Kinetic "jets" from fast moving pulsars

TL;DR

This paper explains asymmetric extended features observed in fast-moving pulsars as kinetically streaming particles escaping through magnetic reconnection, supported by 3D relativistic simulations and archival observations.

Contribution

It introduces a novel explanation for pulsar wind nebula features via magnetic reconnection and kinetic particle streaming, supported by simulations and observational evidence.

Findings

Asymmetric features depend on high ISM magnetic fields (>10 μG).

Reconnection creates magnetic bottles causing asymmetric structures.

Archival observations support the kinetic jet interpretation.

Abstract

Some fast-moving pulsars, like the Guitar and the Lighthouse, exhibit asymmetric non-thermal emission features that extend well beyond their ram pressure confined pulsar wind nebulae (PWNe). Using 3D relativistic simulations we explain these features as kinetically streaming pulsar wind particles that escaped into the interstellar medium (ISM) due to reconnection between the PWN and ISM magnetic fields. The structure of the reconnecting magnetic fields at the incoming and outgoing regions produce highly asymmetric magnetic bottles, and result in asymmetric extended features. For the features to become visible, the ISM magnetic field should be sufficiently high, $B_{\rm ISM}>10$~$\mu$G. We also discuss archival observations of PWNe displaying evidence of kinetic jets: the Dragonfly PWN (PSR J2021+3651), G327.1--1.1, and MSH 11--62, the latter two of which exhibit "snail eyes" morphologies. We suggest that in those cases the pulsar is moving along the ambient magnetic field in a frisbee-type configuration.