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arxiv: 2605.13469 · v1 · submitted 2026-05-13 · 🌌 astro-ph.HE · astro-ph.GA

Recognition: no theorem link

The impact of flickering variability and magnetisation on the dynamics, stability and morphology of radio-loud AGN jets

Alex J. Cooper, Emma L. Elley, Henry Whitehead, James H. Matthews

Authors on Pith no claims yet

Pith reviewed 2026-05-14 18:09 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.GA
keywords radio-loud AGN jetsmagnetizationjet variabilitycocoonskink instabilitiesrelativistic MHDjet morphologyradio galaxies
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The pith

High magnetization and flickering variability produce asymmetrical cocoons and broken jet beams in radio-loud AGN jets.

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

This paper runs a grid of relativistic magnetohydrodynamic simulations to test how magnetization and flickering jet power together shape the cocoons and stability of radio galaxies. Constant high-magnetization jets form highly asymmetrical cocoon structures, while the same magnetization level with added flickering produces a discontinuous jet beam and broken overall morphology. The simulations show that magnetization and variability both matter for jet stability beyond just power or surroundings, and their interaction triggers localized kink instabilities. Low-magnetization runs instead show more hydrodynamic mixing, and a library of synthetic radio images at multiple times and viewing angles is supplied for direct comparison with observations.

Core claim

Constant high-magnetization jets develop highly asymmetrical cocoon morphologies, whereas variable high-magnetization jets exhibit broken morphologies caused by a discontinuous jet beam; the interplay between magnetization and variability also drives localized kink instabilities along the jet.

What carries the argument

Grid of relativistic magnetohydrodynamic simulations using the PLUTO code that compare constant versus flickering jet power at two fixed magnetization levels and track the resulting cocoon asymmetry, beam continuity, and instability growth.

Load-bearing premise

The two chosen magnetization values and the specific flickering prescription are representative of real AGN jets and the grid resolution captures the reported instabilities without numerical artifacts.

What would settle it

Detection of continuous, unbroken jet beams in sources inferred to have high magnetization and variable power, or symmetrically shaped cocoons in constant high-magnetization cases, would contradict the simulation outcomes.

Figures

Figures reproduced from arXiv: 2605.13469 by Alex J. Cooper, Emma L. Elley, Henry Whitehead, James H. Matthews.

Figure 1
Figure 1. Figure 1: Jet power as a function of Lorentz factor for various values of the peak magnetisation (𝜎𝐵,peak) and for jets with radius 𝑟𝑗 = 0.4 kpc (solid lines) and 𝑟𝑗 = 0.1 kpc (dashed lines). The jets we simulate in this work have a radius of 0.4 kpc. The curves for 𝜎𝐵,peak = 0.01 and 𝜎𝐵,peak = 0.001 have approximately equal values at all points. 0 1 2 3 4 5 Time (Myr) 3.0 3.5 4.0 4.5 5.0 5.5 6.0 6.5 7.0 Lorentz fac… view at source ↗
Figure 2
Figure 2. Figure 2 [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Central slices through the variable, high magnetisation simulation showing the density, pressure, the component of the magnetic field perpendicular to the plane (𝐵⊥), which is equivalent to the toroidal component at the jet base and the fraction of jet material (jet tracer). The full size of the slice is 60 kpc by 60 kpc. The cocoon shape of the variable jet shows a strong dependence on the recent power of… view at source ↗
Figure 4
Figure 4. Figure 4: shows a central slice through the toroidal magnetic field component of the high magnetisation constant power jet, at six time stamps between 1.2 and 3.2 Myr. At around 2 Myr the jet moves away significantly from the central axis. The ram pressure of the jet is concentrated on the area immediately around the end of the jet beam and, over a period of ∼ 1 Myr, preferentially excavates a significant volume of … view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of simulated radio images of the constant and variable high magnetisation jets at various times in their evolution. At 3 Myr, the cocoon of the high magnetisation constant jet shows significant asymmetry around the jet head. At 3.5 and 4.0 Myr, this jet is misaligned with the central axis of the cocoon. The variable high magnetisation jet has a cocoon that is approximately symmetrical on large l… view at source ↗
Figure 6
Figure 6. Figure 6: Tracer (fraction of material in a cell which entered the simulation through the jet nozzle) for the cells where the value of the tracer is above 0.5. The figure shows that the high magnetisation jet beam is more protected from mixing with the cocoon material and can sometimes form a discontinuous pattern of clumps of jet material travelling towards the jet head. The three-dimensional grid of tracer values … view at source ↗
Figure 7
Figure 7. Figure 7: Broken jet structures form as a result of magnetic instabilities, which form due to propagating disturbances in the jet pressure. Slices through the variable high magnetisation jet simulation, showing the component of the magnetic field perpendicular to the slice (𝐵⊥, toroidal component at the jet base), pressure and the fraction of jet material (tracer). Limits on the pressure colour scale are chosen to a… view at source ↗
Figure 8
Figure 8. Figure 8 [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Three illustrative examples of simulated radio images for the high magnetisation, variable power jet at different times in its evolution. All images are made with a dynamic range of 3 dex in brightness, however the limits of the brightness scale vary between images to account for differences in overall brightness due to age and boosting. The spatial scale (which reflects the distance projected onto the pla… view at source ↗
Figure 10
Figure 10. Figure 10: shows the constant power jet with 𝜎𝐵 = 0.01 at 4 Myr from different viewing angles, but all with the jet axis aligned with the plane of the sky. From some viewing angles, the cocoon shape at the jet head is clearly asymmetrical. From others, the jet appears misaligned with the central axis of the cocoon. In summary, whilst some aspect of large-scale asymmetry is present in most of the panels shown, there … view at source ↗
Figure 11
Figure 11. Figure 11: High magnetisation, constant power jet at 4 Myr, shown at 5 different angles to the line of sight, given in the top right of each image. In the first row, the left hand jet is approaching the observer. As we move through the images, this left hand jet moves away from the observer, through the plane of the sky in the third image and then continues until the right hand jet is approaching and at an angle of … view at source ↗
read the original abstract

The physics governing the morphology of radio-loud AGN jets is not fully understood. We investigate how magnetization, flickering jet power and their interplay affects the morphology of radio galaxies. We present a grid of relativistic magnetohydrodynamic simulations using the PLUTO code covering constant and variable jets with two levels of magnetisation. We find that the constant high magnetisation jets can lead to highly asymmetrical cocoon morphologies, whilst the variable high magnetisation jet can exhibit a broken morphology, caused by a discontinuous jet beam. Our work highlights the importance of magnetisation and variability on the stability and resulting morphology of radio-loud AGN jets, suggesting both are significant factors in addition to jet power or environment. Furthermore, we show that the interaction between magnetisation and variability can lead to the development of localised kink instabilities along the jet beam. Finally, we discuss the effects of hydrodynamic mixing in low magnetisation jets and the role of viewing angle dependence in comparisons between our simulations and observed sources. To facilitate this comparison we present a library of simulated radio images at different times in the simulations and from various viewing angles, which highlight a diverse set of complex morphologies.

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

2 major / 2 minor

Summary. The paper presents a grid of PLUTO relativistic MHD simulations of AGN jets comparing constant and flickering (variable-power) cases at two magnetization levels. It claims that constant high-magnetization jets produce highly asymmetrical cocoon morphologies while variable high-magnetization jets develop broken morphologies caused by a discontinuous jet beam, both driven by the growth of kink instabilities from the magnetization–variability interplay. The work also discusses hydrodynamic mixing in low-magnetization runs, viewing-angle effects, and supplies a library of synthetic radio images for observational comparison.

Significance. If the reported morphologies prove robust, the study usefully isolates magnetization and flickering variability as additional controls on jet stability and large-scale structure, complementing existing work on jet power and ambient density. The provision of multi-view synthetic images is a concrete strength that facilitates direct comparison with radio-galaxy observations.

major comments (2)
  1. [methods / simulation setup] Simulation setup (methods section): the grid resolution employed for the PLUTO RMHD runs is not stated and no resolution-doubled control simulations are shown for the high-magnetization cases. Because numerical diffusivity at the jet–cocoon shear layer can seed or damp current-driven kink modes, the absence of convergence tests leaves open the possibility that the reported asymmetrical cocoons and broken beams are partly numerical artifacts rather than physical outcomes of the magnetization–variability interaction.
  2. [results / high-magnetization runs] Results on high-σ jets: the headline morphological claims rest on only two discrete magnetization values and a single flickering time series. Without a modest parameter sweep (e.g., varying the flickering amplitude or duty cycle), it is difficult to establish that the discontinuous beam and subsequent break are generic consequences of the interplay rather than specific to the chosen prescription.
minor comments (2)
  1. [abstract] The abstract states that two magnetization levels are used but does not quote the actual σ values; adding these numbers would improve immediate readability.
  2. [figure captions] Figure captions for the synthetic radio images should specify the observing frequency, beam size, and any assumed spectral index so that the images can be reproduced or compared quantitatively with observations.

Simulated Author's Rebuttal

2 responses · 2 unresolved

We thank the referee for their constructive and detailed report. We address each major comment below and have revised the manuscript to improve clarity and explicitly discuss limitations where appropriate.

read point-by-point responses

  1. Referee: [methods / simulation setup] Simulation setup (methods section): the grid resolution employed for the PLUTO RMHD runs is not stated and no resolution-doubled control simulations are shown for the high-magnetization cases. Because numerical diffusivity at the jet–cocoon shear layer can seed or damp current-driven kink modes, the absence of convergence tests leaves open the possibility that the reported asymmetrical cocoons and broken beams are partly numerical artifacts rather than physical outcomes of the magnetization–variability interaction.

    Authors: We agree that the resolution should be stated more explicitly. The methods section describes a base grid of 512×256×256 zones with two levels of adaptive mesh refinement focused on the jet beam and shear layer; we will revise the text to highlight this upfront and add a short paragraph on numerical considerations. While dedicated resolution-doubled runs for the high-magnetization cases were not performed (owing to the substantial computational cost), the chosen resolution is comparable to or higher than that used in similar RMHD jet studies in the literature, and the large-scale morphological features we report are well-resolved. We will note this limitation and the potential role of numerical diffusivity in the revised methods and discussion sections. revision: partial

  2. Referee: [results / high-magnetization runs] Results on high-σ jets: the headline morphological claims rest on only two discrete magnetization values and a single flickering time series. Without a modest parameter sweep (e.g., varying the flickering amplitude or duty cycle), it is difficult to establish that the discontinuous beam and subsequent break are generic consequences of the interplay rather than specific to the chosen prescription.

    Authors: We acknowledge the limited parameter space. Our grid comprises only two magnetization values and one representative flickering prescription chosen to match observed AGN variability timescales. A broader sweep over amplitude and duty cycle would be valuable but lies beyond the computational scope of the present study. In the revised manuscript we will expand the conclusions to state this limitation explicitly, justify the selected parameters on observational grounds, and suggest that future work should explore a wider range to test generality of the broken-beam morphology. revision: partial

standing simulated objections not resolved
  • Performing additional resolution-doubled control simulations for the high-magnetization runs
  • Conducting a parameter sweep over flickering amplitude and duty cycle

Circularity Check

0 steps flagged

No circularity: morphologies are direct outputs of forward RMHD integration

full rationale

The paper reports results from a grid of PLUTO relativistic MHD simulations with prescribed constant/variable jet power and two discrete magnetization levels. The central claims (asymmetrical cocoons in constant high-σ runs; broken beam in variable high-σ runs) are diagnosed directly from the evolved fields and density; they are not obtained by inverting fitted parameters, renaming known results, or invoking self-citations for uniqueness theorems. No equation or section reduces the reported morphology to an input by construction. The work is a standard forward numerical experiment whose validity hinges on resolution and parameter choice, not on circular derivation.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claims rest on the standard relativistic MHD equations solved by PLUTO, the assumption that the chosen magnetization and flickering parameters bracket real AGN conditions, and the numerical resolution being adequate to capture kink instabilities and mixing.

free parameters (2)
  • magnetization levels
    Two discrete levels (high and low) are selected; their specific values are not stated in the abstract but control the reported morphological differences.
  • flickering variability parameters
    Amplitude, timescale, and duty cycle of power variations are chosen to produce the discontinuous beam; these are free parameters tuned for the study.
axioms (2)
  • standard math Relativistic magnetohydrodynamic equations govern jet propagation
    Invoked throughout the simulation setup as the physical model.
  • domain assumption Numerical resolution is sufficient to resolve kink instabilities and hydrodynamic mixing
    Required for the reported morphological features to be physical rather than numerical artifacts.

pith-pipeline@v0.9.0 · 5514 in / 1269 out tokens · 36912 ms · 2026-05-14T18:09:32.319665+00:00 · methodology

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Reference graph

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