Diocotron Modes in Pulsar Magnetospheres: Charge Diffusion and Implications for Radio Emission Variability
Abstract
The diocotron instability is a non-axisymmetric plasma instability that should occur generically in the differentially rotating equatorial plane of pulsar magnetospheres. We present a series of 3D particle-in-cell (PIC) simulations of the diocotron instability in aligned and oblique pulsars. The instability grows on timescales of the rotation period and develops a strong, stable m=1 mode, corresponding to a rotating, dipolar charge asymmetry in the equatorial disk. Stochastic fluctuations in the diocotron mode amplitude and pattern speed drive cross-field diffusion that can rapidly transport charges through the closed zone toward the light cylinder. In the nonlinear stage, the m=1 mode produces electric field perturbations which can modulate the polar cap potential drop and the emission beam angle, with possible connections to pulsar variability such as nulling, periodic amplitude modulation, and drifting subpulses.
Versions
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BibTeX
@misc{goodbred2026diocotron,
title = {{Diocotron Modes in Pulsar Magnetospheres: Charge Diffusion and Implications for Radio Emission Variability}},
author = {Matthew Goodbred and Anatoly Spitkovsky},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2606.03984},
eprint = {2606.03984},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2606.03984},
}
RIS
TY - UNPB
TI - Diocotron Modes in Pulsar Magnetospheres: Charge Diffusion and Implications for Radio Emission Variability
AU - Matthew Goodbred
AU - Anatoly Spitkovsky
PY - 2026
DA - 2026/10/13
PB - arXiv
DO - 10.48550/arxiv.2606.03984
UR - https://arxiv.org/abs/2606.03984
AB - The diocotron instability is a non-axisymmetric plasma instability that should occur generically in the differentially rotating equatorial plane of pulsar magnetospheres. We present a series of 3D particle-in-cell (PIC) simulations of the diocotron instability in aligned and oblique pulsars. The instability grows on timescales of the rotation period and develops a strong, stable m=1 mode, corresponding to a rotating, dipolar charge asymmetry in the equatorial disk. Stochastic fluctuations in the diocotron mode amplitude and pattern speed drive cross-field diffusion that can rapidly transport charges through the closed zone toward the light cylinder. In the nonlinear stage, the m=1 mode produces electric field perturbations which can modulate the polar cap potential drop and the emission beam angle, with possible connections to pulsar variability such as nulling, periodic amplitude modulation, and drifting subpulses.
ER -