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arxiv: 2606.01775 · v1 · pith:SV7N3BODnew · submitted 2026-06-01 · 🌌 astro-ph.HE · astro-ph.CO

Reconnection-Driven Injection and Stochastic Reacceleration during Cosmological Magnetogenesis

Ji-Hoon Ha This is my paper

Pith reviewed 2026-06-28 13:43 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.CO
keywords cosmological magnetogenesismagnetic reconnectioncosmic ray seedsFokker-Planck equationsuprathermal protonsintergalactic mediumshock accelerationgamma-ray emission
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The pith

Reconnection during cosmological magnetogenesis injects suprathermal protons but yields a nonthermal energy fraction of only 10^{-7}.

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

The paper asks whether magnetic reconnection can supply seed particles for cosmic rays in the early universe before galaxies form. It extends an earlier model by adding a source term to the equation tracking ion energies, with the added power drawn from the growing magnetic field. This term creates a visible high-energy tail in the particle distribution, yet the total energy in that tail stays tiny because the available magnetic energy is small in the dilute, high-beta plasma. The tail can raise the number of particles ready for later acceleration at structure-formation shocks by roughly a factor of ten, but the gamma rays those particles would produce remain undetectable.

Core claim

Reconnection acts as a fast injection channel and produces a visible suprathermal tail. However, the resulting nonthermal energy fraction remains very small, of order 10^{-7} in the fiducial model, implying a negligible nonthermal pressure contribution to the pre-structure intergalactic medium. This limitation arises because the extremely high-beta plasma contains only a small magnetic-energy reservoir. Using a test-particle shock reacceleration estimate, the reconnection-produced tail can enhance the suprathermal proton population available for later structure-formation shocks by about an order of magnitude, yet the associated hadronic gamma-ray emission from low-density cluster outskirts s

What carries the argument

A phenomenological reconnection-driven source term added to the Fokker-Planck equation for the isotropic ion distribution, with its injection power tied directly to the magnetic-energy growth rate.

If this is right

  • Reconnection during cosmological magnetogenesis is unlikely to dominate the cosmic-ray energy budget directly.
  • The nonthermal pressure contribution to the pre-structure intergalactic medium remains negligible.
  • The reconnection-produced suprathermal tail enhances the seed population available for structure-formation shocks by about an order of magnitude.
  • Hadronic gamma-ray emission from low-density cluster outskirts remains far below current detectability.

Where Pith is reading between the lines

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

  • If reconnection operates more efficiently at unresolved scales, the seed population could become large enough to alter the starting conditions for shock acceleration in forming structures.
  • The same small magnetic reservoir that caps the nonthermal fraction also limits how much the process could affect the overall thermal history of the intergalactic medium.
  • Future simulations that resolve reconnection sites explicitly could test whether the assumed tie between magnetic growth rate and injection power holds in expanding cosmology.

Load-bearing premise

The power injected by reconnection is taken to scale directly with the rate at which magnetic energy grows, and that reservoir itself is limited by the small magnetic fraction present in the high-beta plasma.

What would settle it

A measurement or simulation showing the nonthermal proton energy fraction during magnetogenesis exceeding roughly 10^{-6} would indicate that the reconnection source term supplies more energy than assumed.

Figures

Figures reproduced from arXiv: 2606.01775 by Ji-Hoon Ha.

Figure 1
Figure 1. Figure 1: Redshift evolution of the normalized reconnection injection rate [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Comparison of the dimensionless loss time [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Critical effective reconnection efficiency ηrec,crit(E,z). Panel (a) shows ηrec,crit as a function of redshift for fixed injected particle energies E = 1, 3, and 10 eV. Panel (b) shows ηrec,crit as a function of injected particle energy at fixed redshifts z = 3, 5, and 10. The dashed horizontal line marks ηrec = 10−8 . ∆ex = 0.1|∆| is used for all calculations. loss processes and injected particles can sur… view at source ↗
Figure 4
Figure 4. Figure 4: Fokker–Planck solutions with reconnection-driven injection. Panel [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Shock reacceleration of reconnection-produced seed particles. [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
read the original abstract

We investigate whether magnetic reconnection can provide suprathermal proton seed particles during cosmological magnetogenesis prior to nonlinear structure formation. Previous work showed that pressure-anisotropy-driven stochastic acceleration alone is strongly limited by cosmological expansion and Coulomb cooling. Here, we extend this framework by adding a phenomenological reconnection-driven source term to the Fokker--Planck equation for the isotropic ion distribution, with the injection power tied to the magnetic-energy growth rate during magnetogenesis. We find that reconnection can act as a fast injection channel and can produce a visible suprathermal tail. However, the resulting nonthermal energy fraction remains very small, of order $10^{-7}$ in the fiducial model, implying a negligible nonthermal pressure contribution to the pre-structure intergalactic medium. This limitation arises because the extremely high-beta plasma contains only a small magnetic-energy reservoir, even when reconnection itself is locally fast. Using a test-particle shock reacceleration estimate, we further show that the reconnection-produced tail can enhance the suprathermal proton population available for later structure-formation shocks by about an order of magnitude. Nevertheless, the associated hadronic gamma-ray emission from low-density cluster outskirts is expected to remain far below current detectability. We therefore conclude that reconnection during cosmological magnetogenesis is unlikely to dominate the cosmic-ray energy budget directly, but may provide a low-level seed population for subsequent shock acceleration.

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

1 major / 2 minor

Summary. The manuscript investigates whether magnetic reconnection can inject suprathermal protons as seed particles during cosmological magnetogenesis by extending prior work on pressure-anisotropy-driven stochastic acceleration. It adds a phenomenological reconnection-driven source term to the Fokker-Planck equation for the isotropic ion distribution, with injection power tied directly to the magnetic-energy growth rate. The central results are that the nonthermal energy fraction remains of order 10^{-7} (negligible for pre-structure IGM pressure), the reconnection tail can enhance the suprathermal population available for later shocks by roughly an order of magnitude, and associated hadronic gamma-ray emission stays below detectability. The conclusion is that reconnection is unlikely to dominate the cosmic-ray budget directly but may supply a low-level seed population.

Significance. If the modeling holds, the work supplies a quantitative upper limit on reconnection's direct contribution to the cosmic-ray energy budget in the high-beta regime, showing that the small magnetic-energy reservoir (combined with expansion and cooling) caps the nonthermal fraction at a very low level. The test-particle shock reacceleration estimate provides a concrete, falsifiable link to structure-formation models and clarifies the seeding role for subsequent acceleration. This is a useful clarification for cosmic-ray origin studies even if the absolute normalization carries model dependence.

major comments (1)
  1. [model description / Fokker-Planck setup] The reconnection-driven source term in the Fokker-Planck equation has its injection power normalized directly to the magnetic-energy growth rate. This choice sets the reported nonthermal fraction (~10^{-7}) by construction once the high-beta limit is adopted, rather than through an independent calibration or external benchmark; the absence of sensitivity tests on the normalization parameter therefore makes the numerical value of the energy fraction and the order-of-magnitude seed enhancement dependent on an unvalidated modeling assumption.
minor comments (2)
  1. No error bars, Monte-Carlo realizations, or parameter-variation scans are described for the fiducial nonthermal fraction or the shock-seed enhancement factor.
  2. The high-beta assumption and the precise form of the phenomenological source term would benefit from a short dedicated paragraph justifying the chosen normalization against existing kinetic simulations of reconnection in high-beta plasmas.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the constructive feedback on our manuscript. We address the single major comment below and indicate the planned revisions.

read point-by-point responses

  1. Referee: The reconnection-driven source term in the Fokker-Planck equation has its injection power normalized directly to the magnetic-energy growth rate. This choice sets the reported nonthermal fraction (~10^{-7}) by construction once the high-beta limit is adopted, rather than through an independent calibration or external benchmark; the absence of sensitivity tests on the normalization parameter therefore makes the numerical value of the energy fraction and the order-of-magnitude seed enhancement dependent on an unvalidated modeling assumption.

    Authors: The normalization to the magnetic-energy growth rate is a phenomenological modeling choice motivated by the physical expectation that reconnection dissipates stored magnetic energy into suprathermal particles. In the high-beta regime relevant to pre-structure IGM, this necessarily yields a small nonthermal fraction because the magnetic reservoir itself is tiny relative to the thermal energy. We acknowledge, however, that the absolute normalization (i.e., the efficiency with which dissipated magnetic energy is channeled into the nonthermal tail) is not independently calibrated and that sensitivity tests are absent. In the revised manuscript we will add explicit sensitivity calculations varying the normalization parameter over a plausible range and will report the resulting variation in the nonthermal fraction and seed enhancement. revision: yes

Circularity Check

0 steps flagged

No significant circularity identified

full rationale

The paper adopts a phenomenological source term with injection power tied to magnetic-energy growth rate as an explicit modeling choice. The resulting nonthermal fraction of order 10^{-7} is a direct numerical consequence of the high-beta regime (magnetic energy reservoir << thermal energy) within that setup. No load-bearing step reduces a claimed derivation or prediction to its own inputs by construction; the limitation is presented as following from the plasma beta and the chosen normalization. The framework is self-contained as a model calculation with no evident self-citation chain or self-definitional reduction in the abstract or described chain.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The result rests on a phenomenological source term whose amplitude is set by the magnetic growth rate and on the domain assumption of an extremely high-beta plasma; no independent evidence for the normalization is supplied.

free parameters (1)
  • reconnection source normalization
    Injection power is tied phenomenologically to magnetic-energy growth rate in the fiducial model; the resulting 10^{-7} fraction depends on this choice.
axioms (2)
  • domain assumption Pressure-anisotropy-driven stochastic acceleration is strongly limited by cosmological expansion and Coulomb cooling
    Invoked as the baseline that reconnection extends.
  • domain assumption Extremely high-beta plasma during magnetogenesis contains only a small magnetic-energy reservoir
    Stated as the reason the nonthermal fraction remains small even with fast reconnection.

pith-pipeline@v0.9.1-grok · 5770 in / 1394 out tokens · 33768 ms · 2026-06-28T13:43:04.297428+00:00 · methodology

discussion (0)

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Works this paper leans on

63 extracted references · 53 canonical work pages · 20 internal anchors

  1. [1]

    2015, , 579, A101

    Aladro, R., Martín, S., Riquelme, D., et al. 2015, , 579, A101

    2015

  2. [2]

    Search for cosmic-ray induced gamma-ray emission in Galaxy Clusters

    Search for Cosmic-Ray-induced Gamma-Ray Emission in Galaxy Clusters. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/787/1/18 , archivePrefix =. 1308.5654 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/787/1/18

  3. [3]

    Detection of the Characteristic Pion-Decay Signature in Supernova Remnants

    Detection of the Characteristic Pion-Decay Signature in Supernova Remnants. Science , keywords =. doi:10.1126/science.1231160 , archivePrefix =. 1302.3307 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.1231160

  4. [4]

    and Le, Truong and Dermer, Charles D

    Becker, Peter A. and Le, Truong and Dermer, Charles D. , title =. 2006 , month =. doi:10.1086/505319 , url =

    work page doi:10.1086/505319 2006

  5. [5]

    Monthly Notices of the Royal Astronomical Society , keywords =

    The acceleration of cosmic rays in shock fronts - I. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/182.2.147 , adsnote =

    work page doi:10.1093/mnras/182.2.147

  6. [6]

    The Astrophysical Journal Letters , keywords =

    Particle acceleration by astrophysical shocks. The Astrophysical Journal Letters , keywords =. doi:10.1086/182658 , adsnote =

    work page doi:10.1086/182658

  7. [7]

    and Lazarian, A

    Brunetti, G. and Lazarian, A. , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2016 , month =

    2016

  8. [8]

    , keywords =

    Compressible turbulence in galaxy clusters: physics and stochastic particle re-acceleration. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1111/j.1365-2966.2007.11771.x , archivePrefix =. astro-ph/0703591 , primaryClass =

    work page doi:10.1111/j.1365-2966.2007.11771.x 2007

  9. [9]

    Simulations of Ion Acceleration at Non-relativistic Shocks. I. Acceleration Efficiency. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/783/2/91 , archivePrefix =. 1310.2943 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/783/2/91

  10. [10]

    Journal of Plasma Physics , author=

    A review of the 0.1 reconnection rate problem , volume=. Journal of Plasma Physics , author=. 2017 , pages=. doi:10.1017/S0022377817000666 , number=

    work page doi:10.1017/s0022377817000666 2017

  11. [11]

    doi:10.3847/1538-4357/ab4c33 , year =

    Comisso, Luca and Sironi, Lorenzo , title =. doi:10.3847/1538-4357/ab4c33 , year =

    work page doi:10.3847/1538-4357/ab4c33

  12. [12]

    Physical Review Letters , volume =

    Particle Acceleration in Relativistic Plasma Turbulence , author =. Physical Review Letters , volume =. 2018 , month =

    2018

  13. [13]

    An introduction to the theory of diffusive shock acceleration of energetic particles in tenuous plasmas.Rep

    REVIEW ARTICLE: An introduction to the theory of diffusive shock acceleration of energetic particles in tenuous plasmas. Reports on Progress in Physics , keywords =. doi:10.1088/0034-4885/46/8/002 , adsnote =

    work page doi:10.1088/0034-4885/46/8/002

  14. [14]

    10.1051/0004-6361/201015652

    Cosmic ray transport in galaxy clusters: implications for radio halos, gamma-ray signatures, and cool core heating , DOI= "10.1051/0004-6361/201015652", journal =

    work page doi:10.1051/0004-6361/201015652

  15. [15]

    and Kowal, G

    Falceta-Gonçalves, D. and Kowal, G. , title =. 2015 , month =. doi:10.1088/0004-637X/808/1/65 , url =

    work page doi:10.1088/0004-637x/808/1/65 2015

  16. [16]

    On the Origin of the Cosmic Radiation.Phys

    On the Origin of the Cosmic Radiation. Physical Review , year = 1949, month = apr, volume =. doi:10.1103/PhysRev.75.1169 , adsurl =

    work page doi:10.1103/physrev.75.1169 1949

  17. [17]

    10.1051/0004-6361/201322295

    Constraining turbulence and conduction in the hot ICM through density perturbations , DOI= "10.1051/0004-6361/201322295", url= "https://doi.org/10.1051/0004-6361/201322295", journal =

    work page doi:10.1051/0004-6361/201322295

  18. [18]

    Gould , abstract =

    R.J. Gould , abstract =. Energy loss of a fast ion in a plasma , journal =. 1971 , issn =. doi:https://doi.org/10.1016/0375-9601(71)90658-X , url =

    work page doi:10.1016/0375-9601(71)90658-x 1971

  19. [19]

    2026 , issn =

    Stochastic particle acceleration during pressure-anisotropy-driven magnetogenesis in the pre-structure Universe , journal =. 2026 , issn =. doi:https://doi.org/10.1016/j.astropartphys.2026.103264 , author =

    work page doi:10.1016/j.astropartphys.2026.103264 2026

  20. [20]

    Universe , VOLUME =

    Ha, Ji-Hoon , TITLE =. Universe , VOLUME =. 2025 , NUMBER =

    2025

  21. [21]

    2023 , month =

    Ha, Ji-Hoon and Ryu, Dongsu and Kang, Hyesung , title =. 2023 , month =. doi:10.3847/1538-4357/acabbe , url =

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

  22. [22]

    2020 , month =

    Ha, Ji-Hoon and Ryu, Dongsu and Kang, Hyesung , title =. 2020 , month =. doi:10.3847/1538-4357/ab7c5b , url =

    work page doi:10.3847/1538-4357/ab7c5b 2020

  23. [23]

    Proton Acceleration in Weak Quasi-parallel Intracluster Shocks: Injection and Early Acceleration

    Proton Acceleration in Weak Quasi-parallel Intracluster Shocks: Injection and Early Acceleration. The Astrophysical Journal , keywords =. doi:10.3847/1538-4357/aad634 , archivePrefix =. 1807.09403 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aad634

  24. [24]

    Properties of Merger Shocks in Merging Galaxy Clusters

    Properties of Merger Shocks in Merging Galaxy Clusters. The Astrophysical Journal , keywords =. doi:10.3847/1538-4357/aab4a2 , archivePrefix =. 1706.05509 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aab4a2

  25. [25]

    The Quiescent Intracluster Medium in the Core of the Perseus Cluster

    The quiescent intracluster medium in the core of the Perseus cluster. Nature , keywords =. doi:10.1038/nature18627 , archivePrefix =. 1607.04487 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature18627

  26. [26]

    The blazar sequence: A new perspective.Mon

    Diffuse radio emission from clusters in the MareNostrum Universe simulation. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1111/j.1365-2966.2008.13955.x , archivePrefix =. 0807.1266 , primaryClass =

    work page doi:10.1111/j.1365-2966.2008.13955.x 2008

  27. [27]

    Shock Waves and Cosmic Ray Acceleration in the Outskirts of Galaxy Clusters

    Shock Waves and Cosmic Ray Acceleration in the Outskirts of Galaxy Clusters. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/785/2/133 , archivePrefix =. 1403.1420 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/785/2/133

  28. [28]

    2011 , month =

    Kang, Hyesung and Ryu, Dongsu , title =. 2011 , month =. doi:10.1088/0004-637X/734/1/18 , url =

    work page doi:10.1088/0004-637x/734/1/18 2011

  29. [29]

    Diffusive Shock Acceleration in Test-Particle Regime

    Diffusive Shock Acceleration in Test-particle Regime. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/721/1/886 , archivePrefix =. 1008.0429 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/721/1/886

  30. [30]

    Gamma-Rays from Intergalactic Shocks

    Gamma Rays from Intergalactic Shocks. The Astrophysical Journal , keywords =. doi:10.1086/345946 , archivePrefix =. astro-ph/0202318 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/345946

  31. [31]

    Nature , year = 1995, month = nov, volume =

    Evidence for shock acceleration of high-energy electrons in the supernova remnant SN1006. Nature , year = 1995, month = nov, volume =. doi:10.1038/378255a0 , adsurl =

    work page doi:10.1038/378255a0 1995

  32. [32]

    and Jones, Thomas W

    Kunz, Matthew W. and Jones, Thomas W. and Zhuravleva, Irina. Plasma Physics of the Intracluster Medium. Handbook of X-ray and Gamma-ray Astrophysics. 2022. doi:10.1007/978-981-16-4544-0_125-1

    work page doi:10.1007/978-981-16-4544-0_125-1 2022

  33. [33]

    Kunz, M. W. and Schekochihin, A. A. and Cowley, S. C. and Binney, J. J. and Sanders, J. S. , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2011 , month =. doi:10.1111/j.1365-2966.2010.17621.x , url =

    work page doi:10.1111/j.1365-2966.2010.17621.x 2011

  34. [34]

    and Smith, K

    Komatsu, E. and Smith, K. M. and Dunkley, J. and Bennett, C. L. and Gold, B. and Hinshaw, G. and Jarosik, N. and Larson, D. and Nolta, M. R. and Page, L. and Spergel, D. N. and Halpern, M. and Hill, R. S. and Kogut, A. and Limon, M. and Meyer, S. S. and Odegard, N. and Tucker, G. S. and Weiland, J. L. and Wollack, E. and Wright, E. L. , title =. 2011 , mo...

    work page internal anchor Pith review doi:10.1088/0067-0049/192/2/18 2011

  35. [35]

    Why does Steady-State Magnetic Reconnection have a Maximum Local Rate of Order 0.1? , author =. Phys. Rev. Lett. , volume =. 2017 , month =

    2017

  36. [36]

    Miniati, Francesco and Bell, A. R. , title =. 2011 , month =. doi:10.1088/0004-637X/729/1/73 , url =

    work page doi:10.1088/0004-637x/729/1/73 2011

  37. [37]

    2003, MNRAS, 344, 1000, doi: 10.1046/j.1365-8711.2003.06897.x

    Numerical modelling of gamma radiation from galaxy clusters. Monthly Notice of the Royal Astronomical Society , keywords =. doi:10.1046/j.1365-8711.2003.06647.x , archivePrefix =. astro-ph/0303593 , primaryClass =

    work page doi:10.1046/j.1365-8711.2003.06647.x 2003

  38. [38]

    Properties of Cosmic Shock Waves in Large Scale Structure Formation

    Properties of Cosmic Shock Waves in Large-Scale Structure Formation. The Astrophysical Journal , keywords =. doi:10.1086/317027 , archivePrefix =. astro-ph/0005444 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/317027

  39. [39]

    Earth, Planets and Space , keywords =

    Magnetic reconnection in large-scale cosmic plasmas. Earth, Planets and Space , keywords =. doi:10.1186/BF03353288 , adsnote =

    work page doi:10.1186/bf03353288

  40. [40]

    Energetics of high-energy cosmic radiations , author =. Phys. Rev. D , volume =. 2019 , month =. doi:10.1103/PhysRevD.99.063012 , url =

    work page doi:10.1103/physrevd.99.063012 2019

  41. [41]

    Origin and impacts of the first cosmic rays , author =. Phys. Rev. D , volume =. 2019 , month =. doi:10.1103/PhysRevD.100.061301 , url =

    work page doi:10.1103/physrevd.100.061301 2019

  42. [42]

    Inverse Compton emission from a cosmic-ray precursor in RX J1713.7-3946 , journal =

    Yutaka Ohira and Ryo Yamazaki , keywords =. Inverse Compton emission from a cosmic-ray precursor in RX J1713.7-3946 , journal =. 2017 , issn =. doi:https://doi.org/10.1016/j.jheap.2017.03.001 , url =

    work page doi:10.1016/j.jheap.2017.03.001 2017

  43. [43]

    Galactic longitudes 6 to 20

    Ohira, Yutaka and Murase, Kohta and Yamazaki, Ryo , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2011 , month =. doi:10.1111/j.1365-2966.2010.17539.x , url =

    work page doi:10.1111/j.1365-2966.2010.17539.x 2011

  44. [44]

    Simultaneous Acceleration of Protons and Electrons at Nonrelativistic Quasiparallel Collisionless Shocks

    Simultaneous Acceleration of Protons and Electrons at Nonrelativistic Quasiparallel Collisionless Shocks. Physical Review Letters , keywords =. doi:10.1103/PhysRevLett.114.085003 , archivePrefix =. 1412.0672 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.114.085003

  45. [45]

    Planck 2018 results. VI. Cosmological parameters. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361/201833910 , archivePrefix =. 1807.06209 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833910 2018

  46. [46]

    Stochastic Acceleration by Turbulence

    Stochastic Acceleration by Turbulence. Space Science Reviews , keywords =. doi:10.1007/s11214-012-9900-6 , archivePrefix =. 1205.2136 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s11214-012-9900-6

  47. [47]

    , keywords =

    Detecting shock waves in cosmological smoothed particle hydrodynamics simulations. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1111/j.1365-2966.2005.09953.x , archivePrefix =. astro-ph/0603483 , primaryClass =

    work page doi:10.1111/j.1365-2966.2005.09953.x 2005

  48. [48]

    Galactic longitudes 6 to 20

    Simulating the -ray emission from galaxy clusters: a universal cosmic ray spectrum and spatial distribution. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1111/j.1365-2966.2010.17328.x , archivePrefix =. 1001.5023 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.17328.x 2010

  49. [49]

    The Astrophysical Journal , keywords =

    A Diffusive Shock Acceleration Model for Protons in Weak Quasi-parallel Intracluster Shocks. The Astrophysical Journal , keywords =. doi:10.3847/1538-4357/ab3a3a , archivePrefix =. 1905.04476 , primaryClass =

    work page doi:10.3847/1538-4357/ab3a3a 1905

  50. [50]

    Science , volume =

    Dongsu Ryu and Hyesung Kang and Jungyeon Cho and Santabrata Das , title =. Science , volume =. 2008 , doi =

    2008

  51. [51]

    Cosmological Shock Waves and Their Role in the Large Scale Structure of the Universe

    Cosmological Shock Waves and Their Role in the Large-Scale Structure of the Universe. The Astrophysical Journal , keywords =. doi:10.1086/376723 , archivePrefix =. astro-ph/0305164 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/376723

  52. [52]

    The Energy Spectrum of Primary Cosmic Ray Electrons in Clusters of Galaxies and Inverse Compton Emission

    The Energy Spectrum of Primary Cosmic-Ray Electrons in Clusters of Galaxies and Inverse Compton Emission. The Astrophysical Journal , keywords =. doi:10.1086/307501 , archivePrefix =. astro-ph/9901061 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/307501

  53. [53]

    Shock finding on a moving-mesh: I. Shock statistics in non-radiative cosmological simulations

    Shock finding on a moving mesh - I. Shock statistics in non-radiative cosmological simulations. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/stu2386 , archivePrefix =. 1407.4117 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu2386

  54. [54]

    Schekochihin, A. A. and Cowley, S. C. , title =. Physics of Plasmas , volume =. 2006 , month =

    2006

  55. [55]

    Schekochihin, A. A. and Cowley, S. C. , title =. Astronomische Nachrichten , volume =. doi:https://doi.org/10.1002/asna.200610600 , year =

    work page doi:10.1002/asna.200610600

  56. [56]

    Schekochihin, A. A. and Cowley, S. C. and Kulsrud, R. M. and Hammett, G. W. and Sharma, P. , title =. doi:10.1086/431202 , year =

    work page doi:10.1086/431202

  57. [57]

    Cosmic Ray Astrophysics

  58. [58]

    Cosmological Shocks in Adaptive Mesh Refinement Simulations and the Acceleration of Cosmic Rays

    Cosmological Shocks in Adaptive Mesh Refinement Simulations and the Acceleration of Cosmic Rays. The Astrophysical Journal , keywords =. doi:10.1086/592496 , archivePrefix =. 0806.1522 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/592496

  59. [59]

    , keywords =

    Shock waves in Eulerian cosmological simulations: main properties and acceleration of cosmic rays. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1111/j.1365-2966.2009.14691.x , archivePrefix =. 0808.0609 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.14691.x 2009

  60. [60]

    The First Magnetic Fields

    The First Magnetic Fields. Space Science Reviews , keywords =. doi:10.1007/s11214-011-9833-5 , archivePrefix =. 1109.4052 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s11214-011-9833-5

  61. [61]

    Monthly Notices of the Royal Astronomical Society , volume =

    Wiener, Joshua and Zweibel, Ellen G , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2019 , month =

    2019

  62. [62]

    and Oh, S

    Wiener, Joshua and Zweibel, Ellen G. and Oh, S. Peng , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2018 , month =

    2018

  63. [63]

    Cosmic Ray Streaming in Clusters of Galaxies

    Cosmic ray streaming in clusters of galaxies. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/stt1163 , archivePrefix =. 1303.4746 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt1163