Superluminal Wave Activation at Relativistic Magnetized Shocks
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| Format: | Preprint |
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2025
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| _version_ | 1866908854524051456 |
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| author | Mahlmann, Jens F. Eskildsen, Logan Vanthieghem, Arno Dai, Dawei Sironi, Lorenzo |
| author_facet | Mahlmann, Jens F. Eskildsen, Logan Vanthieghem, Arno Dai, Dawei Sironi, Lorenzo |
| contents | Fast radio bursts (FRBs) are extremely energetic radio transients, some are generated in magnetar magnetospheres and winds. Despite a growing number of observations, their emission mechanisms remain elusive. It has recently been proposed that Alfvénic perturbations can convert into superluminal O-modes at magnetized shocks and propagate downstream as a radio signal. We validate this superluminal wave activation mechanism using pair-plasma theory and particle-in-cell simulations. Theory predicts two different downstream modes: nonpropagating Alfvénic perturbations and propagating superluminal O-modes. Superluminal wave activation occurs if the frequency of upstream perturbations in the shock frame exceeds the downstream plasma frequency. 1D particle-in-cell simulations confirm wavenumber and frequency jumps across the shock for upstream perturbations with frequencies well above the plasma frequency. Our simulations model both monochromatic upstream waves and broadband spectra with the downstream plasma frequency acting like a high-pass filter for superluminal O-modes. We discuss implications for FRB generation in relativistic magnetized winds. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2512_19892 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Superluminal Wave Activation at Relativistic Magnetized Shocks Mahlmann, Jens F. Eskildsen, Logan Vanthieghem, Arno Dai, Dawei Sironi, Lorenzo High Energy Astrophysical Phenomena Solar and Stellar Astrophysics Plasma Physics Fast radio bursts (FRBs) are extremely energetic radio transients, some are generated in magnetar magnetospheres and winds. Despite a growing number of observations, their emission mechanisms remain elusive. It has recently been proposed that Alfvénic perturbations can convert into superluminal O-modes at magnetized shocks and propagate downstream as a radio signal. We validate this superluminal wave activation mechanism using pair-plasma theory and particle-in-cell simulations. Theory predicts two different downstream modes: nonpropagating Alfvénic perturbations and propagating superluminal O-modes. Superluminal wave activation occurs if the frequency of upstream perturbations in the shock frame exceeds the downstream plasma frequency. 1D particle-in-cell simulations confirm wavenumber and frequency jumps across the shock for upstream perturbations with frequencies well above the plasma frequency. Our simulations model both monochromatic upstream waves and broadband spectra with the downstream plasma frequency acting like a high-pass filter for superluminal O-modes. We discuss implications for FRB generation in relativistic magnetized winds. |
| title | Superluminal Wave Activation at Relativistic Magnetized Shocks |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics Plasma Physics |
| url | https://arxiv.org/abs/2512.19892 |