Using PIC and PIC-MHD to investigate cosmic ray acceleration in mildly relativistic shocks

TL;DR

This paper investigates cosmic ray acceleration in mildly relativistic shocks using PIC and PIC-MHD simulations to understand ion injection rates and shock obliquity effects, extending non-relativistic studies into the relativistic regime.

Contribution

It introduces a combined PIC-MHD methodology to model large-scale shock evolution with ion injection rates dependent on local shock obliquity in the mildly relativistic regime.

Findings

Ion injection rate varies with shock obliquity in the relativistic regime.

Perpendicular shocks are less efficient for DSA at higher Lorentz factors.

The combined PIC-MHD approach enables larger, longer simulations of shock evolution.

Abstract

Astrophysical shocks create cosmic rays by accelerating charged particles to relativistic speeds. However, the relative contribution of various types of shocks to the cosmic ray spectrum is still the subject of ongoing debate. Numerical studies have shown that in the non-relativistic regime, oblique shocks are capable of accelerating cosmic rays, depending on the Alfv\'enic Mach number of the shock. We now seek to extend this study into the mildly relativistic regime. In this case, dependence of the ion reflection rate on the shock obliquity is different compared to the nonrelativistic regime. Faster relativistic shocks are perpendicular for the majority of shock obliquity angles therefore their ability to initialize efficient DSA is limited. We define the ion injection rate using fully kinetic PIC simulation where we follow the formation of the shock and determine the fraction of ions that gets involved into formation of the shock precursor in the mildly relativistic regime covering a Lorentz factor range from 1 to 3. Then, with this result, we use a combined PIC-MHD method to model the large-scale evolution of the shock with the ion injection recipe dependent on the local shock obliquity. This methodology accounts for the influence of the self-generated or pre-existing upstream turbulence on the shock obliquity which allows study substantially larger and longer simulations compared to classical hybrid techniques.