On electromagnetic instabilities at ultra-relativistic shock waves

TL;DR

This paper investigates the growth of electromagnetic micro-instabilities in relativistic shock waves, analyzing how magnetic field generation influences particle acceleration and shock precursor dynamics in astrophysical environments.

Contribution

It provides a detailed calculation of growth rates for various instabilities in both magnetized and unmagnetized shocks, linking plasma physics to astrophysical phenomena.

Findings

Weibel and filamentation instabilities dominate in unmagnetized shocks.

Resonant Cerenkov modes have longer lifetimes and influence downstream magnetization.

Conditions for efficient Fermi acceleration are characterized.

Abstract

(Abridged) This paper addresses the issue of magnetic field generation in a relativistic shock precursor through micro-instabilities. The level of magnetization of the upstream plasma turns out to be a crucial parameter, notably because the length scale of the shock precursor is limited by the Larmor rotation of the accelerated particles in the background magnetic field and by the speed of the shock wave. We discuss in detail and calculate the growth rates of the following beam plasma instabilities seeded by the accelerated and reflected particle populations: for an unmagnetized shock, the Weibel and filamentation instabilities, as well as the Cerenkov resonant longitudinal and oblique modes; for a magnetized shock, the Weibel instability and the resonant Cerenkov instabilities with the longitudinal electrostatic modes, as well as the Alfven, Whisler and extraordinary modes. All these instabilities are generated upstream, then they are transmitted downstream. The modes excited by Cerenkov resonant instabilities take on particular importance with respect to the magnetisation of the downstream medium since, being plasma eigenmodes, they have a longer lifetime than the Weibel modes. We discuss the main limitation of the wave growth associated with the length of the precursor and the magnetisation of the upstream medium for both oblique and parallel shock waves. We also characterize the proper conditions to obtain Fermi acceleration. We recover some results of most recent particle-in-cell simulations and conclude with some applications to astrophysical cases of interest, pulsar winds and gamma-ray burst external shock waves in particular. (Abridged)