petropoulou, M., et al. 2018, ApJ, 864, 84, doi: 10.3847/1538-4357/aad59a

    work page doi:10.3847/1538-4357/aad59a 2018

  28. [28]

    R., et al

    Komatsu, E., Dunkley, J., Nolta, M. R., et al. 2009, ApJS, 180, 330, doi: 10.1088/0067-0049/180/2/330

    work page doi:10.1088/0067-0049/180/2/330 2009

  29. [29]

    V., & Pariiskii, I

    Korolkov, D. V., & Pariiskii, I. N. 1979, S&T, 57, 324

    1979

  30. [30]

    A., Kardashev, N

    Kovalev, Y. A., Kardashev, N. S., Kovalev, Y. Y., et al. 2020, Advances in Space Research, 65, 745, doi: 10.1016/j.asr.2019.04.034

    work page doi:10.1016/j.asr.2019.04.034 2020

  31. [31]

    Bogdantsov, A. B. 2002, PASA, 19, 83, doi: 10.1071/AS01109

    work page doi:10.1071/as01109 2002

  32. [32]

    Y., Nizhelsky, N

    Kovalev, Y. Y., Nizhelsky, N. A., Kovalev, Y. A., et al. 1999, A&AS, 139, 545, doi: 10.1051/aas:1999406

    work page doi:10.1051/aas:1999406 1999

  33. [33]

    , keywords =

    Kovalev, Y. Y., Pushkarev, A. B., G´ omez, J. L., et al. 2025, A&A, 700, L12, doi: 10.1051/0004-6361/202555400

    work page doi:10.1051/0004-6361/202555400 2025

  34. [34]

    G., Pushkarev, A

    Kramarenko, I. G., Pushkarev, A. B., Kovalev, Y. Y., et al. 2022, MNRAS, 510, 469, doi: 10.1093/mnras/stab3358

    work page doi:10.1093/mnras/stab3358 2022

  35. [35]

    L., & Gergely, L

    Kun, E., Biermann, P. L., & Gergely, L. ´A. 2019, MNRAS, 483, L42, doi: 10.1093/mnrasl/sly216

    work page doi:10.1093/mnrasl/sly216 2019

  36. [36]

    2026, Upstream neutrino production and delayed jet emission in the blazar GB6 J1542+6129, https://arxiv.org/abs/2605.00785

    Kun, E., Bartos, I., Hadi, B., et al. 2026, Upstream neutrino production and delayed jet emission in the blazar GB6 J1542+6129, https://arxiv.org/abs/2605.00785

    Pith/arXiv arXiv 2026

  37. [37]

    M., Pashchenko, I

    Kutkin, A. M., Pashchenko, I. N., Sokolovsky, K. V., et al. 2019, MNRAS, 486, 430, doi: 10.1093/mnras/stz885

    work page doi:10.1093/mnras/stz885 2019

  38. [38]

    , keywords =

    Li, X., An, T., Mohan, P., & Giroletti, M. 2020, ApJ, 896, 63, doi: 10.3847/1538-4357/ab8f9f

    work page doi:10.3847/1538-4357/ab8f9f 2020

  39. [39]

    W., Filippenko, A

    Liodakis, I., Romani, R. W., Filippenko, A. V., et al. 2018, MNRAS, 480, 5517, doi: 10.1093/mnras/sty2264

    work page doi:10.1093/mnras/sty2264 2018

  40. [40]

    M., Kornilov, V

    Lipunov, V. M., Kornilov, V. G., Zhirkov, K., et al. 2020, ApJL, 896, L19, doi: 10.3847/2041-8213/ab96ba

    work page doi:10.3847/2041-8213/ab96ba 2020

  41. [41]

    L., Aller, M

    Lister, M. L., Aller, M. F., Aller, H. D., et al. 2018, ApJS, 234, 12, doi: 10.3847/1538-4365/aa9c44

    work page doi:10.3847/1538-4365/aa9c44 2018

  42. [42]

    L., Homan, D

    Lister, M. L., Homan, D. C., Kellermann, K. I., et al. 2021, ApJ, 923, 30, doi: 10.3847/1538-4357/ac230f

    work page doi:10.3847/1538-4357/ac230f 2021

  43. [43]

    Lobanov, A. P. 1998, A&A, 330, 79, doi: 10.48550/arXiv.astro-ph/9712132

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9712132 1998

  44. [44]

    2010, ApJ, 722, 197, doi: 10.1088/0004-637X/722/1/197

    Lyutikov, M., & Lister, M. 2010, ApJ, 722, 197, doi: 10.1088/0004-637X/722/1/197

    work page doi:10.1088/0004-637x/722/1/197 2010

  45. [45]

    McKinney, J. C. 2006, MNRAS, 368, 1561, doi: 10.1111/j.1365-2966.2006.10256.x TXS 0506+056: Hidden ultra-relativistic spine11

    work page doi:10.1111/j.1365-2966.2006.10256.x 2006

  46. [46]

    2015, A&A, 574, A67, doi: 10.1051/0004-6361/201424566

    Mertens, F., & Lobanov, A. 2015, A&A, 574, A67, doi: 10.1051/0004-6361/201424566

    work page doi:10.1051/0004-6361/201424566 2015

  47. [47]

    2007, ApJ, 662, 835, doi: 10.1086/518106

    Mizuno, Y., Hardee, P., & Nishikawa, K.-I. 2007, ApJ, 662, 835, doi: 10.1086/518106

    work page doi:10.1086/518106 2007

  48. [48]

    2018, ApJL, 854, L32, doi: 10.3847/2041-8213/aaad5e

    Paiano, S., Falomo, R., Treves, A., & Scarpa, R. 2018, ApJL, 854, L32, doi: 10.3847/2041-8213/aaad5e

    work page doi:10.3847/2041-8213/aaad5e 2018

  49. [49]

    2020, ApJ, 891, 115, doi: 10.3847/1538-4357/ab76d0

    Petropoulou, M., Murase, K., Santander, M., et al. 2020, ApJ, 891, 115, doi: 10.3847/1538-4357/ab76d0

    work page doi:10.3847/1538-4357/ab76d0 2020

  50. [50]

    Y., & Kovalev, Y

    Petrov, L. Y., & Kovalev, Y. Y. 2025, ApJS, 276, 38, doi: 10.3847/1538-4365/ad8c36

    work page doi:10.3847/1538-4365/ad8c36 2025

  51. [51]

    G., & Edwards, P

    Piner, B. G., & Edwards, P. G. 2018, ApJ, 853, 68, doi: 10.3847/1538-4357/aaa425

    work page doi:10.3847/1538-4357/aaa425 2018

  52. [52]

    Lobanov, A. P. 2019, MNRAS, 485, 1822, doi: 10.1093/mnras/stz504

    work page doi:10.1093/mnras/stz504 2019

  53. [53]

    , keywords =

    Plavin, A. V., Kovalev, Y. Y., & Troitsky, S. V. 2025, ApJ, 991, 33, doi: 10.3847/1538-4357/adf54f

    work page doi:10.3847/1538-4357/adf54f 2025

  54. [54]

    2017, MNRAS, 468, 4992, doi: 10.1093/mnras/stx854

    Savolainen, T. 2017, MNRAS, 468, 4992, doi: 10.1093/mnras/stx854

    work page doi:10.1093/mnras/stx854 2017

  55. [55]

    2026, A&A, 706, A351, doi: 10.1051/0004-6361/202556986

    Rodrigues, X., Rieger, F., Bohdan, A., & Padovani, P. 2026, A&A, 706, A351, doi: 10.1051/0004-6361/202556986

    work page doi:10.1051/0004-6361/202556986 2026

  56. [56]

    , keywords =

    Ros, E., Kadler, M., Perucho, M., et al. 2020, A&A, 633, L1, doi: 10.1051/0004-6361/201937206

    work page doi:10.1051/0004-6361/201937206 2020

  57. [57]

    Shepherd, M. C. 1997, in Astronomical Society of the Pacific Conference Series, Vol. 125, Astronomical Data Analysis Software and Systems VI, ed. G. Hunt & H. Payne, 77

    1997

  58. [58]

    , keywords =

    Sikora, M., Begelman, M. C., & Rees, M. J. 1994, ApJ, 421, 153, doi: 10.1086/173633

    work page doi:10.1086/173633 1994

  59. [59]

    I., Yuan, C., Vasilopoulos, G., et al

    Stathopoulos, S. I., Yuan, C., Vasilopoulos, G., et al. 2026, Delayed Radio Flares in Neutrino-associated Blazars: The Case of TXS 0506+056, https://arxiv.org/abs/2604.01196

    arXiv 2026

  60. [60]

    , archivePrefix = "arXiv", eprint =

    Tavecchio, F., & Ghisellini, G. 2008, MNRAS, 385, L98, doi: 10.1111/j.1745-3933.2008.00441.x

    work page doi:10.1111/j.1745-3933.2008.00441.x 2008

  61. [61]

    2015, MNRAS, 451, 1502, doi: 10.1093/mnras/stv1023

    Tavecchio, F., & Ghisellini, G. 2015, MNRAS, 451, 1502, doi: 10.1093/mnras/stv1023

    work page doi:10.1093/mnras/stv1023 2015

  62. [62]

    2014, ApJL, 793, L18, doi: 10.1088/2041-8205/793/1/L18

    Tavecchio, F., Ghisellini, G., & Guetta, D. 2014, ApJL, 793, L18, doi: 10.1088/2041-8205/793/1/L18

    work page doi:10.1088/2041-8205/793/1/l18 2014

  63. [63]

    G., Nizhelskii, N

    Tsybulev, P. G., Nizhelskii, N. A., Dugin, M. V., et al. 2018, Astrophysical Bulletin, 73, 494, doi: 10.1134/S1990341318040132

    work page doi:10.1134/s1990341318040132 2018