On the origin of jet-like features in bow shock pulsar wind nebulae

Abstract

Bow shock pulsar wind nebulae are a large class of non-thermal synchrotron sources associated to old pulsars, that have emerged from their parent supernova remnant and are directly interacting with the interstellar medium. Within this class a few objects show extended X-ray features, generally referred as "jets", that defies all the expectations from the canonical MHD models, being strongly misaligned respect to the pulsar direction of motion. It has been suggested that these jets might originate from high energy particles that escape from the system. Here we investigate this possibility, computing particle trajectories on top of a 3D relativistic MHD model of the flow and magnetic field structure, and we show not only that beamed escape is possible, but that it can easily be asymmetric and charge separated, which as we will discuss are important aspects to explain known objects.

8 pages, 4 figures

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• Prospects for a survey of the Galactic plane with the Cherenkov Telescope Array
• A NuSTAR and Chandra Investigation of the Misaligned Outflow of PSR J1101-6101 and the Lighthouse Pulsar Wind Nebula
• A Quarter Century of Guitar Nebula/Filament Evolution
• Pulsar-wind-nebula-powered Galactic center X-ray filament G0.13-0.11: Proof of the synchrotron nature by IXPE
• A Catalog of Pulsar X-ray Filaments
• A deep X-ray spectral imaging of the bow-shock pulsar wind nebula associated with PSR B1929+10
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