A global model of particle acceleration at pulsar wind termination shocks

TL;DR

This study uses large-scale simulations to reveal how the global magnetic field structure influences particle acceleration in pulsar wind nebulae, highlighting shear flows and turbulence as key mechanisms for producing high-energy particles.

Contribution

It demonstrates that large-scale anisotropic magnetic fields and downstream flow dynamics are essential for efficient particle acceleration in relativistic shocks, challenging local plane parallel models.

Findings

Efficient nonthermal particle acceleration via shear-flow mechanisms.

Spectrum hardens with increasing magnetization, similar to reconnection studies.

Formation of cavities at the shock front leads to high-energy particle surfing.

Abstract

Pulsar wind nebulae are efficient particle accelerators, and yet the processes at work remain elusive. Self-generated, microturbulence is too weak in relativistic magnetized shocks to accelerate particles over a wide energy range, suggesting that the global dynamics of the nebula may be involved in the acceleration process instead. In this work, we study the role played by the large-scale anisotropy of the transverse magnetic field profile on the shock dynamics. We performed large two-dimensional particle-in-cell simulations for a wide range of upstream plasma magnetizations. A large-scale velocity shear and current sheets form in the equatorial regions and at the poles, where they drive strong plasma turbulence via Kelvin-Helmholtz vortices and kinks. The mixing of current sheets in the downstream flow leads to efficient nonthermal particle acceleration. The power-law spectrum hardens with increasing magnetization, akin to those found in relativistic reconnection and kinetic turbulence studies. The high end of the spectrum is composed of particles surfing on the wake produced by elongated spearhead-shaped cavities forming at the shock front and piercing through the upstream flow. These particles are efficiently accelerated via the shear-flow acceleration mechanism near the Bohm limit. Magnetized relativistic shocks are very efficient particle accelerators. Capturing the global dynamics of the downstream flow is crucial to understanding them, and therefore local plane parallel studies may not be appropriate for pulsar wind nebulae and possibly other astrophysical relativistic magnetized shocks. A natural outcome of such shocks is a variable and Doppler-boosted synchrotron emission at the high end of the spectrum originating from the shock-front cavities, reminiscent of the mysterious Crab Nebula gamma-ray flares.