English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The dynamics of a standing shock front in a Poynting-flux dominatedrelativistic flow is investigated by using a one-dimensional, relativistic,two-fluid simulation. An upstream flow containing a circularly polarized,sinusoidal magnetic shear wave is considered, mimicking a wave driven by anobliquely rotating pulsar. It is demonstrated that this wave is converted intolarge amplitude electromagnetic waves with superluminal phase speeds byinteracting with the shock when the shock-frame frequency of the wave exceedsthe proper plasma frequency. The superluminal waves propagate in the upstream,modify the shock structure substantially, and form a well-developed precursorregion ahead of a subshock. Dissipation of Poynting flux occurs in theprecursor as well as in the downstream region through a parametric instabilitydriven by the superluminal waves. The Poynting flux remaining in the downstreamregion is carried entirely by the superluminal waves. The downstream plasma istherefore an essentially unmagnetized, relativistically hot plasma with anon-relativistic flow speed, as suggested by observations of pulsar windnebulae.

The Role of Superluminal Electromagnetic Waves in Pulsar Wind Termination Shocks