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arxiv: 2606.31439 · v1 · pith:P4LYWFBWnew · submitted 2026-06-30 · 🌌 astro-ph.HE

Scattering of Strong Radio Waves by Particles in Strongly Magnetized Plasmas and Implications for Fast Radio Bursts

Yuanhong Qu , Pawan Kumar This is my paper

Pith reviewed 2026-07-01 04:37 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords fast radio burstsmagnetar magnetospheresscattering cross sectionsstrongly magnetized plasmasO-mode and X-mode wavesrelativistic particle motionoptical depthAlfvén waves
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The pith

Strong radio waves from fast radio bursts experience scattering cross sections suppressed by relativistic motion when propagating nearly parallel to magnetic field lines, yielding optical depths well below unity.

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

The paper solves the relativistic equations of motion for a charged particle interacting with large-amplitude electromagnetic waves of arbitrary polarization and angle to the background field. It derives the resulting scattering cross sections for O-mode and X-mode waves and shows that, in the strongly magnetized quasi-parallel limit, these cross sections recover the familiar linear-regime scalings yet are further reduced by relativistic effects. The corresponding optical depths through a typical magnetar magnetosphere therefore remain far below one, and curvature-radiation losses for the O-mode are likewise suppressed. The work proposes that Alfvén waves triggered by crust quakes can straighten open field lines, reducing the propagation angle and thereby enabling the waves to escape without significant single-particle scattering.

Core claim

By solving the relativistic motion of a single particle in electromagnetic waves of arbitrary polarization and propagation angle θ_B, the scattering cross section of the O-mode exceeds that of the X-mode when a sin θ_B < ω_B/ω and becomes comparable when a sin θ_B > ω_B/ω; in the strongly magnetized and quasi-parallel limits the cross sections recover linear-regime scalings while being strongly suppressed by relativistic particle motion, producing optical depths well below unity and allowing large-amplitude waves to propagate through open field lines without significant scattering losses.

What carries the argument

Relativistic single-particle scattering cross section computed from the particle trajectory in waves of arbitrary polarization and angle θ_B to the background magnetic field.

If this is right

  • Optical depths for both O- and X-modes fall well below unity in the strongly magnetized quasi-parallel regime.
  • Curvature radiation losses for O-mode waves are suppressed, permitting escape at moderate plasma multiplicities.
  • Field-line straightening by large-amplitude Alfvén waves further reduces θ_B and scattering losses.
  • Large-amplitude waves aligned with open field lines can therefore propagate through the magnetosphere without significant single-particle scattering.

Where Pith is reading between the lines

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

  • If the suppression holds, FRB polarization and frequency structure may be preserved from deeper in the magnetosphere than previously expected.
  • The same relativistic suppression mechanism could apply to other coherent radio sources in strongly magnetized environments, such as pulsar giant pulses.
  • Observational tests could include searching for a correlation between FRB polarization angle and inferred propagation geometry relative to the magnetic axis.

Load-bearing premise

Alfvén waves excited by magnetar crust quakes can reach amplitudes comparable to the background magnetic field and thereby straighten field lines enough to reduce the wave propagation angle θ_B.

What would settle it

A direct numerical integration of the particle motion showing that the optical depth remains above unity for quasi-parallel propagation at the amplitudes and densities inferred for FRB sources.

Figures

Figures reproduced from arXiv: 2606.31439 by Pawan Kumar, Yuanhong Qu.

Figure 1
Figure 1. Figure 1: Top panel: In a static dipolar magnetic field, both X- and O-mode waves can escape from the magnetosphere in regions close to the magnetic moment, where the wave vector is nearly quasi-parallel to the background magnetic field (yellow region). In regions farther from the magnetic moment (orange region), only X-mode waves can escape, since O-mode waves undergo stronger nonlinear scattering when propagating … view at source ↗
Figure 2
Figure 2. Figure 2: The normalized cross section 𝜎′/𝜎T as a function of 𝜔′ 𝐵 /𝜔′ for O-mode waves with 𝑎 = 1 (orange) and 𝑎 = 102 (red), evaluated at a fixed propagation angle 𝜃 ′ 𝐵 = 0.1. where 𝜎 is the cross section in the lab frame, 𝑃 ′ and 𝑆 ′ denote the emitted power of the particle and Poynting flux of incident waves in the comoving frame. We first solve the particle dynamics in the comoving frame, then evaluate the rad… view at source ↗
Figure 3
Figure 3. Figure 3: Total emitted curvature-radiation energy (color scale; upper left, upper right, and lower left panels) and characteristic energy of curvature photons (lower right panel) as functions of the FRB luminosity 𝐿FRB for O-mode waves and the propagation angle 𝜃𝐵. The upper left, upper right, and lower left panels correspond to 𝜉 = 102 , 104 , and 106 , respectively. The three black dashed contours indicate the fr… view at source ↗
Figure 4
Figure 4. Figure 4: The electron Lorentz factor (upper subpanel) and normalized scattering cross section (lower subpanel) as a function of time for different 𝜃 ′ 𝐵 = 0.1, 0.5, 𝜋/2 for left, central and right panels, respectively. The non-linear parameter 𝑎 = 104 and 𝜔′ 𝐵 /𝜔′ = 35 are adopted for all panels. sections are further reduced. They remain nearly flat as a function of 𝜔 ′ 𝐵 /𝜔 ′ before undergoing a rapid decline at t… view at source ↗
Figure 5
Figure 5. Figure 5: The normalized scattering cross section 𝜎′/(𝑎 2 𝜎T) as a function of 𝜔′ 𝐵 /𝜔′ for different propagation angles 𝜃 ′ 𝐵 . The four panels correspond to 𝜃 ′ 𝐵 = 𝜋/2, 10−1 , 10−2 , 10−3 (from top left to bottom right). Red, blue, and orange curves denote X-mode, O-mode, and circularly polarized waves, respectively. The black dotted lines indicate the characteristic scalings in different regimes: 𝜎′ ∝ (𝜔′ 𝐵 /𝜔′ … view at source ↗
Figure 6
Figure 6. Figure 6: The normalized cross section 𝜎′/𝜎T as a function of 𝜃 ′ 𝐵 (left panel) and 𝜙 ′ 𝐵 (right panel). Following parameters are adopted: 𝑎LP = 104 , 𝑎CP = 𝑎LP/ √ 2, and 𝜔′ 𝐵 /𝜔′ = 35 [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Same as [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Scattering optical depth 𝜏 as a function of 𝛾 and 𝜃𝐵 for X-mode (left), O-mode (middle), and circularly polarized waves (right), computed for 𝑎LP = 104 (𝑎CP = 𝑎LP/ √ 2) and 𝜔′ 𝐵 /𝜔′ = 35. Black solid curves denote 𝜏 = 1, dashed curves correspond to 𝜏 = 10−2 , 10−4 , and 10−6 , as labeled. The optical depth decreases outside each contour curve, i.e., regions enclosed by a given curve correspond to optical d… view at source ↗
read the original abstract

Fast Radio Bursts (FRBs) are millisecond-duration radio transients that are widely believed to originate within magnetar magnetospheres. Large-amplitude radio waves associated with FRBs propagate through strongly magnetized plasmas, where nonlinear scattering can affect their propagation. By solving the relativistic motion of a single particle interacting with electromagnetic waves of arbitrary polarization and propagation angle $\theta_B$, we compute the scattering cross section and the corresponding optical depth. The scattering cross section of the O-mode can exceed that of the X-mode when $a\sin\theta_B < \omega_B/\omega$, and becomes comparable to that of the X-mode when $a\sin\theta_B > \omega_B/\omega$, where $\theta_B$ is the angle between the wave vector and the background field. In the strongly magnetized and quasi-parallel limits, the cross sections asymptotically recover the linear regime scalings and are strongly suppressed by relativistic particle motion, leading to optical depths well below unity. We also show that curvature radiation losses of O-mode waves are strongly suppressed for quasi-parallel propagation, allowing them to escape from the magnetosphere at moderate multiplicities. We propose that Alfv\'en waves excited by magnetar crust quakes can reach amplitudes comparable to the background magnetic field, thus straightening field lines and reducing $\theta_B$. This geometrical alignment enhances the ability of FRBs to freely propagate through the open field line region. These results suggest that large-amplitude waves propagating quasi-parallel to open magnetic field lines can avoid significant single-particle scattering losses, providing a possible condition for their escape.

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 paper solves the relativistic Lorentz force for a single charged particle interacting with arbitrarily polarized strong electromagnetic waves at angle θ_B to a background magnetic field B_0. From the resulting particle trajectories it extracts the time-averaged scattering cross sections σ_O and σ_X (and the associated optical depths) as functions of wave amplitude a, frequency ω, and magnetization parameter ω_B/ω. In the strongly magnetized (ω_B ≫ ω) and quasi-parallel (θ_B small) limits the cross sections recover the known linear-regime scalings and are further suppressed by relativistic particle motion, yielding τ ≪ 1. Curvature-radiation losses for the O-mode are likewise shown to be suppressed at small θ_B. The authors propose that Alfvén waves excited by magnetar crust quakes can reach amplitudes a ∼ 1, thereby straightening open field lines, reducing θ_B, and permitting FRB escape.

Significance. If the single-particle derivation is correct, the work supplies a concrete, parameter-free mechanism by which large-amplitude radio waves can avoid significant scattering losses when propagating quasi-parallel to open magnetar field lines. The direct extraction of cross sections from the Lorentz-force trajectory (rather than from a fitted model) is a methodological strength. The final implication for FRB escape, however, rests on an unquantified auxiliary assumption whose removal would leave only the more limited statement that scattering is suppressed for sufficiently small θ_B.

major comments (2)
  1. [Abstract, §5] Abstract (final paragraph) and §5 (implications): the statement that “Alfvén waves excited by magnetar crust quakes can reach amplitudes comparable to the background magnetic field” is invoked to reduce θ_B and thereby enable escape, yet no amplitude estimate, energy budget, or propagation calculation is supplied. This assumption is load-bearing for the central claim that FRBs “can avoid significant single-particle scattering losses.”
  2. [§3] §3 (cross-section derivation): while the asymptotic recovery of linear scalings is stated, the manuscript provides neither an explicit numerical check against the known linear cross sections at a ≪ 1 nor an error analysis or comparison to full kinetic simulations. Because the suppression result is the load-bearing quantitative claim, such verification is required to establish the accuracy of the nonlinear expressions.
minor comments (1)
  1. [§3] Notation for the wave amplitude a and the angle θ_B should be defined once at first use and used consistently; several equations in §3 introduce auxiliary quantities (e.g., the effective E_p) without immediate reference back to the Lorentz-force equation.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful and constructive review. We respond point-by-point to the major comments below.

read point-by-point responses

  1. Referee: [Abstract, §5] Abstract (final paragraph) and §5 (implications): the statement that “Alfvén waves excited by magnetar crust quakes can reach amplitudes comparable to the background magnetic field” is invoked to reduce θ_B and thereby enable escape, yet no amplitude estimate, energy budget, or propagation calculation is supplied. This assumption is load-bearing for the central claim that FRBs “can avoid significant single-particle scattering losses.”

    Authors: We agree that the Alfvén-wave proposal is presented without supporting amplitude or energy-budget calculations. The statement is offered as a physically motivated hypothesis rather than a derived result. In revision we will rephrase the abstract and §5 to present the mechanism as speculative, note that quantitative modeling of Alfvén-wave amplitudes lies outside the present scope, and explicitly state that the scattering-suppression result for small θ_B is independent of this hypothesis. revision: yes

  2. Referee: [§3] §3 (cross-section derivation): while the asymptotic recovery of linear scalings is stated, the manuscript provides neither an explicit numerical check against the known linear cross sections at a ≪ 1 nor an error analysis or comparison to full kinetic simulations. Because the suppression result is the load-bearing quantitative claim, such verification is required to establish the accuracy of the nonlinear expressions.

    Authors: We accept that an explicit numerical verification would strengthen the presentation. We will add to the revised §3 a direct comparison of the computed σ_O and σ_X against the known linear-regime analytic expressions for a ≪ 1, including a quantitative assessment of agreement across the relevant parameter space. A comparison against full kinetic simulations is beyond the scope of the single-particle Lorentz-force calculation performed here. revision: yes

Circularity Check

0 steps flagged

No significant circularity; cross sections derived from particle trajectory equations

full rationale

The paper obtains scattering cross sections by directly solving the relativistic single-particle motion equation for arbitrary wave polarization and angle θ_B, then computes optical depths from those expressions. This chain is self-contained and does not reduce to fitted inputs, self-citations, or ansatzes imported from prior work by the same authors. The Alfvén-wave straightening step is explicitly labeled a proposal in the abstract and does not serve as a load-bearing premise for the computed cross sections or optical-depth results. No renaming of known results or uniqueness theorems invoked via self-citation appear in the derivation.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 1 invented entities

The central claim rests on the relativistic single-particle Lorentz equation plus standard cold-plasma dispersion for O/X modes; the escape condition additionally invokes an unquantified Alfvén-wave amplitude from crust quakes.

axioms (2)
  • standard math Relativistic equation of motion for a charged particle in combined background B and wave E,B fields is solved exactly for arbitrary polarization and θ_B.
    Invoked in the first sentence of the abstract as the starting point for the cross-section calculation.
  • domain assumption O-mode and X-mode are the relevant cold-plasma eigenmodes in strongly magnetized plasma.
    Used without derivation when comparing cross sections of the two modes.
invented entities (1)
  • Alfvén waves excited by magnetar crust quakes that reach amplitudes comparable to the background magnetic field no independent evidence
    purpose: Straighten field lines and reduce θ_B to enable quasi-parallel propagation
    Introduced in the final paragraph of the abstract as a proposed mechanism; no independent evidence or amplitude estimate supplied.

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discussion (0)

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Reference graph

Works this paper leans on

212 extracted references · 193 canonical work pages · 50 internal anchors

  1. [1]

    FRB 121102 Bursts Show Complex Time-Frequency Structure

    FRB 121102 Bursts Show Complex Time-Frequency Structure. , keywords =. doi:10.3847/2041-8213/ab13ae , archivePrefix =. 1811.10748 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/ab13ae 2041

  2. [2]

    , keywords =

    Global Kinetic Simulations of Monster Shocks and Their Emission. , keywords =. doi:10.1103/y9p7-1zms , archivePrefix =. 2506.04175 , primaryClass =

    work page doi:10.1103/y9p7-1zms

  3. [3]

    , keywords =

    Bright Bursts with Submillisecond Structures of FRB 20230607A in a Highly Magnetized Environment. , keywords =. doi:10.3847/1538-4357/addfdb , archivePrefix =. 2504.11173 , primaryClass =

    work page doi:10.3847/1538-4357/addfdb

  4. [4]

    , keywords =

    Investigating FRB 20240114A with FAST: Morphological Classification and Drifting Rate Measurements in a Burst-cluster Framework. , keywords =. doi:10.3847/1538-4357/ae314a , archivePrefix =. 2507.14711 , primaryClass =

    work page doi:10.3847/1538-4357/ae314a

  5. [5]

    , keywords =

    Magnetospheric origin of a fast radio burst constrained using scintillation. , keywords =. doi:10.1038/s41586-024-08297-w , archivePrefix =. 2406.11053 , primaryClass =

    work page doi:10.1038/s41586-024-08297-w

  6. [6]

    , keywords =

    Monster Radiative Shocks in the Perturbed Magnetospheres of Neutron Stars. , keywords =. doi:10.3847/1538-4357/acf659 , archivePrefix =. 2210.13509 , primaryClass =

    work page doi:10.3847/1538-4357/acf659

  7. [7]

    Conversion Measure of Faraday Rotation-Conversion with application to Fast Radio Bursts

    Conversion Measure of Faraday Rotation-Conversion with Application to Fast Radio Bursts. , keywords =. doi:10.3847/1538-4357/ab0fa3 , archivePrefix =. 1902.01485 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab0fa3 1902

  8. [8]

    Classical Electrodynamics, 3rd Edition

  9. [9]

    Radiative processes in astrophysics

  10. [10]

    A bright millisecond radio burst of extragalactic origin

    A Bright Millisecond Radio Burst of Extragalactic Origin. Science , keywords =. doi:10.1126/science.1147532 , archivePrefix =. 0709.4301 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.1147532

  11. [11]

    A Population of Fast Radio Bursts at Cosmological Distances

    A Population of Fast Radio Bursts at Cosmological Distances. Science , keywords =. doi:10.1126/science.1236789 , archivePrefix =. 1307.1628 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.1236789

  12. [12]

    The direct localization of a fast radio burst and its host

    A direct localization of a fast radio burst and its host. , keywords =. doi:10.1038/nature20797 , archivePrefix =. 1701.01098 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature20797

  13. [13]

    A single fast radio burst localized to a massive galaxy at cosmological distance

    A single fast radio burst localized to a massive galaxy at cosmological distance. Science , keywords =. doi:10.1126/science.aaw5903 , archivePrefix =. 1906.11476 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.aaw5903 1906

  14. [14]

    Fast Radio Burst Discovered in the Arecibo Pulsar ALFA Survey

    Fast Radio Burst Discovered in the Arecibo Pulsar ALFA Survey. , keywords =. doi:10.1088/0004-637X/790/2/101 , archivePrefix =. 1404.2934 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/790/2/101

  15. [15]

    FRBCAT: The Fast Radio Burst Catalogue

    FRBCAT: The Fast Radio Burst Catalogue. , keywords =. doi:10.1017/pasa.2016.35 , archivePrefix =. 1601.03547 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1017/pasa.2016.35 2016

  16. [16]

    A Multi-telescope Campaign on FRB 121102: Implications for the FRB Population

    A Multi-telescope Campaign on FRB 121102: Implications for the FRB Population. , keywords =. doi:10.3847/1538-4357/aa9700 , archivePrefix =. 1705.07553 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa9700

  17. [17]

    , year = 1969, month = dec, volume =

    Generation and Transfer of Polarized Synchrotron Radiation. , year = 1969, month = dec, volume =

    1969

  18. [18]

    An extreme magneto-ionic environment associated with the fast radio burst source FRB 121102

    An extreme magneto-ionic environment associated with the fast radio burst source FRB 121102. , keywords =. doi:10.1038/nature25149 , archivePrefix =. 1801.03965 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature25149

  19. [19]

    , keywords =

    CHIME/FRB Discovery of Eight New Repeating Fast Radio Burst Sources. , keywords =. doi:10.3847/2041-8213/ab4a80 , archivePrefix =. 1908.03507 , primaryClass =

    work page doi:10.3847/2041-8213/ab4a80 2041

  20. [20]

    Event rate density

    On the FRB luminosity function - - II. Event rate density. , keywords =. doi:10.1093/mnras/staa704 , archivePrefix =. 2003.04848 , primaryClass =

    work page doi:10.1093/mnras/staa704 2003

  21. [21]

    Faraday conversion and magneto-ionic variations in Fast Radio Bursts

    Faraday conversion and magneto-ionic variations in fast radio bursts. , keywords =. doi:10.1093/mnrasl/slz038 , archivePrefix =. 1812.07889 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/slz038

  22. [22]

    Faraday rotation: effect of magnetic field reversals

    Faraday Rotation: Effect of Magnetic Field Reversals. , keywords =. doi:10.1088/0004-637X/725/2/1600 , archivePrefix =. 1010.3442 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/725/2/1600

  23. [23]

    T., Zhang, B., et al

    Polarization changes of pulsars due to wave propagation through magnetospheres. , keywords =. doi:10.1111/j.1365-2966.2009.16074.x , archivePrefix =. 0910.2793 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.16074.x 2009

  24. [24]

    Single stars

    Cyclotron absorption of radio emission within pulsar magnetospheres. , keywords =. doi:10.1046/j.1365-8711.2001.04402.x , adsurl =

    work page doi:10.1046/j.1365-8711.2001.04402.x 2001

  25. [25]

    Toward an Empirical Theory of Pulsar Emission. V. On the Circular Polarization in Pulsar Radiation. , keywords =. doi:10.1086/168531 , adsurl =

    work page doi:10.1086/168531

  26. [26]

    , keywords =

    A theory of subpulse polarization patterns from radio pulsars. , keywords =. doi:10.1086/156959 , adsurl =

    work page doi:10.1086/156959

  27. [27]

    , keywords =

    Polarization transfer in a pulsar magnetosphere. , keywords =. doi:10.1111/j.1365-2966.2005.09941.x , archivePrefix =. astro-ph/0512140 , primaryClass =

    work page doi:10.1111/j.1365-2966.2005.09941.x 2005

  28. [28]

    , keywords =

    Faraday depolarization and induced circular polarization by multipath propagation with application to FRBs. , keywords =. doi:10.1093/mnras/stab3730 , archivePrefix =. 2110.00028 , primaryClass =

    work page doi:10.1093/mnras/stab3730

  29. [29]

    , keywords =

    FRB coherent emission from decay of Alfv \'e n waves. , keywords =. doi:10.1093/mnras/staa774 , archivePrefix =. 2004.00644 , primaryClass =

    work page doi:10.1093/mnras/staa774 2004

  30. [30]

    Fast radio burst source properties and curvature radiation model

    Fast radio burst source properties and curvature radiation model. , keywords =. doi:10.1093/mnras/stx665 , archivePrefix =. 1703.06139 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx665

  31. [31]

    Bunching Coherent Curvature Radiation in Three-Dimensional Magnetic Field Geometry: Application to Pulsars and Fast Radio Bursts

    Bunching Coherent Curvature Radiation in Three-dimensional Magnetic Field Geometry: Application to Pulsars and Fast Radio Bursts. , keywords =. doi:10.3847/1538-4357/aae685 , archivePrefix =. 1712.02702 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aae685

  32. [32]

    , keywords =

    Pair Separation in Parallel Electric Field in Magnetar Magnetosphere and Narrow Spectra of Fast Radio Bursts. , keywords =. doi:10.3847/2041-8213/abb535 , archivePrefix =. 2006.03270 , primaryClass =

    work page doi:10.3847/2041-8213/abb535 2041

  33. [33]

    A model for fast extragalactic radio bursts

    A model for fast extragalactic radio bursts. , keywords =. doi:10.1093/mnrasl/slu046 , archivePrefix =. 1401.6674 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/slu046

  34. [34]

    A flaring magnetar in FRB 121102?

    A Flaring Magnetar in FRB 121102?. , keywords =. doi:10.3847/2041-8213/aa78f3 , archivePrefix =. 1702.08644 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aa78f3 2041

  35. [35]

    , keywords =

    Blast Waves from Magnetar Flares and Fast Radio Bursts. , keywords =. doi:10.3847/1538-4357/ab83eb , archivePrefix =. 1908.07743 , primaryClass =

    work page doi:10.3847/1538-4357/ab83eb 1908

  36. [36]

    The synchrotron maser emission from relativistic shocks in Fast Radio Bursts: 1D PIC simulations of cold pair plasmas

    The synchrotron maser emission from relativistic shocks in Fast Radio Bursts: 1D PIC simulations of cold pair plasmas. , keywords =. doi:10.1093/mnras/stz640 , archivePrefix =. 1901.01029 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz640 1901

  37. [37]

    Fast radio bursts as synchrotron maser emission from decelerating relativistic blast waves

    Fast radio bursts as synchrotron maser emission from decelerating relativistic blast waves. , keywords =. doi:10.1093/mnras/stz700 , archivePrefix =. 1902.01866 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz700 1902

  38. [38]

    Magnetospheric eclipses in the double pulsar system J0737-3039

    Magnetospheric Eclipses in the Double-Pulsar System PSR J0737-3039. , keywords =. doi:10.1086/432248 , archivePrefix =. astro-ph/0412355 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/432248

  39. [39]

    , keywords =

    Propagation-induced Circular Polarisation in Synchrotron Sources. , keywords =. doi:10.1071/AS98211 , adsurl =

    work page doi:10.1071/as98211

  40. [40]

    Proceedings of the Royal Society of London Series A , year = 1935, month = jun, volume =

    The Application of the Magneto-Ionic Theory to the Ionosphere. Proceedings of the Royal Society of London Series A , year = 1935, month = jun, volume =. doi:10.1098/rspa.1935.0101 , adsurl =

    work page doi:10.1098/rspa.1935.0101 1935

  41. [41]

    , year = 1960, month = may, volume =

    Magnetoionic Mode Coupling at High Frequencies. , year = 1960, month = may, volume =. doi:10.1086/146878 , adsurl =

    work page doi:10.1086/146878 1960

  42. [42]

    , year = 1969, month = aug, volume =

    Pulsar Electrodynamics. , year = 1969, month = aug, volume =. doi:10.1086/150119 , adsurl =

    work page doi:10.1086/150119 1969

  43. [43]

    , keywords =

    A unified picture of Galactic and cosmological fast radio bursts. , keywords =. doi:10.1093/mnras/staa2450 , archivePrefix =. 2005.06736 , primaryClass =

    work page doi:10.1093/mnras/staa2450 2005

  44. [44]

    , keywords =

    Coherent Inverse Compton Scattering by Bunches in Fast Radio Bursts. , keywords =. doi:10.3847/1538-4357/ac3979 , archivePrefix =. 2111.06571 , primaryClass =

    work page doi:10.3847/1538-4357/ac3979

  45. [45]

    Electromagnetic Processes in Dispersive Media

  46. [46]

    , keywords =

    Can a Strong Radio Burst Escape the Magnetosphere of a Magnetar?. , keywords =. doi:10.3847/2041-8213/ac2fa0 , archivePrefix =. 2108.07881 , primaryClass =

    work page doi:10.3847/2041-8213/ac2fa0 2041

  47. [47]

    Sitzungsberichte der K

    \"U ber das Gravitationsfeld eines Massenpunktes nach der Einsteinschen Theorie. Sitzungsberichte der K

  48. [48]

    Nature Astronomy , keywords =

    HXMT identification of a non-thermal X-ray burst from SGR J1935+2154 and with FRB 200428. Nature Astronomy , keywords =

  49. [49]

    The classical theory of fields

  50. [50]

    , keywords =

    The plasma suppression effect can be ignored in realistic FRB models invoking bunched coherent radio emission. , keywords =. doi:10.1093/mnras/stac3111 , archivePrefix =. 2111.12269 , primaryClass =

    work page doi:10.1093/mnras/stac3111

  51. [51]

    , year = 1969, month = aug, volume =

    Coherent Mechanisms of Radio Emission and Magnetic Models of Pulsars. , year = 1969, month = aug, volume =. doi:10.1007/BF00651351 , adsurl =

    work page doi:10.1007/bf00651351 1969

  52. [52]

    On the radiation mechanism of repeating fast radio bursts

    On the radiation mechanism of repeating fast radio bursts. , keywords =. doi:10.1093/mnras/sty716 , archivePrefix =. 1710.10270 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty716

  53. [53]

    , keywords =

    A bright millisecond-duration radio burst from a Galactic magnetar. , keywords =. doi:10.1038/s41586-020-2863-y , archivePrefix =. 2005.10324 , primaryClass =

    work page doi:10.1038/s41586-020-2863-y 2005

  54. [54]

    Nature Physical Science , year = 1972, month = dec, volume =

    Lorentz Transformation Properties of the Stokes Parameters. Nature Physical Science , year = 1972, month = dec, volume =. doi:10.1038/physci240161b0 , adsurl =

    work page doi:10.1038/physci240161b0 1972

  55. [55]

    Nature Astronomy , keywords =

    An X-ray burst from a magnetar enlightening the mechanism of fast radio bursts. Nature Astronomy , keywords =. doi:10.1038/s41550-020-01276-x , archivePrefix =. 2005.12164 , primaryClass =

    work page doi:10.1038/s41550-020-01276-x 2005

  56. [56]

    Nature Astronomy , keywords =

    A peculiar hard X-ray counterpart of a Galactic fast radio burst. Nature Astronomy , keywords =. doi:10.1038/s41550-020-01265-0 , archivePrefix =. 2005.11178 , primaryClass =

    work page doi:10.1038/s41550-020-01265-0 2005

  57. [57]

    , keywords =

    A fast radio burst associated with a Galactic magnetar. , keywords =. doi:10.1038/s41586-020-2872-x , archivePrefix =. 2005.10828 , primaryClass =

    work page doi:10.1038/s41586-020-2872-x 2005

  58. [58]

    , keywords =

    INTEGRAL Discovery of a Burst with Associated Radio Emission from the Magnetar SGR 1935+2154. , keywords =. doi:10.3847/2041-8213/aba2cf , archivePrefix =. 2005.06335 , primaryClass =

    work page doi:10.3847/2041-8213/aba2cf 1935

  59. [59]

    , year = 2022, month = sep, volume =

    A fast radio burst source at a complex magnetized site in a barred galaxy. , year = 2022, month = sep, volume =. doi:10.1038/s41586-022-05071-8 , adsurl =

    work page doi:10.1038/s41586-022-05071-8 2022

  60. [60]

    The Astronomer's Telegram , keywords =

    Recent high activity from a repeating Fast Radio Burst discovered by CHIME/FRB. The Astronomer's Telegram , keywords =

  61. [61]

    arXiv e-prints , keywords =

    Circularly polarized radio emission from the repeating fast radio burst source FRB 20201124A. arXiv e-prints , keywords =

  62. [62]

    , keywords =

    The physical mechanisms of fast radio bursts. , keywords =. doi:10.1038/s41586-020-2828-1 , archivePrefix =. 2011.03500 , primaryClass =

    work page doi:10.1038/s41586-020-2828-1 2011

  63. [63]

    Celotti and G

    Wave modes in the magnetospheres of pulsars and magnetars. , keywords =. doi:10.1111/j.1365-2966.2007.11531.x , archivePrefix =. astro-ph/0611924 , primaryClass =

    work page doi:10.1111/j.1365-2966.2007.11531.x 2007

  64. [64]

    Resonant Conversion of Photon Modes Due to Vacuum Polarization in a Magnetized Plasma: Implications for X-Ray Emission from Magnetars

    Resonant Conversion of Photon Modes Due to Vacuum Polarization in a Magnetized Plasma: Implications for X-Ray Emission from Magnetars. , keywords =. doi:10.1086/338074 , archivePrefix =. astro-ph/0108127 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/338074

  65. [65]

    An inverse Compton scattering (ICS) model of pulsar emission. I. Core and conal emission beams. , keywords =

  66. [66]

    , keywords =

    Constraints on the engines of fast radio bursts. , keywords =. doi:10.1093/mnras/staa1036 , archivePrefix =. 1911.05765 , primaryClass =

    work page doi:10.1093/mnras/staa1036 1911

  67. [67]

    High-energy radiation from magnetized neutron stars

  68. [68]

    , keywords =

    Plasmoid Ejection by Alfv \'e n Waves and the Fast Radio Bursts from SGR 1935+2154. , keywords =. doi:10.3847/2041-8213/abafa8 , archivePrefix =. 2006.04649 , primaryClass =

    work page doi:10.3847/2041-8213/abafa8 1935

  69. [69]

    A., Primack, J

    Atmosphere models of magnetized neutron stars: QED effects, radiation spectra and polarization signals. , keywords =. doi:10.1111/j.1365-2966.2006.11098.x , archivePrefix =. astro-ph/0607168 , primaryClass =

    work page doi:10.1111/j.1365-2966.2006.11098.x 2006

  70. [70]

    , keywords =

    Wave Propagation in Pulsar Magnetospheres: Dispersion Relations and Normal Modes of Plasmas in Superstrong Magnetic Fields. , keywords =. doi:10.1086/163978 , adsurl =

    work page doi:10.1086/163978

  71. [71]

    An Inverse Compton Scattering Model of Pulsar Emission. III. Polarization. , keywords =. doi:10.1086/308824 , archivePrefix =. astro-ph/9911253 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/308824

  72. [72]

    , keywords =

    Transparency of fast radio burst waves in magnetar magnetospheres. , keywords =. doi:10.1093/mnras/stac1910 , archivePrefix =. 2204.10953 , primaryClass =

    work page doi:10.1093/mnras/stac1910

  73. [73]

    Repeating Fast Radio Bursts from Magnetars with Low Magnetospheric Twist

    Repeating Fast Radio Bursts from Magnetars with Low Magnetospheric Twist. , keywords =. doi:10.3847/1538-4357/ab2240 , archivePrefix =. 1904.12036 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab2240 1904

  74. [74]

    Circular Polarization in Pulsars due to Curvature Radiation

    Circular Polarization in Pulsars Due to Curvature Radiation. , keywords =. doi:10.1088/0004-637X/710/1/29 , archivePrefix =. 1001.2671 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/710/1/29

  75. [75]

    , keywords =

    Magnetospheric Curvature Radiation by Bunches as Emission Mechanism for Repeating Fast Radio Bursts. , keywords =. doi:10.3847/1538-4357/ac4097 , archivePrefix =. 2111.11841 , primaryClass =

    work page doi:10.3847/1538-4357/ac4097

  76. [76]

    Research in Astronomy and Astrophysics , keywords =

    Circular Polarization of Fast Radio Bursts in the Curvature Radiation Scenario. Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/ac71a5 , archivePrefix =. 2202.05475 , primaryClass =

    work page doi:10.1088/1674-4527/ac71a5

  77. [77]

    , keywords =

    Pulsar emission as curvature-generated polarized shot noise. , keywords =

  78. [78]

    , keywords =

    A bimodal burst energy distribution of a repeating fast radio burst source. , keywords =. doi:10.1038/s41586-021-03878-5 , archivePrefix =. 2107.08205 , primaryClass =

    work page doi:10.1038/s41586-021-03878-5

  79. [79]

    Physics of the Interstellar and Intergalactic Medium

  80. [80]

    , keywords =

    Propagation of Alfv \'e n waves in the charge starvation regime. , keywords =. doi:10.1093/mnras/stac2446 , adsurl =

    work page doi:10.1093/mnras/stac2446

Showing first 80 references.