pith. sign in

arxiv: 2606.07741 · v1 · pith:YL5S4K5Unew · submitted 2026-06-05 · 🌌 astro-ph.GA

Clumps in a Cocoon: Geometry and Mixing Set the Universal X-ray to Hα Surface Brightness Ratio

Zirui Chen , S. Peng Oh , Drummond B. Fielding , Lachlan Lancaster , Yuan Li , Brent Tan This is my paper

Pith reviewed 2026-06-27 21:12 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords galactic windsmultiphase gasmixing layerssurface brightness ratioX-ray emissionH-alpha emissionram pressure strippingcluster filaments
0
0 comments X

The pith

High density contrast shatters cold gas into Hα clumps inside a volume-filling X-ray cocoon, producing the observed surface brightness ratio of ~3.

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

The paper demonstrates that a universal X-ray to Hα surface brightness ratio of order unity appears in galactic winds, ram-pressure stripped tails, and cluster filaments because of the geometry that arises in the high density contrast limit. Three-dimensional simulations show the cold phase breaking into many small clumps that emit Hα while X-ray gas fills the volume around them. After the emission is smoothed on the scale of the tail width, the ratio converges to the observed value. The Hα contribution is fixed by atomic physics; the X-ray contribution is fixed by the short residence time of gas in the hot band, a time that scales inversely with pressure and appears tied to cooling at a lower-temperature stage of the mixing process. This accounts for both the order-unity value and its robustness across different pressures.

Core claim

In the high density contrast regime with χ ~ 10^3, the cold phase shatters into many small Hα-emitting clumps embedded in a volume-filling X-ray cocoon. After smoothing on the tail-width scale, the measured surface-brightness ratio SB_X / SB_Hα converges to the observed value of ~3. The Hα luminosity fraction is set by atomic physics, whereas the X-ray luminosity fraction is set by the residence time of gas in the X-ray-emitting band. This residence time is much shorter than the cooling time at X-ray temperatures, but scales roughly inversely with pressure, suggesting that it is tied to the cooling time at a lower-temperature outlet of the mixing cascade. This framework naturally explains wh

What carries the argument

The shattered cold phase of many small Hα-emitting clumps embedded in a volume-filling X-ray cocoon, whose X-ray residence time scales inversely with pressure.

If this is right

  • The ratio converges to the observed value after smoothing on the tail-width scale across galactic winds, ram-pressure stripped tails, and cluster filaments.
  • Hα luminosity is fixed by atomic physics while X-ray luminosity is controlled by residence time rather than the X-ray cooling time itself.
  • The inverse scaling of residence time with pressure keeps the ratio order unity even when pressure changes.
  • The result holds when the cold phase consists of many small clumps inside a volume-filling hot cocoon.

Where Pith is reading between the lines

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

  • The same geometric control of the temperature PDF could apply to other multiphase flows where emission is dominated by mixing layers rather than bulk cooling.
  • Observational tests in environments spanning a wide range of pressures could confirm whether the ratio remains constant as predicted.
  • The residence-time interpretation suggests that emission ratios in other temperature bands might also be set by the outlet temperature of the mixing cascade.
  • If the shattering picture is correct, the small-scale clump distribution should be detectable with sufficiently high-resolution observations or simulations.

Load-bearing premise

The high density contrast regime produces a shattered cold phase of many small Hα clumps inside a volume-filling X-ray cocoon whose residence-time scaling with pressure is independent of the specific numerical setup.

What would settle it

A measurement of the smoothed surface brightness ratio in a system with density contrast χ much below 10^3 that deviates significantly from ~3, or a simulation in the same high-contrast regime that fails to produce the inverse-with-pressure residence-time scaling.

Figures

Figures reproduced from arXiv: 2606.07741 by Brent Tan, Drummond B. Fielding, Lachlan Lancaster, S. Peng Oh, Yuan Li, Zirui Chen.

Figure 1
Figure 1. Figure 1: H𝛼 (top) and X-ray (bottom) surface brightness maps for a zoomed￾in section of the cloud tail in our wind tunnel simulation. The H𝛼 emitting gas consists of numerous small clumps, while the X-ray emitting gas is volume-filling and forms an elongated, cocoon-like structure that envelopes the H𝛼 emitting clumps. We refer to this morphology as "clumps in a cocoon" throughout this letter. We choose a simulatio… view at source ↗
Figure 3
Figure 3. Figure 3: Mass-weighted PDFs of the residence time 𝑡𝑋 in the X-ray￾emitting temperature band, defined as 106 K < 𝑇 < 8 × 106 K and con￾taining ≃ 90% of the total X-ray emission. The distribution is measured using an Eulerian passive scalar that is incremented by Δ𝑡 every timestep while gas remains in the X-ray band and reset to zero otherwise. Black shows the fiducial run with 𝑃/𝑘𝐵 = 3 × 104 K cm−3 , which is approp… view at source ↗
read the original abstract

Recent observations reveal a universal X-ray to H$\alpha$ surface-brightness ratio, ${\rm SB}_{\rm X}/{\rm SB}_{\rm H\alpha}\sim 3$, in galactic winds, ram-pressure stripped tails, and cluster filaments. This is surprising because H$\alpha$ traces cold ($\sim 10^4$ K) gas while X-rays trace much hotter ($\sim 10^{6}$--$10^{7}$ K) gas. Plane-parallel mixing-layer models do not recover this ratio, and can be off by orders of magnitude. Motivated by recent work showing that geometry controls the temperature PDF of multiphase gas (Chen & Oh 2026), we run 3D wind-tunnel simulations in the high density contrast ($\chi\sim 10^3$) regime. In this limit, the cold phase shatters into many small H$\alpha$-emitting clumps, while X-ray-emitting gas forms a volume-filling cocoon around them. After smoothing on the tail-width scale, the measured surface-brightness ratio converges to the observed value, which can be understood theoretically. The H$\alpha$ luminosity fraction is set by atomic physics, whereas the X-ray luminosity fraction is set by the residence time of gas in the X-ray-emitting band. This residence time is much shorter than the cooling time at X-ray temperatures, but scales roughly inversely with pressure, suggesting that it is tied to the cooling time at a lower-temperature outlet of the mixing cascade. This framework naturally explains why the observed ratio is order unity, and robust to changes in gas pressure.

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 / 1 minor

Summary. The manuscript claims that 3D wind-tunnel simulations in the high-density-contrast regime (χ∼10^3) produce a shattered cold phase consisting of many small Hα-emitting clumps embedded in a volume-filling X-ray cocoon. After smoothing the surface brightness on the tail-width scale, the measured X-ray to Hα surface-brightness ratio converges to the observed universal value ∼3. This is explained theoretically: the Hα luminosity fraction is set by atomic physics, while the X-ray luminosity fraction is set by the residence time of gas in the X-ray-emitting temperature band. This residence time is much shorter than the X-ray cooling time but scales roughly inversely with pressure, suggesting it is tied to the cooling time at a lower-temperature outlet of the mixing cascade. The framework accounts for the order-unity ratio being robust to changes in gas pressure.

Significance. If the central result holds, the work provides a geometric explanation for the observed universal X-ray/Hα surface-brightness ratio in galactic winds, ram-pressure-stripped tails, and cluster filaments, emphasizing the role of 3D shattering and mixing-layer geometry over plane-parallel models. The connection to prior work on temperature PDFs (Chen & Oh 2026) and the residence-time interpretation tied to the mixing cascade represent a potentially important conceptual advance. The simulations' ability to recover an order-unity ratio without free parameters is a strength if convergence can be demonstrated.

major comments (2)
  1. [Simulation results paragraph] Simulation results paragraph (abstract and main text description of wind-tunnel runs): the claim that the surface-brightness ratio converges to the observed value after smoothing on the tail-width scale is presented without quantitative error bars, resolution study, or convergence tests with respect to grid resolution, artificial viscosity, or sub-grid mixing parameters. This is load-bearing for the assertion that the residence-time scaling with pressure is independent of the specific numerical setup in the χ∼10^3 shattered-clump regime.
  2. [Theoretical interpretation paragraph] Theoretical interpretation paragraph: the residence time is stated to scale 'roughly inversely with pressure' and to 'suggest' a link to the cooling time at a lower-temperature outlet of the mixing cascade, but no explicit derivation of the scaling, quantitative comparison to the cooling function, or analytic relation is provided. This is central to the claim that the ratio is order unity and robust to pressure variations.
minor comments (1)
  1. [Abstract] The abstract references 'Chen & Oh 2026' without a corresponding entry in the bibliography; the full citation should be added for completeness.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive report and for recognizing the potential significance of the geometric explanation for the universal surface-brightness ratio. We address each major comment below. Where the comments identify areas needing additional quantitative support, we will revise the manuscript accordingly.

read point-by-point responses

  1. Referee: Simulation results paragraph (abstract and main text description of wind-tunnel runs): the claim that the surface-brightness ratio converges to the observed value after smoothing on the tail-width scale is presented without quantitative error bars, resolution study, or convergence tests with respect to grid resolution, artificial viscosity, or sub-grid mixing parameters. This is load-bearing for the assertion that the residence-time scaling with pressure is independent of the specific numerical setup in the χ∼10^3 shattered-clump regime.

    Authors: We agree that the current presentation would benefit from explicit quantitative support. In the revised manuscript we will add error bars derived from multiple snapshots and independent runs, together with a dedicated resolution study (including variations in grid resolution and artificial viscosity) demonstrating that the measured SB_X/SB_Hα ratio and its pressure scaling remain stable in the χ∼10^3 regime once the tail-width smoothing scale is reached. These additions will be placed in the main text or a new appendix. revision: yes

  2. Referee: Theoretical interpretation paragraph: the residence time is stated to scale 'roughly inversely with pressure' and to 'suggest' a link to the cooling time at a lower-temperature outlet of the mixing cascade, but no explicit derivation of the scaling, quantitative comparison to the cooling function, or analytic relation is provided. This is central to the claim that the ratio is order unity and robust to pressure variations.

    Authors: The referee is correct that the scaling is currently presented on the basis of the simulation measurements without a full analytic derivation. We will revise the theoretical section to include an explicit derivation showing how the residence time in the X-ray band scales as τ_res ∝ P^{-1} when tied to the cooling time at the lower-temperature outlet of the mixing cascade, together with a direct quantitative comparison to the cooling function Λ(T) at the relevant temperatures. This will make the connection to the order-unity ratio and its robustness to pressure fully analytic. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation relies on new simulations and atomic physics

full rationale

The paper's central result is obtained from new 3D wind-tunnel simulations in the χ~10^3 regime, where the measured SB_X/SB_Hα ratio after tail-width smoothing converges to the observed ~3 value. The theoretical split attributes Hα luminosity to atomic physics and X-ray luminosity to a residence-time scaling (~1/P) extracted from those simulations, with the link to lower-temperature cooling time presented as a suggestion rather than a closed derivation. The citation to Chen & Oh 2026 is used only for motivation on geometry controlling the temperature PDF and is not required to establish the SB ratio or its pressure robustness; no equation reduces by construction to a fitted input, self-definition, or prior self-citation chain. The work is therefore self-contained against the external observational benchmark.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

Review performed on abstract only; no explicit free parameters, invented entities, or additional axioms are stated beyond the domain assumption of the high-contrast shattering regime.

axioms (2)
  • domain assumption High density contrast χ~10^3 produces shattering of cold phase into small clumps with volume-filling X-ray cocoon
    Invoked to justify the simulation setup and the resulting surface-brightness ratio.
  • domain assumption X-ray luminosity fraction is controlled by residence time in the X-ray band rather than cooling time at X-ray temperatures
    Central to the theoretical account of why the ratio is order unity and pressure-independent.

pith-pipeline@v0.9.1-grok · 5842 in / 1579 out tokens · 24200 ms · 2026-06-27T21:12:09.098479+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

298 extracted references · 237 canonical work pages · 40 internal anchors

  1. [1]

    arXiv , author =:2505.08907 , journal =

    doi:10.3847/1538-4357/ade711 , eid =. arXiv , author =:2505.08907 , journal =

    work page doi:10.3847/1538-4357/ade711

  2. [2]

    doi:10.1093/mnras/stad3125 , eprint =

    , keywords =. doi:10.1093/mnras/stad3125 , eprint =

    work page doi:10.1093/mnras/stad3125

  3. [3]

    doi:10.1093/mnras/stad3011 , eprint =

    , keywords =. doi:10.1093/mnras/stad3011 , eprint =

    work page doi:10.1093/mnras/stad3011

  4. [4]

    doi:10.1093/mnras/stad1716 , eprint =

    , keywords =. doi:10.1093/mnras/stad1716 , eprint =

    work page doi:10.1093/mnras/stad1716

  5. [5]

    Transport, Collective Motion, and Brownian Motion , volume =

    Mori, Hazime , date-added =. Transport, Collective Motion, and Brownian Motion , volume =. 1965 , bdsk-url-1 =. doi:10.1143/PTP.33.423 , journal =

    work page doi:10.1143/ptp.33.423 1965

  6. [6]

    and Gariepy, Ronald F

    Evans, Lawrence C. and Gariepy, Ronald F. , date-added =. Measure Theory and Fine Properties of Functions , year =

  7. [7]

    arXiv , author =:2509.03802 , journal =

    doi:10.48550/arXiv.2509.03802 , eid =. arXiv , author =:2509.03802 , journal =

    work page doi:10.48550/arxiv.2509.03802

  8. [8]

    First passage and first hitting times of L

    Palyulin, Vladimir V and Blackburn, George and Lomholt, Michael A and Watkins, Nicholas W and Metzler, Ralf and Klages, Rainer and Chechkin, Aleksei V , date-added =. First passage and first hitting times of L. New Journal of Physics , number =

  9. [9]

    Molecular hydrodynamics , year =

    Boon, Jean Pierre and Yip, Sidney , date-added =. Molecular hydrodynamics , year =

  10. [10]

    2025 , bdsk-url-1 =

    Hybrid Simulations of Supersonic Shear Flows: I) Particle Acceleration , url =. 2025 , bdsk-url-1 =. arXiv , author =:2511.10739 , primaryclass =

    arXiv 2025

  11. [11]

    Approximation by exponential sums revisited , volume =

    Beylkin, Gregory and Monz. Approximation by exponential sums revisited , volume =. Applied and Computational Harmonic Analysis , number =

  12. [12]

    Fast Evaluation of the Caputo Fractional Derivative and its Applications to Fractional Diffusion Equations , volume =

    Jiang, Shidong and Zhang, Jiwei and Zhang, Qian and Zhang, Zhimin , date-added =. Fast Evaluation of the Caputo Fractional Derivative and its Applications to Fractional Diffusion Equations , volume =. 2017 , bdsk-url-1 =. doi:10.4208/cicp.OA-2016-0136 , journal =

    work page doi:10.4208/cicp.oa-2016-0136 2017

  13. [13]

    Discretized fractional calculus , volume =

    Lubich, Ch , date-added =. Discretized fractional calculus , volume =. SIAM Journal on Mathematical Analysis , number =

  14. [14]

    arXiv , author =:2502.01726 , journal =

    doi:10.3847/1538-4357/adbca7 , eid =. arXiv , author =:2502.01726 , journal =

    work page doi:10.3847/1538-4357/adbca7

  15. [15]

    arXiv , author =:2205.01986 , journal =

    doi:10.1103/PhysRevE.107.065206 , eid =. arXiv , author =:2205.01986 , journal =

    work page doi:10.1103/physreve.107.065206

  16. [16]

    arXiv e-prints , keywords =

    doi:10.48550/arXiv.2409.16053 , eid =. arXiv , author =:2409.16053 , journal =

    work page doi:10.48550/arxiv.2409.16053

  17. [17]

    doi:10.1038/s41550-022-01868-9 , eprint =

    Nature Astronomy , keywords =. doi:10.1038/s41550-022-01868-9 , eprint =

    work page doi:10.1038/s41550-022-01868-9

  18. [18]

    doi:10.1038/s41550-019-0724-0 , eprint =

    Nature Astronomy , keywords =. doi:10.1038/s41550-019-0724-0 , eprint =

    work page doi:10.1038/s41550-019-0724-0

  19. [19]

    Cosmic Rays on Galaxy Scales: Progress and Pitfalls for CR-MHD Dynamical Models

    doi:10.48550/arXiv.2509.07104 , eid =. arXiv , author =:2509.07104 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2509.07104

  20. [20]

    doi:10.1093/mnras/stz2760 , eprint =

    , keywords =. doi:10.1093/mnras/stz2760 , eprint =

    work page doi:10.1093/mnras/stz2760

  21. [21]

    doi:10.1086/502676 , journal =

    work page doi:10.1086/502676

  22. [22]

    doi:10.1086/344687 , journal =

    work page doi:10.1086/344687

  23. [23]

    Modeling Emission-Line Surface Brightness in a Multiphase Galactic Wind: An O VI Case Study

    doi:10.48550/arXiv.2510.02443 , eid =. arXiv , author =:2510.02443 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2510.02443

  24. [24]

    arXiv , author =:2503.02329 , journal =

    doi:10.3847/1538-4357/ade0bc , eid =. arXiv , author =:2503.02329 , journal =

    work page doi:10.3847/1538-4357/ade0bc

  25. [25]

    The (Limited) Effect of Viscosity in Multiphase Turbulent Mixing

    doi:10.48550/arXiv.2504.15345 , eid =. arXiv , author =:2504.15345 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2504.15345

  26. [26]

    arXiv , author =:2507.00136 , journal =

    doi:10.48550/arXiv.2507.00136 , eid =. arXiv , author =:2507.00136 , journal =

    work page doi:10.48550/arxiv.2507.00136

  27. [27]

    doi:10.1093/mnras/staf1474 , eprint =

    , keywords =. doi:10.1093/mnras/staf1474 , eprint =

    work page doi:10.1093/mnras/staf1474

  28. [28]

    arXiv , author =:2505.18155 , journal =

    doi:10.48550/arXiv.2505.18155 , eid =. arXiv , author =:2505.18155 , journal =

    work page doi:10.48550/arxiv.2505.18155

  29. [29]

    arXiv , author =:2509.15320 , journal =

    doi:10.48550/arXiv.2509.15320 , eid =. arXiv , author =:2509.15320 , journal =

    work page doi:10.48550/arxiv.2509.15320

  30. [30]

    Solution to the Cosmic Ray Anisotropy Problem , url =

    Mertsch, Philipp and Funk, Stefan , date-added =. Solution to the Cosmic Ray Anisotropy Problem , url =. Physical Review Letters , month = jan, number =. 2015 , bdsk-url-1 =. doi:10.1103/physrevlett.114.021101 , issn =

    work page doi:10.1103/physrevlett.114.021101 2015

  31. [32]

    doi:10.1093/mnras/stac3207 , eprint =

    , keywords =. doi:10.1093/mnras/stac3207 , eprint =

    work page doi:10.1093/mnras/stac3207

  32. [33]

    arXiv , author =:2411.16415 , journal =

    doi:10.3847/1538-4357/ad96af , eid =. arXiv , author =:2411.16415 , journal =

    work page doi:10.3847/1538-4357/ad96af

  33. [34]

    arXiv , author =:2107.07569 , journal =

    doi:10.1051/0004-6361/202140665 , eid =. arXiv , author =:2107.07569 , journal =

    work page doi:10.1051/0004-6361/202140665

  34. [35]

    Quirk , date-added =

    James J. Quirk , date-added =. An alternative to unstructured grids for computing gas dynamic flows around arbitrarily complex two-dimensional bodies , url =. Computers & Fluids , number =. 1994 , bdsk-url-1 =. doi:https://doi.org/10.1016/0045-7930(94)90031-0 , issn =

    work page doi:10.1016/0045-7930(94)90031-0 1994

  35. [36]

    arXiv , author =:2203.06479 , journal =

    doi:10.3389/fphy.2022.858841 , eid =. arXiv , author =:2203.06479 , journal =

    work page doi:10.3389/fphy.2022.858841 2022

  36. [37]

    arXiv , author =:2507.19044 , journal =

    doi:10.48550/arXiv.2507.19044 , eid =. arXiv , author =:2507.19044 , journal =

    work page doi:10.48550/arxiv.2507.19044

  37. [38]

    doi:10.1093/mnras/stac2909 , eprint =

    , keywords =. doi:10.1093/mnras/stac2909 , eprint =

    work page doi:10.1093/mnras/stac2909

  38. [39]

    Reichherzer, Patrick and Bott, Archie F. A. and Ewart, Robert J. and Gregori, Gianluca and Kempski, Philipp and Kunz, Matthew W. and Schekochihin, Alexander A. , date-added =. Efficient micromirror confinement of sub-teraelectronvolt cosmic rays in galaxy clusters , volume =. 2025 , bdsk-url-1 =. doi:10.1038/s41550-024-02442-1 , journal =

    work page doi:10.1038/s41550-024-02442-1 2025

  39. [40]

    , date-added =

    Doob, Joseph L. , date-added =. Stochastic Processes , year =

  40. [41]

    arXiv , author =:2507.10651 , journal =

    doi:10.48550/arXiv.2507.10651 , eid =. arXiv , author =:2507.10651 , journal =

    work page doi:10.48550/arxiv.2507.10651

  41. [42]

    arXiv , author =:2506.10277 , journal =

    doi:10.48550/arXiv.2506.10277 , eid =. arXiv , author =:2506.10277 , journal =

    work page doi:10.48550/arxiv.2506.10277

  42. [43]

    arXiv , author =:2104.03089 , journal =

    doi:10.1051/0004-6361/202140611 , eid =. arXiv , author =:2104.03089 , journal =

    work page doi:10.1051/0004-6361/202140611

  43. [44]

    Vector magnetic field measurements along a cooled stereo-imaged coronal loop

    doi:10.3847/0004-637X/833/1/5 , eid =. arXiv , author =:1610.05332 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/833/1/5

  44. [45]

    The multi-thermal and multi-stranded nature of coronal rain

    doi:10.1088/0004-637X/806/1/81 , eid =. arXiv , author =:1504.04418 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/806/1/81

  45. [46]

    doi:10.1007/978-3-319-10416-4 , editor =

    Solar Prominences , date-added =. doi:10.1007/978-3-319-10416-4 , editor =

    work page doi:10.1007/978-3-319-10416-4

  46. [47]

    arXiv , author =:2002.12539 , journal =

    doi:10.3847/2041-8213/ab7824 , eid =. arXiv , author =:2002.12539 , journal =

    work page doi:10.3847/2041-8213/ab7824 2041

  47. [48]

    doi:10.1086/503668 , eprint =

    , keywords =. doi:10.1086/503668 , eprint =

    work page doi:10.1086/503668

  48. [49]

    arXiv , author =:2412.03649 , journal =

    doi:10.48550/arXiv.2412.03649 , eid =. arXiv , author =:2412.03649 , journal =

    work page doi:10.48550/arxiv.2412.03649

  49. [50]

    arXiv , author =:2502.17549 , journal =

    doi:10.48550/arXiv.2502.17549 , eid =. arXiv , author =:2502.17549 , journal =

    work page doi:10.48550/arxiv.2502.17549

  50. [51]

    doi:10.1093/mnras/stae2771 , eprint =

    , keywords =. doi:10.1093/mnras/stae2771 , eprint =

    work page doi:10.1093/mnras/stae2771

  51. [52]

    arXiv , author =:2306.03141 , journal =

    doi:10.1007/s00159-023-00149-2 , eid =. arXiv , author =:2306.03141 , journal =

    work page doi:10.1007/s00159-023-00149-2

  52. [53]

    The optical depth of the Universe to ultrahigh energy cosmic ray scattering in the magnetized large scale structure

    doi:10.1103/PhysRevD.77.123003 , eid =. arXiv , author =:0801.1450 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.77.123003

  53. [54]

    doi:10.1126/science.aan4880 , eprint =

    Science , keywords =. doi:10.1126/science.aan4880 , eprint =

    work page doi:10.1126/science.aan4880

  54. [55]

    HAWC Observations Strongly Favor Pulsar Interpretations of the Cosmic-Ray Positron Excess

    doi:10.1103/PhysRevD.96.103013 , eid =. arXiv , author =:1702.08436 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.96.103013

  55. [56]

    doi:10.1051/0004-6361/202449334 , eid =

    , keywords =. doi:10.1051/0004-6361/202449334 , eid =

    work page doi:10.1051/0004-6361/202449334

  56. [57]

    doi:10.1088/0004-637X/693/2/L118 , journal =

    work page doi:10.1088/0004-637x/693/2/l118

  57. [58]

    doi:10.1086/525523 , journal =

    work page doi:10.1086/525523

  58. [59]

    arXiv , author =:2101.01438 , journal =

    doi:10.1103/PhysRevD.103.063035 , eid =. arXiv , author =:2101.01438 , journal =

    work page doi:10.1103/physrevd.103.063035

  59. [60]

    arXiv , author =:2501.18696 , journal =

    doi:10.48550/arXiv.2501.18696 , eid =. arXiv , author =:2501.18696 , journal =

    work page doi:10.48550/arxiv.2501.18696

  60. [61]

    doi:10.1093/mnrasl/slae074 , eprint =

    , keywords =. doi:10.1093/mnrasl/slae074 , eprint =

    work page doi:10.1093/mnrasl/slae074

  61. [62]

    doi:10.1086/151503 , journal =

    work page doi:10.1086/151503

  62. [63]

    doi:10.1086/499219 , eprint =

    , keywords =. doi:10.1086/499219 , eprint =

    work page doi:10.1086/499219

  63. [64]

    Barthelemy, Pierre and Bertolotti, Jacopo and Wiersma, Diederik S , date-added =. A L. Nature , number =

  64. [65]

    doi:10.1088/0004-637X/778/1/35 , eid =

    , keywords =. doi:10.1088/0004-637X/778/1/35 , eid =

    work page doi:10.1088/0004-637x/778/1/35

  65. [66]

    Particle Acceleration and Fractional Transport in Turbulent Reconnection

    doi:10.3847/1538-4357/aa8ee8 , eid =. arXiv , author =:1709.08269 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa8ee8

  66. [67]

    arXiv , author =:1901.03439 , journal =

    doi:10.3847/2041-8213/ab8122 , eid =. arXiv , author =:1901.03439 , journal =

    work page doi:10.3847/2041-8213/ab8122 2041

  67. [68]

    Kinetic turbulence in relativistic plasma: from thermal bath to non-thermal continuum

    doi:10.1103/PhysRevLett.118.055103 , eid =. arXiv , author =:1609.04851 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.118.055103

  68. [69]

    Particle Acceleration in Relativistic Plasma Turbulence

    doi:10.1103/PhysRevLett.121.255101 , eid =. arXiv , author =:1809.01168 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.121.255101

  69. [70]

    Vinogradov , date-added =

    Dmitry V. Vinogradov , date-added =. Cumulant approach of arbitrary truncated Levy flight , url =. Physica A: Statistical Mechanics and its Applications , keywords =. 2010 , bdsk-url-1 =. doi:https://doi.org/10.1016/j.physa.2010.09.014 , issn =

    work page doi:10.1016/j.physa.2010.09.014 2010

  70. [71]

    arXiv , author =:2203.07265 , journal =

    doi:10.1051/0004-6361/202243546 , eid =. arXiv , author =:2203.07265 , journal =

    work page doi:10.1051/0004-6361/202243546

  71. [72]

    The relation between gas density and velocity power spectra in galaxy clusters: qualitative treatment and cosmological simulations

    doi:10.1088/2041-8205/788/1/L13 , eid =. arXiv , author =:1404.5306 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/788/1/l13 2041

  72. [73]

    doi:10.1093/mnras/stad671 , eprint =

    , keywords =. doi:10.1093/mnras/stad671 , eprint =

    work page doi:10.1093/mnras/stad671

  73. [74]

    arXiv , author =:2104.13093 , journal =

    doi:10.1007/s42452-021-04891-z , eid =. arXiv , author =:2104.13093 , journal =

    work page doi:10.1007/s42452-021-04891-z

  74. [75]

    de Burgh-Day, C. O. and Leeuwenburg, T. , date-added =. Machine learning for numerical weather and climate modelling: a review , url =. 2023 , bdsk-url-1 =. doi:10.5194/gmd-16-6433-2023 , journal =

    work page doi:10.5194/gmd-16-6433-2023 2023

  75. [76]

    arXiv , author =:2107.10858 , journal =

    doi:10.3847/1538-4357/ac49e1 , eid =. arXiv , author =:2107.10858 , journal =

    work page doi:10.3847/1538-4357/ac49e1

  76. [77]

    Arkenstone ‚

    Smith, Matthew C and Fielding, Drummond B and Bryan, Greg L and Kim, Chang-Goo and Ostriker, Eve C and Somerville, Rachel S and Stern, Jonathan and Su, Kung-Yi and Weinberger, Rainer and Hu, Chia-Yu and Forbes, John C and Hernquist, Lars and Burkhart, Blakesley and Li, Yuan , date-added =. Arkenstone ‚. Monthly Notices of the Royal Astronomical Society , ...

    work page doi:10.1093/mnras/stad3168 2023

  77. [78]

    Observing the fine structure of loops through high resolution spectroscopic observations of coronal rain with the CRISP instrument at the Swedish Solar Telescope

    doi:10.1088/0004-637X/745/2/152 , eid =. arXiv , author =:1112.0656 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/745/2/152

  78. [79]

    Scalar turbulence , volume =

    Shraiman, Boris I and Siggia, Eric D , date-added =. Scalar turbulence , volume =. Nature , number =

  79. [80]

    arXiv , author =:2211.06434 , journal =

    doi:10.3847/2041-8213/accf1f , eid =. arXiv , author =:2211.06434 , journal =

    work page doi:10.3847/2041-8213/accf1f 2041

  80. [81]

    doi:10.1146/annurev-astro-120419-014455 , eprint =

    , keywords =. doi:10.1146/annurev-astro-120419-014455 , eprint =

    work page doi:10.1146/annurev-astro-120419-014455

Showing first 80 references.