pith. sign in

arxiv: 2606.07733 · v1 · pith:VPBG4N3Anew · submitted 2026-06-05 · 🌌 astro-ph.HE · astro-ph.GA

The Effects of Cosmic Ray Protons on Galactic Nonthermal Filaments

Mohan Richter-Addo , Roark Habegger , Ellen Zweibel , Dylan M. Par\'e , David T. Chuss This is my paper

Pith reviewed 2026-06-27 20:49 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.GA
keywords nonthermal filamentsgalactic centercosmic ray protonscosmic ray leptonsMHD simulationssynchrotron emissionturbulence
0
0 comments X

The pith

Cosmic ray proton and lepton simulations produce similar nonthermal filament properties, motivating a turbulence origin for galactic center filaments.

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

The paper aims to distinguish whether nonthermal filaments in the Galactic Center are powered by lepton-dominated jets from pulsar wind nebulae or proton-dominated particles from interstellar shocks. Using modified MHD simulations that include cosmic ray losses for both species, the authors vary magnetic field, density, and diffusion parameters to model propagation and emission. They find few observable differences between the two cases in terms of heating, flow, and synchrotron emission. This result leads them to suggest that the filaments may instead be generated by intermittent structures in Galactic Center turbulence. Readers would care because clarifying the origin affects models of cosmic ray acceleration and energy transport in the dense galactic center environment.

Core claim

Simulations of cosmic ray propagation in nonthermal filaments using an MHD code modified for radiative and collisional losses show few observable differences between proton-dominated and lepton-dominated cases across varied parameters of magnetic field strength, plasma density, and diffusion coefficient. Comparing these models to observed filament properties motivates consideration of a third formation mechanism in which NTFs arise from intermittent structures in Galactic Center turbulence.

What carries the argument

Modified Athena++ MHD code that accounts for radiative and collisional losses in the propagation of lepton and proton cosmic ray species.

If this is right

  • Varying magnetic field strength, plasma density, and CR diffusion coefficient produces similar effects on CR propagation, heating, plasma flow, and observed synchrotron emission for both proton and lepton cases.
  • Observed properties of filaments do not provide clear distinction between the two proposed injection mechanisms.
  • The similarity motivates considering generation of NTFs from intermittent structures in Galactic Center turbulence as an alternative.

Where Pith is reading between the lines

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

  • Filament brightness or length might correlate with local turbulence statistics rather than proximity to pulsars or shocks.
  • High-resolution mapping of filament variability could test for intermittent turbulence signatures.
  • CR acceleration in the GC may be more widespread and less tied to specific sources if turbulence dominates.

Load-bearing premise

The chosen ranges of magnetic field strength, plasma density, and CR diffusion coefficient, together with the implemented radiative and collisional loss terms, are representative of actual conditions inside the observed nonthermal filaments and sufficient to produce distinguishable signatures if one injection mechanism dominates.

What would settle it

High-resolution observations revealing systematic differences in synchrotron spectra or spatial distributions between filaments near pulsars and those near shocks that match one simulation model distinctly over the other would challenge the finding of few observable differences.

Figures

Figures reproduced from arXiv: 2606.07733 by David T. Chuss, Dylan M. Par\'e, Ellen Zweibel, Mohan Richter-Addo, Roark Habegger.

Figure 1
Figure 1. Figure 1: A one square degree image of a portion of the Galactic Plane showing multiple NTFs taken at 1.28 GHz with the MeerKAT telescope, data from I. Heywood et al. (2022). trend of steepening spectral index in filaments at higher Galactic latitude (F. Yusef-Zadeh et al. 2022c; D. M. Par´e et al. 2022). Our study aims to test and differentiate between two particular origin theories: either 1) they are fueled by je… view at source ↗
Figure 2
Figure 2. Figure 2: Illustration of the loss timescales of CRe± through various processes as a function of the particle’s γ. The blue line is the synchrotron timescale, the green line is the bremsstrahlung timescale, the red line is the inverse Compton timescale, and the orange line is the Coulomb timescale. The solid black line is the total loss timescale due to these combined processes. Both the top and right axes assume a … view at source ↗
Figure 3
Figure 3. Figure 3: Time evolution of the CR energy density in a 1D flux tube with κ = 1026 cm2 s −1 , B = 200 µG, and ne = 100 cm−3 , in the case of a proton injection. We see a strong peak persist at the injection site for the duration of the injection which then diffuses and streams outward to overall double the background CR energy density at around 10kyr. Dotted contours trace lines of constant energy den￾sity, and are p… view at source ↗
Figure 4
Figure 4. Figure 4: Plots at t = 40 kyr of the energy density (top row) and normalized luminosity per length (bottom row) within these lepton-only simulations. Left column, simulations “kvar[n]”: When changing the diffusion coefficient, the Gaussian wings get larger while the streaming length stays the same. Middle column, simulations “nvar[n]”: When changing the number density, the streaming length changes (as well as increa… view at source ↗
Figure 5
Figure 5. Figure 5: Plots at t = 40 kyr of the induced velocities and heating cause by streaming in the same simulations as [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Lepton-only energy profiles of special cases to illustrate the synergistic effects of non-adiabatic losses, sec￾ondary production, and protons. Case 1 replots the fiducial model of “original-lowdiff”, Case 2 replots the high density model of “nvar5,” Case 3 plots a modified “nvar5” model that now includes secondary production, and Case 4 plots a modified ’‘nvar5” model while now neglecting non-adiabatic lo… view at source ↗
Figure 8
Figure 8. Figure 8: Phase space of diffusion vs streaming domina￾tion given specific B and ne values. Colored lines represent contours where diffusion and streaming have equal contri￾butions: above these lines, diffusion dominates; below these lines, streaming dominates. These lines all follow the ana￾lytic form vA = κ/l. The colored dot indicates our specific (B, ne) parameters for our simulation (which roughly corre￾sponds … view at source ↗
Figure 9
Figure 9. Figure 9: Modeled spectral index due to energy-dependent diffusion at different ages with κ = 1026 cm2 s −1 at this en￾ergy band. Here, we set the original power law spectrum to be p = 2.5 and the energy-dependent diffusion index to be q = 0.2 in order to get an equilibrium population index that matches 2.6, the power law index we assumed without energy-dependent diffusion. cle’s time-dependent energy γ(t) and its o… view at source ↗
Figure 10
Figure 10. Figure 10: Plotted are cosmic ray distribution functions as a function of energy at different ages. Only synchrotron losses are assumed in these predictions. In the bottom plot, the CR synchrotron spectral index is plotted as a function of time between the VLA C– and X–bands that cover 4–8 GHz (blue region) and 8–12 GHz (pink region) respectively. The vertical asymptote shown is the time when there are no more parti… view at source ↗
Figure 11
Figure 11. Figure 11: Plots of the velocity and pressure 10 kyr after a lepton-only injection, zoomed in on the center pc of the simulated filament. When not varying a specific parameter, these convergence tests were run with a resolution of dx = 1/64 pc, a CFL number of 0.2, a spatial order of 3, and using the RK integrator “rk4.” For the complete suite of simulations, we set dx = 1/64 pc in order to minimize the jagged veloc… view at source ↗
read the original abstract

The Galactic Center (GC) contains a collection of filaments that are typically tens of parsecs in length, illuminated by synchrotron radiation from cosmic rays (CR). The origin of these nonthermal filaments (NTFs) is unclear. We aim to distinguish two injection mechanisms: the first mechanism posits that NTFs are fueled either by jets from pulsar wind nebulae and are lepton-dominated; the second mechanism posits that NTFs are fueled by accelerated particles from interstellar shocks and are proton-dominated. We explore these mechanisms using the magnetohydrodynamics (MHD) code Athena++, modified to account for radiative and collisional losses, to simulate CR propagation with lepton and proton CR species. We vary parameters such as magnetic field strength, plasma density, and the CR diffusion coefficient to determine how the range of conditions present in the GC can affect CRs' propagation, heating, plasma flow, and the observed synchrotron emission. We find few observable differences between the proton- and lepton-dominated cases, but comparing the models with observed filament properties motivates consideration of a third formation mechanism: the generation of NTFs arise from intermittent structures in Galactic Center turbulence.

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 uses modified Athena++ MHD simulations to model cosmic ray (CR) propagation in Galactic Center nonthermal filaments (NTFs), comparing lepton-dominated (pulsar wind nebulae) and proton-dominated (interstellar shocks) injection by varying magnetic field strength, plasma density, and CR diffusion coefficient while including radiative and collisional losses. It reports few observable differences between the cases in CR propagation, heating, plasma flow, and synchrotron emission, and uses this plus a qualitative match to observations to motivate a third mechanism: NTFs arising from intermittent structures in GC turbulence.

Significance. A robust null result showing indistinguishable observables between the two CR species would help constrain NTF origins. The work is credited for implementing both CR species with loss terms in MHD runs. However, without quantitative metrics or a turbulence simulation, the significance for motivating a third mechanism remains limited.

major comments (2)
  1. [Abstract] Abstract: the central claim of 'few observable differences' between proton- and lepton-dominated cases supplies no quantitative metrics, error estimates, difference tables, or direct comparison to observed filament properties, preventing evaluation of whether the null result is robust or sensitive to the chosen parameter ranges.
  2. [Abstract] Abstract: the step from the two simulated mechanisms producing similar outputs to motivating an un-simulated third mechanism (intermittent GC turbulence structures) is not load-bearing tested; no metric shows observed properties lie outside the envelope of both runs, and no turbulence realization is performed for comparison.
minor comments (1)
  1. The abstract would be strengthened by stating the specific ranges explored for B, n, and D_CR and by noting any direct quantitative matches or mismatches to observed NTF lengths, widths, or brightnesses.

Simulated Author's Rebuttal

2 responses · 1 unresolved

We thank the referee for their constructive comments on our manuscript. We address each major comment below and indicate where revisions will be made to strengthen the presentation.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central claim of 'few observable differences' between proton- and lepton-dominated cases supplies no quantitative metrics, error estimates, difference tables, or direct comparison to observed filament properties, preventing evaluation of whether the null result is robust or sensitive to the chosen parameter ranges.

    Authors: We agree that quantitative support for the 'few observable differences' claim would improve the manuscript. In the revised version we will add a table summarizing percentage differences in CR energy density, plasma heating rate, flow velocity, and synchrotron surface brightness between the proton- and lepton-dominated runs across the explored parameter space. We will also include direct numerical comparisons of these quantities to published radio and X-ray properties of observed NTFs (e.g., from MeerKAT and Chandra data) to allow readers to assess robustness. revision: yes

  2. Referee: [Abstract] Abstract: the step from the two simulated mechanisms producing similar outputs to motivating an un-simulated third mechanism (intermittent GC turbulence structures) is not load-bearing tested; no metric shows observed properties lie outside the envelope of both runs, and no turbulence realization is performed for comparison.

    Authors: The manuscript presents the turbulence scenario as a motivated hypothesis rather than a quantitatively tested conclusion, based on the similarity of the two injection models and their qualitative consistency with observed filament properties. We will revise the abstract and discussion to make this distinction explicit and to state that a dedicated turbulence simulation lies outside the present scope. No metric demonstrating that observations fall outside the simulated envelope is currently available, and we do not claim one. revision: partial

standing simulated objections not resolved
  • A full MHD simulation of intermittent turbulence structures in the Galactic Center, with direct comparison to the two injection scenarios, cannot be performed within the current study.

Circularity Check

0 steps flagged

No circularity: simulations report direct outputs and qualitative comparison

full rationale

The paper runs Athena++ MHD simulations for lepton- versus proton-dominated CR injection, varies B, density, and diffusion coefficient as free inputs, and reports resulting differences in propagation, heating, flow, and synchrotron emission. The claim of few observable differences and the motivation for a third (turbulence) mechanism follows from those simulation outputs plus external observational properties; no equation reduces a reported quantity to a parameter fitted from the same data, no self-citation supplies a uniqueness theorem, and no ansatz is smuggled in. The derivation chain is therefore self-contained against the stated simulation setup.

Axiom & Free-Parameter Ledger

3 free parameters · 2 axioms · 0 invented entities

The central claim rests on the assumption that the chosen parameter ranges and loss physics are representative of the Galactic Center and that the Athena++ modifications correctly capture proton versus lepton propagation differences. No new particles or forces are introduced.

free parameters (3)
  • magnetic field strength
    Varied across GC-relevant values to test propagation and emission; not fitted to filament data but chosen as input.
  • plasma density
    Varied across GC-relevant values to test propagation and emission; not fitted to filament data but chosen as input.
  • CR diffusion coefficient
    Varied across GC-relevant values to test propagation and emission; not fitted to filament data but chosen as input.
axioms (2)
  • domain assumption Standard ideal MHD equations plus added radiative and collisional loss terms for CR species accurately describe filament evolution.
    Invoked by the choice to modify Athena++ and run the described parameter survey.
  • domain assumption Synchrotron emission, heating, and plasma flow are the primary observables that would distinguish proton- versus lepton-dominated injection.
    Implicit in the statement that few observable differences were found.

pith-pipeline@v0.9.1-grok · 5748 in / 1565 out tokens · 16825 ms · 2026-06-27T20:49:00.264270+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

60 extracted references · 52 canonical work pages · 19 internal anchors

  1. [1]

    , keywords =

    The Source of the Relativistic Particles in the Galactic Center Arc. , keywords =. doi:10.1086/187282 , adsurl =

    work page doi:10.1086/187282

  2. [2]

    Interactions of Cosmic Ray Nuclei

    Interactions of cosmic ray nuclei. , keywords =. doi:10.48550/arXiv.astro-ph/9402042 , archivePrefix =. astro-ph/9402042 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9402042

  3. [3]

    Radiative Processes in Astrophysics

  4. [4]

    Radio Halos of Galaxy Clusters from Hadronic Secondary Electron Injection in Realistic Magnetic Field Configurations

    Radio halos of galaxy clusters from hadronic secondary electron injection in realistic magnetic field configurations. , keywords =. doi:10.48550/arXiv.astro-ph/0008333 , archivePrefix =. astro-ph/0008333 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0008333

  5. [5]

    arXiv , author =:1912.08491 , journal =

    Probing Cosmic-Ray Transport with Radio Synchrotron Harps in the Galactic Center. , keywords =. doi:10.3847/2041-8213/ab7237 , archivePrefix =. 1912.08491 , primaryClass =

    work page doi:10.3847/2041-8213/ab7237 2041

  6. [6]

    New Journal of Physics , year = 2013, month = jan, volume =

    On the Galactic Center being the main source of galactic cosmic rays as evidenced by recent cosmic ray and gamma ray observations. New Journal of Physics , year = 2013, month = jan, volume =. doi:10.1088/1367-2630/15/1/013053 , adsurl =

    work page doi:10.1088/1367-2630/15/1/013053 2013

  7. [7]

    , keywords =

    The Impact of Cosmic Ray Injection on Magnetic Flux Tubes in a Galactic Disk. , keywords =. doi:10.3847/1538-4357/accf8e , archivePrefix =. 2211.04503 , primaryClass =

    work page doi:10.3847/1538-4357/accf8e

  8. [8]

    A New Numerical Scheme for Cosmic Ray Transport

    A New Numerical Scheme for Cosmic-Ray Transport. , keywords =. doi:10.3847/1538-4357/aaa6ce , archivePrefix =. 1712.07117 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aaa6ce

  9. [9]

    The Cosmic Ray Population of the Galactic Central Molecular Zone

    The Cosmic-Ray Population of the Galactic Central Molecular Zone. , keywords =. doi:10.1088/0004-637X/790/2/86 , archivePrefix =. 1405.7059 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/790/2/86

  10. [10]

    , keywords =

    A Very Large Array Study of Newly Discovered Southern Latitude Nonthermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties. , keywords =. doi:10.3847/1538-4357/aca40a , archivePrefix =. 2209.08153 , primaryClass =

    work page doi:10.3847/1538-4357/aca40a

  11. [11]

    Cosmic Ray Astrophysics

  12. [12]

    M., Tomida, K., White, C

    The Athena++ Adaptive Mesh Refinement Framework: Design and Magnetohydrodynamic Solvers. , keywords =. doi:10.3847/1538-4365/ab929b , archivePrefix =. 2005.06651 , primaryClass =

    work page doi:10.3847/1538-4365/ab929b 2005

  13. [13]

    Computing in Science and Engineering , keywords =

    Matplotlib: A 2D Graphics Environment. Computing in Science and Engineering , keywords =. doi:10.1109/MCSE.2007.55 , adsurl =

    work page doi:10.1109/mcse.2007.55 2007

  14. [14]

    The NumPy array: a structure for efficient numerical computation

    The NumPy Array: A Structure for Efficient Numerical Computation. Computing in Science and Engineering , keywords =. doi:10.1109/MCSE.2011.37 , archivePrefix =. 1102.1523 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1109/mcse.2011.37 2011

  15. [15]

    Array Programming with NumPy

    Array programming with NumPy. , keywords =. doi:10.1038/s41586-020-2649-2 , archivePrefix =. 2006.10256 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41586-020-2649-2 2006

  16. [16]

    Astropy: A Community Python Package for Astronomy

    Astropy: A community Python package for astronomy. , keywords =. doi:10.1051/0004-6361/201322068 , archivePrefix =. 1307.6212 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322068

  17. [17]

    The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

    The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. , keywords =. doi:10.3847/1538-3881/aabc4f , archivePrefix =. 1801.02634 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aabc4f

  18. [18]

    High Energy Radiation from Black Holes: Gamma Rays, Cosmic Rays, and Neutrinos

  19. [19]

    A Wide-area VLA Continuum Survey near the Galactic Center at 6 and 20 cm Wavelengths

    A Wide-Area VLA Continuum Survey near the Galactic Center at 6 and 20 cm Wavelengths. , keywords =. doi:10.1086/588218 , archivePrefix =. 0803.1412 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/588218

  20. [20]

    , keywords =

    Statistical Properties of the Population of the Galactic Center Filaments: the Spectral Index and Equipartition Magnetic Field. , keywords =. doi:10.3847/2041-8213/ac4802 , archivePrefix =. 2201.10552 , primaryClass =

    work page doi:10.3847/2041-8213/ac4802 2041

  21. [21]

    Cosmic Rays below Z=30 in a diffusion model: new constraints on propagation parameters

    Cosmic Rays below Z=30 in a Diffusion Model: New Constraints on Propagation Parameters. , keywords =. doi:10.1086/321496 , archivePrefix =. astro-ph/0101231 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/321496

  22. [22]

    Turbulent Origin of the Galactic-Center Magnetic Field: Nonthermal Radio Filaments

    Turbulent Origin of the Galactic Center Magnetic Field: Nonthermal Radio Filaments. , keywords =. doi:10.1086/500411 , archivePrefix =. astro-ph/0512373 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/500411

  23. [23]

    , keywords =

    Large, highly organized radio structures near the galactic centre. , keywords =. doi:10.1038/310557a0 , adsurl =

    work page doi:10.1038/310557a0

  24. [24]

    , keywords =

    The 1.28 GHz MeerKAT Galactic Center Mosaic. , keywords =. doi:10.3847/1538-4357/ac449a , archivePrefix =. 2201.10541 , primaryClass =

    work page doi:10.3847/1538-4357/ac449a

  25. [25]

    , keywords =

    A novel analytical model of the magnetic field configuration in the Galactic center. , keywords =. doi:10.1051/0004-6361/201936081 , archivePrefix =. 1906.05211 , primaryClass =

    work page doi:10.1051/0004-6361/201936081 1906

  26. [26]

    , keywords =

    Cosmic-Ray Feedback on Bistable Interstellar Medium Turbulence. , keywords =. doi:10.3847/1538-4357/ad67da , archivePrefix =. 2403.07976 , primaryClass =

    work page doi:10.3847/1538-4357/ad67da

  27. [27]

    Malicious User Experience Design Research for Cybersecurity

    Theory of Star Formation. , keywords =. doi:10.1146/annurev.astro.45.051806.110602 , archivePrefix =. 0707.3514 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev.astro.45.051806.110602

  28. [28]

    , keywords =

    Unusual threads of radio emission near the Galactic Center. , keywords =. doi:10.1086/113955 , adsurl =

    work page doi:10.1086/113955

  29. [29]

    , keywords =

    A New System of Nonthermal Filaments near the Galactic Center. , keywords =. doi:10.1086/167003 , adsurl =

    work page doi:10.1086/167003

  30. [30]

    , keywords =

    Inflation of 430-parsec bipolar radio bubbles in the Galactic Centre by an energetic event. , keywords =. doi:10.1038/s41586-019-1532-5 , archivePrefix =. 1909.05534 , primaryClass =

    work page doi:10.1038/s41586-019-1532-5 1909

  31. [31]

    , keywords =

    Origin of the new axisymmetric radio sources. , keywords =. doi:10.1038/313118a0 , adsurl =

    work page doi:10.1038/313118a0

  32. [32]

    First Course in Turbulence

  33. [33]

    , keywords =

    Tearing-mediated Alfv \'e nic Turbulence in a Relativistic Plasma. , keywords =. doi:10.3847/1538-4357/ada28a , adsurl =

    work page doi:10.3847/1538-4357/ada28a

  34. [34]

    , keywords =

    Magnetogenesis in a Collisionless Plasma: From Weibel Instability to Turbulent Dynamo. , keywords =. doi:10.3847/1538-4357/ad0b0f , archivePrefix =. 2308.01924 , primaryClass =

    work page doi:10.3847/1538-4357/ad0b0f

  35. [35]

    As a matter of force - Systematic biases in idealized turbulence simulations

    As a Matter of Force Systematic Biases in Idealized Turbulence Simulations. , keywords =. doi:10.3847/2041-8213/aac0f5 , archivePrefix =. 1803.05481 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aac0f5 2041

  36. [36]

    , keywords =

    Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds. , keywords =. doi:10.3847/1538-4357/ad8631 , archivePrefix =. 2410.09258 , primaryClass =

    work page doi:10.3847/1538-4357/ad8631

  37. [37]

    , keywords =

    Reduced MHD in Astrophysical Applications: Two-dimensional or Three-dimensional?. , keywords =. doi:10.3847/1538-4357/aa67e2 , adsurl =

    work page doi:10.3847/1538-4357/aa67e2

  38. [38]

    Field lines twisting in a noisy corona: implications for energy storage and release, and initiation of solar eruptions

    Field Lines Twisting in a Noisy Corona: Implications for Energy Storage and Release, and Initiation of Solar Eruptions. , keywords =. doi:10.1088/0004-637X/771/2/76 , archivePrefix =. 1301.7678 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/771/2/76

  39. [39]

    , keywords =

    Coronal heating by phase-mixed shear Alfven waves. , keywords =

  40. [40]

    Physics of Plasmas , keywords =

    Formation and evolution of coherent structures in 3D strongly turbulent magnetized plasmas. Physics of Plasmas , keywords =. doi:10.1063/5.0141512 , archivePrefix =. 2303.15351 , primaryClass =

    work page doi:10.1063/5.0141512

  41. [41]

    arXiv e-prints , keywords =

    The stable ``Unstable Natural Media'' due to the presence of turbulence. arXiv e-prints , keywords =. doi:10.48550/arXiv.2407.14199 , archivePrefix =. 2407.14199 , primaryClass =

    work page doi:10.48550/arxiv.2407.14199

  42. [42]

    Influence of a large-scale field on energy dissipation in magnetohydrodynamic turbulence

    Influence of a large-scale field on energy dissipation in magnetohydrodynamic turbulence. , keywords =. doi:10.1093/mnras/stx611 , archivePrefix =. 1703.03433 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx611

  43. [43]

    , keywords =

    Impact of Anisotropic Cosmic-Ray Transport on the Gamma-Ray Signatures in the Galactic Center. , keywords =. doi:10.3847/1538-4357/ad2ea1 , archivePrefix =. 2312.15206 , primaryClass =

    work page doi:10.3847/1538-4357/ad2ea1

  44. [44]

    A 100-parsec elliptical and twisted ring of cold and dense molecular clouds revealed by Herschel around the Galactic Center

    A 100 pc Elliptical and Twisted Ring of Cold and Dense Molecular Clouds Revealed by Herschel Around the Galactic Center. , keywords =. doi:10.1088/2041-8205/735/2/L33 , archivePrefix =. 1105.5486 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/735/2/l33 2041

  45. [45]

    The spacing between filaments

    Statistical properties of the population of the Galactic centre filaments - II. The spacing between filaments. , keywords =. doi:10.1093/mnras/stac1696 , archivePrefix =. 2206.10732 , primaryClass =

    work page doi:10.1093/mnras/stac1696

  46. [46]

    SOFIA/HAWC+ Far-Infrared Polarimetric Large Area CMZ Exploration Survey. V. The Magnetic Field Strength and Morphology in the Sagittarius C Complex. arXiv e-prints , keywords =. doi:10.48550/arXiv.2502.14961 , archivePrefix =. 2502.14961 , primaryClass =

    work page doi:10.48550/arxiv.2502.14961

  47. [47]

    Physics of the Interstellar and Intergalactic Medium

  48. [48]

    The Central 300 pc of the Galaxy Probed by Infrared Spectra of \ \ \ H\ \ \ \_\ 3\ \^\ +\ and CO. I. Predominance of Warm and Diffuse Gas and High H _ 2 Ionization Rate. , keywords =. doi:10.3847/1538-4357/ab3647 , archivePrefix =. 1910.04762 , primaryClass =

    work page doi:10.3847/1538-4357/ab3647 1910

  49. [49]

    , keywords =

    AMS-02 beryllium data and its implication for cosmic ray transport. , keywords =. doi:10.1103/PhysRevD.101.023013 , archivePrefix =. 1910.04113 , primaryClass =

    work page doi:10.1103/physrevd.101.023013 1910

  50. [50]

    Magnetic Field in Clusters of Galaxies

    Magnetic Fields in Clusters of Galaxies. International Journal of Modern Physics D , keywords =. doi:10.1142/S0218271804005080 , archivePrefix =. astro-ph/0410182 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1142/s0218271804005080

  51. [51]

    Candidate radio and stellar sources

    The population of Galactic Centre filaments - III. Candidate radio and stellar sources. , keywords =. doi:10.1093/mnras/stac2415 , archivePrefix =. 2208.11589 , primaryClass =

    work page doi:10.1093/mnras/stac2415

  52. [52]

    Physics of Plasmas , author =

    The basis for cosmic ray feedback:. Physics of Plasmas , author =. 2017 , keywords =. doi:10.1063/1.4984017 , abstract =

    work page doi:10.1063/1.4984017 2017

  53. [53]

    Effect of Alfv \'e n waves on particles

    Cosmic ray streaming - I. Effect of Alfv \'e n waves on particles. , keywords =. doi:10.1093/mnras/172.3.557 , adsurl =

    work page doi:10.1093/mnras/172.3.557

  54. [54]

    Effect of particles on Alfv \'e n waves

    Cosmic ray streaming - II. Effect of particles on Alfv \'e n waves. , keywords =. doi:10.1093/mnras/173.2.245 , adsurl =

    work page doi:10.1093/mnras/173.2.245

  55. [55]

    Plasma Physics for Astrophysics

  56. [56]

    Galactic cosmic rays after the AMS-02 observations

    Galactic cosmic rays after the AMS-02 observations. , keywords =. doi:10.1103/PhysRevD.99.103023 , archivePrefix =. 1904.10220 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.99.103023 1904

  57. [57]

    Galaxies , keywords =

    Cosmic Ray Processes in Galactic Ecosystems. Galaxies , keywords =. doi:10.3390/galaxies11040086 , archivePrefix =. 2306.09924 , primaryClass =

    work page doi:10.3390/galaxies11040086

  58. [58]

    The Origin of Cosmic Rays

  59. [59]

    , keywords =

    Bayesian Approach to Equipartition Estimation of Magnetic Field Strength. , keywords =. doi:10.3847/1538-4365/ad98f5 , archivePrefix =. 2412.03494 , primaryClass =

    work page doi:10.3847/1538-4365/ad98f5

  60. [60]

    High-Resolution, Wide-Field Imaging of the Galactic Center Region at 330 MHz

    High-Resolution, Wide-Field Imaging of the Galactic Center Region at 330 MHz. , keywords =. doi:10.1086/424001 , archivePrefix =. astro-ph/0407178 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/424001