Particle acceleration at magnetized, relativistic turbulent shock fronts

TL;DR

This study demonstrates that turbulence in the pre-shock plasma can enable and influence particle acceleration mechanisms at relativistic, magnetized shock fronts, producing power-law energy spectra.

Contribution

First simulation study showing how pre-shock turbulence affects particle acceleration in relativistic, magnetized shocks, revealing new acceleration regimes and spectral outcomes.

Findings

Turbulence can revive particle acceleration in superluminal shocks.

Power-law spectra with index s ~ 2.5-3.5 are produced.

Stochastic acceleration can dominate at higher magnetizations.

Abstract

The efficiency of particle acceleration at shock waves in relativistic, magnetized astrophysical outflows is a debated topic with far-reaching implications. Here, for the first time, we study the impact of turbulence in the pre-shock plasma. Our simulations demonstrate that, for a mildly relativistic, magnetized pair shock (Lorentz factor $\gamma_{\rm sh} \simeq 2.7$, magnetization level $\sigma \simeq 0.01$), strong turbulence can revive particle acceleration in a superluminal configuration that otherwise prohibits it. Depending on the initial plasma temperature and magnetization, stochastic-shock-drift or diffusive-type acceleration governs particle energization, producing powerlaw spectra $\mathrm{d}N/\mathrm{d}\gamma \propto \gamma^{-s}$ with $s \sim 2.5-3.5$. At larger magnetization levels, stochastic acceleration within the pre-shock turbulence becomes competitive and can even take over shock acceleration.