The Role of Superluminal Electromagnetic Waves in Pulsar Wind Termination Shocks

TL;DR

This study uses relativistic two-fluid simulations to show how superluminal electromagnetic waves influence the structure and energy dissipation in pulsar wind termination shocks, revealing their role in shaping nebulae.

Contribution

It demonstrates the conversion of magnetic shear waves into superluminal waves at shocks and their impact on shock structure and energy dissipation in pulsar winds.

Findings

Superluminal waves form ahead of the shock, creating a precursor region.

Poynting flux dissipates via parametric instability driven by superluminal waves.

Downstream plasma becomes unmagnetized and relativistically hot.

Abstract

The dynamics of a standing shock front in a Poynting-flux dominated relativistic 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 an obliquely rotating pulsar. It is demonstrated that this wave is converted into large amplitude electromagnetic waves with superluminal phase speeds by interacting with the shock when the shock-frame frequency of the wave exceeds the proper plasma frequency. The superluminal waves propagate in the upstream, modify the shock structure substantially, and form a well-developed precursor region ahead of a subshock. Dissipation of Poynting flux occurs in the precursor as well as in the downstream region through a parametric instability driven by the superluminal waves. The Poynting flux remaining in the downstream region is carried entirely by the superluminal waves. The downstream plasma is therefore an essentially unmagnetized, relativistically hot plasma with a non-relativistic flow speed, as suggested by observations of pulsar wind nebulae.