Skip to content
DraconiticResearch
Search Sources API
197,768 studies31 sourcesUpdated just now
PreprintCC BY 4.0arXiv

Interaction of Strong X-mode Waves with Magnetized Pair Plasmas

Abstract

The interaction of strong (a0>1), superluminal X-mode electromagnetic waves with magnetized pair plasma falls into two regimes set by εB≡ a0ωB/ω0, the ratio of the wave strength parameter to its frequency, in units of cyclotron frequency. For εB<1 the wave propagates until induced scattering disrupts it. Using analytical theory and kinetic simulations, we show that the background magnetic field introduces a restoring frequency ΩB to scattering; when ΩB exceeds the scattering rate, the unattenuated length grows from ≃εp−2/3 to ≃εB1/2/εp wavelengths (εp≡ a0ωp/ω0; ωp is the plasma frequency). When a02>εB>1, the plasma current is nonlinear, and the wave is damped while riding a motional electric field, so one half-cycle appears attenuated. This framework has implications for the duration of fast radio bursts and whether they can escape their surroundings.

Related

  1. Rapid Energy Dissipation by Colliding Waves in Strongly Magnetized Plasmas
    Tianshu Wu, Xinyu Li, Yangyang Cai
    arXivPreprintarXiv licenceFull textHigh-energy astrophysicsPlasma physicsarXiv
  2. Evolution of Jeans instability in nonthermal magnetized complex plasmas
    Dipankar Ray, Pralay Kumar Karmakar, Bharati Kakad +1
    arXivPreprintarXiv licenceFull textHigh-energy astrophysicsSolar & stellar physicsarXiv
  3. Revisiting damping of Alfvén waves in partially ionized plasmas
    Yutaka Ohira
    arXivPreprintCC BY 4.0Full textHigh-energy astrophysicsarXiv
  4. Linear Mode Conversion Theory of Radio Emission from Turbulent Solar Wind Plasmas
    C. Krafft, A S Volokitin
    The Astrophysical Journal Supplement SeriesPeer-reviewedCC BY 4.0Full text2 citedSolar & stellar physicsComputational physicsHAL
  5. Non-linear dynamo waves in magnetized shear flows: a candidate mechanism for the solar cycle
    Uddipan Banik
    arXivPreprintCC BY 4.0Full textHigh-energy astrophysicsPlanetary science & exoplanetsarXiv
BibTeX
@misc{sridhar2026interaction,
  title = {{Interaction of Strong X-mode Waves with Magnetized Pair Plasmas}},
  author = {Navin Sridhar},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.35849},
  eprint = {2610.35849},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.35849},
  note = {CC BY 4.0},
}
RIS
TY  - UNPB
TI  - Interaction of Strong X-mode Waves with Magnetized Pair Plasmas
AU  - Navin Sridhar
PY  - 2026
DA  - 2026/10/26
PB  - arXiv
DO  - 10.48550/arxiv.2610.35849
UR  - https://arxiv.org/abs/2610.35849
AB  - The interaction of strong (a_0>1), superluminal X-mode electromagnetic waves with magnetized pair plasma falls into two regimes set by ε_B≡ a_0ω_B/ω_0, the ratio of the wave strength parameter to its frequency, in units of cyclotron frequency. For ε_B<1 the wave propagates until induced scattering disrupts it. Using analytical theory and kinetic simulations, we show that the background magnetic field introduces a restoring frequency Ω_B to scattering; when Ω_B exceeds the scattering rate, the unattenuated length grows from ≃ε_p^−2/3 to ≃ε_B^1/2/ε_p wavelengths (ε_p≡ a_0ω_p/ω_0; ω_p is the plasma frequency). When a_0^2>ε_B>1, the plasma current is nonlinear, and the wave is damped while riding a motional electric field, so one half-cycle appears attenuated. This framework has implications for the duration of fast radio bursts and whether they can escape their surroundings.
ER  -