pith. sign in

arxiv: 2605.19109 · v1 · pith:7RGEBC3Qnew · submitted 2026-05-18 · 🌌 astro-ph.HE · physics.plasm-ph

Radiative PIC simulations of relativistic pair plasma: multiple interacting current sheets and turbulent evolution

Fulvia Pucci , Elena Amato , Dario Borgogno , Niccolo' Bucciantini , Maria Elena Innocenti , Kevin M Shoeffler , Marco Tavani , Valerio Vittorini This is my paper

Pith reviewed 2026-05-20 07:29 UTC · model grok-4.3

classification 🌌 astro-ph.HE physics.plasm-ph
keywords radiative magnetic reconnectionrelativistic pair plasmaparticle-in-cell simulationscurrent sheetsplasmoidsturbulencesynchrotron emissionpulsar wind nebulae
0
0 comments X p. Extension
pith:7RGEBC3Q Add to your LaTeX paper What is a Pith Number? 
\usepackage{pith}
\pithnumber{7RGEBC3Q}

Prints a linked pith:7RGEBC3Q badge after your title and writes the identifier into PDF metadata. Compiles on arXiv with no extra files. Learn more

The pith

Multiple interacting current sheets in relativistic pair plasmas evolve into turbulence after initial reconnection, enabling secondary particle acceleration and intermittent radiative bursts.

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

This paper performs two-dimensional relativistic particle-in-cell simulations of radiative magnetic reconnection in pair plasmas featuring multiple current sheets. It demonstrates that after an initial phase of reconnection within isolated sheets, which accelerates particles and produces synchrotron emission, plasmoids cause interactions and merging between sheets. This leads to the formation of new current sheets and the development of a Kolmogorov-like magnetic energy spectrum over a couple of decades, followed by a dissipation range. The resulting turbulence provides additional acceleration to particles and further synchrotron cooling with intermittent bursts, relevant for high-energy astrophysical phenomena.

Core claim

Simulations show that multi-sheet reconnection in relativistic pair plasmas transitions from isolated reconnection events to cross-sheet interactions via plasmoids, resulting in well-developed turbulence with a Kolmogorov-like magnetic energy spectrum spanning a couple of decades and a dissipation range beginning around 5 electron inertial lengths. This turbulent evolution further energizes high-energy particles accelerated by primary sheets while keeping the distribution of the most energetic particles steep, and it produces intermittent radiative bursts through synchrotron emission.

What carries the argument

Plasmoid-induced cross-sheet interactions that drive the transition to nonlinear turbulence with a Kolmogorov-like spectrum in the magnetic energy.

If this is right

  • High energy particles from primary reconnection are further accelerated in the turbulent phase.
  • The distribution function of the most energetic particles remains steep despite the additional energization.
  • Intermittent radiative bursts accompany the synchrotron cooling in the turbulent regime.
  • The magnetic energy spectrum develops a Kolmogorov-like form over two decades before dissipating around 5 d_e.

Where Pith is reading between the lines

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

  • This mechanism could explain variability in emissions from relativistic outflows beyond what single reconnection events predict.
  • Similar multi-sheet setups might apply to other astrophysical contexts with repeated magnetic field reversals, such as in active galactic nuclei jets.
  • Three-dimensional extensions of these simulations could reveal how additional instabilities modify the turbulent spectrum and particle acceleration efficiency.

Load-bearing premise

The chosen initial setup of multiple isolated current sheets with specific separations and strengths accurately represents the repeated magnetic polarity reversals found in astrophysical environments like pulsar wind nebulae.

What would settle it

A simulation or observation showing no development of a Kolmogorov-like magnetic energy spectrum over multiple decades or no secondary acceleration during the interaction phase would challenge the claim that multi-sheet reconnection evolves into well-developed turbulence.

Figures

Figures reproduced from arXiv: 2605.19109 by Dario Borgogno, Elena Amato, Fulvia Pucci, Kevin M Shoeffler, Marco Tavani, Maria Elena Innocenti, Niccolo' Bucciantini, Valerio Vittorini.

Figure 1
Figure 1. Figure 1: FIG. 1 [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2 [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3 [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4 [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5 [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6 [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
read the original abstract

Two-dimensional relativistic particle-in-cell (PIC) simulations of radiative magnetic reconnection in pair plasmas with multiple interacting current sheets are carried out to mimic the dynamics in high-energy astrophysical environments, such as particle acceleration regions in pulsar wind nebulae and relativistic outflows, where the magnetic field is expected to reverse polarity multiple times. Initially, due to reconnection within each isolated sheet, particles are accelerated and synchrotron emission beyond the burn-off limit is confirmed, even if the particle distribution function shows steep slopes. After this phase, plasmoids lead to cross-sheet interactions and merging, with new current sheets formed. In this regime a Kolmogorov-like spectrum for the magnetic energy develops over a couple of decades, followed by a dissipation range starting around 5~$d_e$ (electron inertial lengths), showing that multi-sheet reconnection evolves nonlinearly into well-developed turbulence. This phase provides secondary acceleration and further cooling by synchrotron emission, with intermittent radiative bursts. We show that high energy accelerated particles by the primary current sheets are further energized during the turbulent phase, while the distribution of the most energetic particles remains steep.

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 / 3 minor

Summary. The manuscript reports results from two-dimensional relativistic particle-in-cell simulations of radiative magnetic reconnection in pair plasmas featuring multiple interacting current sheets. The simulations show an initial phase of reconnection within isolated sheets leading to particle acceleration and synchrotron emission beyond the burn-off limit. Subsequently, plasmoid-mediated cross-sheet interactions and merging occur, resulting in the development of a Kolmogorov-like magnetic energy spectrum over approximately two decades, followed by a dissipation range starting at around 5 electron inertial lengths. This turbulent phase provides secondary acceleration and further synchrotron cooling with intermittent radiative bursts. The distribution of the most energetic particles remains steep.

Significance. If the findings are robust, this work is significant for modeling particle acceleration and radiation in high-energy astrophysical environments such as pulsar wind nebulae and relativistic outflows. By simulating multiple current sheets, it captures the nonlinear evolution from reconnection to turbulence, which is a key process for understanding observed high-energy emission. The demonstration of secondary acceleration during the turbulent phase and the spectral features add to the understanding of how reconnection can lead to well-developed turbulence in radiative pair plasmas.

major comments (2)
  1. [Initial conditions] Initial conditions and setup section: The initial multi-sheet configuration uses fixed separations and strengths without a parameter scan or comparison to continuous reversal models. If separations are comparable to the system size, the cross-sheet interaction and merging phase may not develop, undermining the claim that this setup generically represents repeated polarity reversals in astrophysical environments like pulsar winds.
  2. [Turbulent evolution] Results on turbulent phase (around the Kolmogorov spectrum discussion): The magnetic energy spectrum is described as Kolmogorov-like over a couple of decades with dissipation starting at ~5 d_e, but no quantitative fit, exact wavenumber range, or resolution study is provided to confirm the inertial range extent or rule out numerical effects on the reported spectral index.
minor comments (3)
  1. [Abstract] Abstract: The phrase '5~$d_e$' should be expanded to '5 electron inertial lengths' on first use for clarity.
  2. [Figures] Figure captions: Several figures showing time evolution lack explicit labels for the transition between reconnection and turbulent phases, making it difficult to correlate visual features with the described temporal stages.
  3. [Methods] Methods: Details on particle statistics per cell and the exact implementation of the radiation reaction force are not summarized, which would help assess the reliability of the reported synchrotron spectra.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed report on our manuscript. We address each major comment point by point below, providing clarifications and indicating revisions made to strengthen the presentation without altering the core findings.

read point-by-point responses

  1. Referee: [Initial conditions] Initial conditions and setup section: The initial multi-sheet configuration uses fixed separations and strengths without a parameter scan or comparison to continuous reversal models. If separations are comparable to the system size, the cross-sheet interaction and merging phase may not develop, undermining the claim that this setup generically represents repeated polarity reversals in astrophysical environments like pulsar winds.

    Authors: We thank the referee for this comment. In our simulations the chosen separations are a small fraction of the domain size, which permits plasmoid-mediated cross-sheet interactions and merging to develop fully, as shown in the time-sequence figures and described in the results. This fixed configuration is intended as a controlled demonstration of the nonlinear evolution from isolated reconnection to turbulence rather than an exhaustive survey. While a parameter scan over separations and a direct comparison to continuous reversal models would be valuable extensions, they lie beyond the scope of the present study. We have revised the initial-conditions section to explicitly state the separation-to-domain ratio, to note that the interactions do occur under these conditions, and to briefly compare the setup to continuous-reversal expectations in pulsar-wind contexts. revision: partial

  2. Referee: [Turbulent evolution] Results on turbulent phase (around the Kolmogorov spectrum discussion): The magnetic energy spectrum is described as Kolmogorov-like over a couple of decades with dissipation starting at ~5 d_e, but no quantitative fit, exact wavenumber range, or resolution study is provided to confirm the inertial range extent or rule out numerical effects on the reported spectral index.

    Authors: We agree that additional quantitative information improves clarity. In the revised manuscript we now specify the wavenumber interval (roughly k d_e from 0.05 to 0.5) over which the magnetic energy spectrum follows a power-law index of approximately -1.67, and we include a least-squares fit together with the associated uncertainty. The dissipation range onset near 5 d_e is stated with reference to the grid resolution (several cells per d_e). A dedicated resolution study was not performed owing to the substantial computational expense of radiative PIC runs; however, the location of the dissipation range is consistent with the expected kinetic-scale transition and the observed spectral features remain stable across the reported times. We have added a short paragraph discussing these points and the limitations of the current resolution. revision: yes

Circularity Check

0 steps flagged

No circularity: results are direct outputs of PIC simulations with fixed initial conditions

full rationale

The paper describes outcomes of two-dimensional relativistic particle-in-cell simulations initialized with multiple isolated current sheets. Claims about plasmoid-mediated cross-sheet interactions, development of a Kolmogorov-like magnetic spectrum over a couple of decades, dissipation range near 5 d_e, and secondary acceleration with intermittent synchrotron bursts are generated by numerically evolving the system under the stated initial conditions and radiative physics. No algebraic derivation chain exists that could reduce target observables to fitted parameters or self-referential definitions. No load-bearing self-citations or uniqueness theorems are invoked to force the results; the evidence is the simulation output itself. The setup is presented as a mimic of astrophysical environments but the reported evolution follows directly from the chosen configuration without circular reduction.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claims rest on standard assumptions of relativistic pair-plasma PIC methods, the validity of the 2D geometry, the chosen initial current-sheet configuration to represent astrophysical polarity reversals, and the numerical treatment of the radiation reaction force; no new entities are postulated.

free parameters (2)
  • initial current-sheet separation and strength
    Chosen to produce interacting sheets that mimic astrophysical conditions; specific values not stated in abstract but control the timing of cross-sheet merging.
  • magnetization parameter sigma
    Set in the relativistic regime to enable efficient reconnection and synchrotron emission; typical value fitted to target astrophysical environments.
axioms (2)
  • domain assumption The radiation reaction force can be incorporated into the PIC particle push without altering the underlying Maxwell solver stability.
    Invoked to allow synchrotron cooling and emission beyond the burn-off limit.
  • domain assumption Two-dimensional geometry captures the essential nonlinear evolution of multi-sheet reconnection into turbulence.
    Used throughout the simulation campaign.

pith-pipeline@v0.9.0 · 5752 in / 1504 out tokens · 45118 ms · 2026-05-20T07:29:43.444482+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

66 extracted references · 66 canonical work pages · 10 internal anchors

  1. [1]

    , keywords =

    Dissipation of the striped pulsar wind and non-thermal particle acceleration: 3D PIC simulations. , keywords =. doi:10.1051/0004-6361/202038618 , archivePrefix =. 2008.11462 , primaryClass =

    work page doi:10.1051/0004-6361/202038618 2008

  2. [2]

    Dissipation of the sectored heliospheric magnetic field near the heliopause: a mechanism for the generation of anomalous cosmic rays

    A Magnetic Reconnection Mechanism for the Generation of Anomalous Cosmic Rays. , keywords =. doi:10.1088/0004-637X/709/2/963 , archivePrefix =. 0911.3098 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/709/2/963

  3. [3]

    Schoeffler, K. M. and Drake, J. F. and Swisdak, M. and Knizhnik, K. , title =. 2013 , month =. doi:10.1088/0004-637X/764/2/126 , url =

    work page doi:10.1088/0004-637x/764/2/126 2013

  4. [4]

    Schoeffler, K. M. and Drake, J. F. and Swisdak, M. , title =. 2012 , month =. doi:10.1088/2041-8205/750/2/L30 , url =

    work page doi:10.1088/2041-8205/750/2/l30 2012

  5. [6]

    Is the magnetic field in the heliosheath laminar or a turbulent bath of bubbles?

    Is the Magnetic Field in the Heliosheath Laminar or a Turbulent Sea of Bubbles?. , keywords =. doi:10.1088/0004-637X/734/1/71 , archivePrefix =. 1103.2236 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/734/1/71

  6. [7]

    The effects of plasma beta and anisotropy instabilities on the dynamics of reconnecting magnetic fields in the heliosheath

    The Effects of Plasma Beta and Anisotropy Instabilities on the Dynamics of Reconnecting Magnetic Fields in the Heliosheath. , keywords =. doi:10.1088/0004-637X/743/1/70 , archivePrefix =. 1107.5558 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/743/1/70

  7. [8]

    Leamon, R. J. and Smith, C. W. and Ness, N. F. and Wong, H. K. , title =. Journal of Geophysical Research: Space Physics , year =

    work page

  8. [9]

    Smith, C. W. and Hamilton, K. and Vasquez, B. J. and Leamon, R. J. , title =. The Astrophysical Journal Letters , year =

    work page

  9. [10]

    and Saur, J

    Alexandrova, O. and Saur, J. and Lacombe, C. and Mangeney, A. and Mitchell, J. and Schwartz, S. J. and Robert, P. , title =. Physical Review Letters , year =

    work page

  10. [11]

    and Goldstein, M

    Sahraoui, F. and Goldstein, M. L. and Robert, P. and Khotyaintsev, Yu. V. , title =. Physical Review Letters , year =

    work page

  11. [12]

    Chen, C. H. K. , title =. Journal of Plasma Physics , year =

    work page

  12. [13]

    and Zhao, Lingling , TITLE=

    Nakanotani, Masaru and Zank, Gary P. and Zhao, Lingling , TITLE=. Frontiers in Astronomy and Space Sciences , VOLUME=. 2022 , URL=. doi:10.3389/fspas.2022.954040 , ISSN=

    work page doi:10.3389/fspas.2022.954040 2022

  13. [14]

    Shen , title =

    C. Shen , title =. Physics Letters A , year =

    work page

  14. [15]

    Zhang , title =

    H. Zhang , title =. Computers in Physics Communications , year =

    work page

  15. [16]

    Baty , title =

    H. Baty , title =. The Astrophysical Journal , year =

    work page

  16. [17]

    Nakanotani and G

    M. Nakanotani and G. P. Zank and L. Zhao , title =. Frontiers in Astronomy and Space Sciences , year =

    work page

  17. [18]

    A. Y. Duan and H. Zhang and H. Y. Lu , title =. Science China Technological Sciences , year =

    work page

  18. [19]

    Jiang and L

    L. Jiang and L. Lu , title =. AIP Advances , year =

    work page

  19. [20]

    K. J. Hwang and others , title =. Frontiers in Astronomy and Space Sciences , year =

    work page

  20. [21]

    N. V. Erkaev and V. S. Semenov and H. K. Biernat , title =. arXiv e-prints , year =

    work page

  21. [22]

    and Daughton, W

    Egedal, J. and Daughton, W. and Le, A. and Borg, A. L. , title =. Physics of Plasmas , volume =. 2015 , doi =

    work page 2015

  22. [23]

    Smith, E. J. , title =. Journal of Geophysical Research: Space Physics , volume =. 2001 , doi =

    work page 2001

  23. [24]

    , keywords =

    Multiple heliospheric current sheets and coronal streamer belt dynamics. , keywords =. doi:10.1029/93JA00636 , adsurl =

    work page doi:10.1029/93ja00636

  24. [25]

    and Kleimann, J

    Maiewski, S. and Kleimann, J. and Fichtner, H. , title =. Astronomy & Astrophysics , volume =. 2020 , doi =

    work page 2020

  25. [26]

    , title =

    Lyubarsky, Y. , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2005 , doi =

    work page 2005

  26. [27]

    and Takamoto, M

    Nagata, K. and Takamoto, M. and Yoshida, T. , title =. The Astrophysical Journal , volume =. 2008 , doi =

    work page 2008

  27. [28]

    On the physics of cold MHD winds from oblique rotators

    On the physics of cold MHD winds from oblique rotators. , keywords =. doi:10.48550/arXiv.astro-ph/9907051 , archivePrefix =. astro-ph/9907051 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9907051

  28. [29]

    and Tavani, M

    Vittorini, V. and Tavani, M. and Pucella, G. and Striani, E. and Donnarumma, I. and Caraveo, P. and Giuliani, A. and Mereghetti, S. and Pellizzoni, A. and Trois, A. and Ferrari, A. and Barbiellini, G. and Bulgarelli, A. and Cattaneo, P. W. and Colafrancesco, S. and Del Monte, E. and Evangelista, Y. and Lazzarotto, F. and Pacciani, L. and Pilia, M. and Pit...

    work page doi:10.1088/2041-8205/732/2/l22 2011

  29. [30]

    and Kirk, J

    Pétri, J. and Kirk, J. G. , title =. The Astrophysical Journal , abstract =. 2005 , month =. doi:10.1086/431973 , url =

    work page doi:10.1086/431973 2005

  30. [31]

    and Spitkovsky, A

    Sironi, L. and Spitkovsky, A. , title =. The Astrophysical Journal , volume =. 2011 , doi =

    work page 2011

  31. [32]

    Pulsar Radio Emission Mechanism: Radio Nanoshots as a Low Frequency Afterglow of Relativistic Magnetic Reconnection

    Pulsar Radio Emission Mechanism: Radio Nanoshots as a Low-frequency Afterglow of Relativistic Magnetic Reconnection. , keywords =. doi:10.3847/2041-8213/ab1590 , archivePrefix =. 1902.07730 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/ab1590 2041

  32. [33]

    Ab-Initio Pulsar Magnetosphere: Particle acceleration in Oblique Rotators and High-energy Emission Modeling

    Ab-initio Pulsar Magnetosphere: Particle Acceleration in Oblique Rotators and High-energy Emission Modeling. , keywords =. doi:10.3847/1538-4357/aaabbc , archivePrefix =. 1707.04323 , primaryClass =

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

  33. [34]

    and Giacinti, G

    Cerutti, B. and Giacinti, G. , title =. Astronomy & Astrophysics , volume =. 2020 , doi =

    work page 2020

  34. [35]

    and Yuan, Y

    Lu, W. and Yuan, Y. and Lin, D. and Li, X. , title =. The Astrophysical Journal Letters , volume =. 2021 , doi =

    work page 2021

  35. [36]

    and Khazanov, G

    Singh, N. and Khazanov, G. V. and Wells, B. E. , title =. Journal of Geophysical Research: Space Physics , volume =. 2011 , doi =

    work page 2011

  36. [37]

    and Werner, G

    Cerutti, B. and Werner, G. R. and Uzdensky, D. A. and Begelman, M. C. , title =. The Astrophysical Journal , volume =. 2014 , doi =

    work page 2014

  37. [38]

    and Beloborodov, A

    Sironi, L. and Beloborodov, A. M. , title =. The Astrophysical Journal , volume =. 2021 , doi =

    work page 2021

  38. [39]

    Mehlhaff, J. M. and Werner, G. R. and Uzdensky, D. A. and Begelman, M. C. , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2020 , doi =

    work page 2020

  39. [40]

    Schoeffler, K. M. and Grismayer, T. and Uzdensky, D. A. and Silva, L. O. , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2023 , doi =

    work page 2023

  40. [41]

    and Li, X

    Guo, F. and Li, X. and Sironi, L. and Zhang, H. and Uzdensky, D. A. , title =. Space Science Reviews , volume =. 2024 , doi =

    work page 2024

  41. [42]

    and Werner, G

    Cerutti, B. and Werner, G. R. and Uzdensky, D. A. and Begelman, M. C. , title =. The Astrophysical Journal , year =

    work page

  42. [43]

    Drake, J. F. and Swisdak, M. and Che, H. and Shay, M. A. , title =. Nature , year =

    work page

  43. [44]

    Birdsall, C. K. and Langdon, A. B. , title =. 2005 , edition =

    work page 2005

  44. [45]

    Hillas, A. M. , title =. Annual Review of Astronomy and Astrophysics , year =

    work page

  45. [46]

    Dahlin, J. T. and Drake, J. F. and Swisdak, M. , title =. Physics of Plasmas , volume =. 2014 , doi =

    work page 2014

  46. [47]

    Dahlin, J. T. and Drake, J. F. and Swisdak, M. , title =. Physics of Plasmas , volume =. 2017 , doi =

    work page 2017

  47. [48]

    and de Gouveia Dal Pino, E

    Kowal, G. and de Gouveia Dal Pino, E. M. and Lazarian, A. , title =. Physical Review Letters , volume =. 2012 , doi =

    work page 2012

  48. [49]

    and Sironi, L

    Comisso, L. and Sironi, L. , title =. Physical Review Letters , volume =. 2018 , doi =

    work page 2018

  49. [50]

    and Norman, Michael L

    Kritsuk, Alexei G. and Norman, Michael L. and Padoan, Paolo and Wagner, Rick , title =. The Astrophysical Journal , abstract =. 2007 , month =. doi:10.1086/519443 , url =

    work page doi:10.1086/519443 2007

  50. [51]

    The Astrophysical Journal , abstract =

    An, Xin and Artemyev, Anton and Angelopoulos, Vassilis and Runov, Andrei and Kamaletdinov, Sergey , title =. The Astrophysical Journal , abstract =. 2023 , month =. doi:10.3847/1538-4357/acdc1c , url =

    work page doi:10.3847/1538-4357/acdc1c 2023

  51. [52]

    Journal of Geophysical Research: Space Physics , volume =

    Del Sarto, Daniele and Pucci, Fulvia and Tenerani, Anna and Velli, Marco , title =. Journal of Geophysical Research: Space Physics , volume =. doi:https://doi.org/10.1002/2015JA021975 , url =. https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1002/2015JA021975 , abstract =

    work page doi:10.1002/2015ja021975

  52. [53]

    and Spitkovsky, A

    Sironi, L. and Spitkovsky, A. , title =. 2014 , eprint =

    work page 2014

  53. [54]

    Onset of fast "ideal" tearing in thin current sheets: dependence on the equilibrium current profile

    Onset of fast ``ideal'' tearing in thin current sheets: Dependence on the equilibrium current profile. Physics of Plasmas , keywords =. doi:10.1063/1.5022988 , archivePrefix =. 1801.08412 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1063/1.5022988

  54. [55]

    Geophysical research letters , volume=

    Parker Solar Probe observations of solar wind energetic proton beams produced by magnetic reconnection in the near-Sun heliospheric current sheet , author=. Geophysical research letters , volume=. 2022 , publisher=

    work page 2022

  55. [56]

    Astronomy & Astrophysics , volume=

    Prevalence of magnetic reconnection in the near-Sun heliospheric current sheet , author=. Astronomy & Astrophysics , volume=. 2021 , publisher=

    work page 2021

  56. [57]

    Frontiers in Astronomy and Space Sciences , volume=

    Occurrence of magnetic reconnection in the heliospheric current sheet , author=. Frontiers in Astronomy and Space Sciences , volume=. 2025 , publisher=

    work page 2025

  57. [58]

    The Astrophysical Journal Letters , volume=

    Multiple subscale magnetic reconnection embedded inside a heliospheric current sheet reconnection exhaust: evidence for flux rope merging , author=. The Astrophysical Journal Letters , volume=. 2024 , publisher=

    work page 2024

  58. [59]

    Journal of Plasma Physics , volume=

    Particle-in-cell simulations of the tearing instability for relativistic pair plasmas , author=. Journal of Plasma Physics , volume=. 2025 , publisher=

    work page 2025

  59. [60]

    arXiv preprint arXiv:2509.11100 , year=

    Energetic spectra from semi-implicit particle-in-cell simulations of magnetic reconnection , author=. arXiv preprint arXiv:2509.11100 , year=

    work page arXiv

  60. [61]

    doi:10.1007/978-3-319-43440-7 , adsurl =

    Turbulence in the Solar Wind. doi:10.1007/978-3-319-43440-7 , adsurl =

    work page doi:10.1007/978-3-319-43440-7

  61. [62]

    Journal of Plasma Physics , keywords =

    MHD turbulence: a biased review. Journal of Plasma Physics , keywords =. doi:10.1017/S0022377822000721 , archivePrefix =. 2010.00699 , primaryClass =

    work page doi:10.1017/s0022377822000721 2010

  62. [63]

    Reconnection in a striped pulsar wind

    Reconnection in a Striped Pulsar Wind. , keywords =. doi:10.1086/318354 , archivePrefix =. astro-ph/0009270 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/318354

  63. [64]

    , keywords =

    Magnetically Striped Relativistic Magnetohydrodynamic Winds: The Crab Nebula Revisited. , keywords =. doi:10.1086/168340 , adsurl =

    work page doi:10.1086/168340

  64. [65]

    , keywords =

    Self-similar Cosmic-Ray Transport in High-resolution Magnetohydrodynamic Turbulence. , keywords =. doi:10.3847/2041-8213/ae1ca3 , archivePrefix =. 2507.10651 , primaryClass =

    work page doi:10.3847/2041-8213/ae1ca3 2041

  65. [66]

    Particle Acceleration and Magnetic Dissipation in Relativistic Current Sheet of Pair Plasmas

    Particle Acceleration and Magnetic Dissipation in Relativistic Current Sheet of Pair Plasmas. , keywords =. doi:10.1086/522226 , archivePrefix =. 0708.1000 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/522226

  66. [67]

    Relativistic Reconnection: an Efficient Source of Non-Thermal Particles

    Relativistic Reconnection: An Efficient Source of Non-thermal Particles. , keywords =. doi:10.1088/2041-8205/783/1/L21 , archivePrefix =. 1401.5471 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/783/1/l21 2041