The microphysics of collisionless shock waves

Abstract

Collisionless shocks, that is shocks mediated by electromagnetic processes, are customary in space physics and in astrophysics. They are to be found in a great variety of objects and environments: magnetospheric and heliospheric shocks, supernova remnants, pulsar winds and their nebulæ, active galactic nuclei, gamma-ray bursts and clusters of galaxies shock waves. Collisionless shock microphysics enters at different stages of shock formation, shock dynamics and particle energization and/or acceleration. It turns out that the shock phenomenon is a multi-scale non-linear problem in time and space. It is complexified by the impact due to high-energy cosmic rays in astrophysical environments. This review adresses the physics of shock formation, shock dynamics and particle acceleration based on a close examination of available multi-wavelength or in-situ observations, analytical and numerical developments. A particular emphasize is made on the different instabilities triggered during the shock formation and in association with particle acceleration processes with regards to the properties of the background upstream medium. It appears that among the most important parameters the background magnetic field through the magnetization and its obliquity is the dominant one. The shock velocity that can reach relativistic speeds has also a strong impact over the development of the micro-instabilities and the fate of particle acceleration. Recent developments of laboratory shock experiments has started to bring some new insights in the physics of space plasma and astrophysical shock waves. A special section is dedicated to new laser plasma experiments probing shock physics

This is an author-created, un-copyedited version of an article accepted for publication/published in Reports on progress in physics. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at 10.1088/0034-4885/79/4/046901

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• Jitter radiation: towards TeV-photons of gamma-ray bursts
• Particle acceleration and pitch-angle evolution in relativistic turbulence
• Unveiling the Magnetic Structure of VHE SNRs/PWNe with XIPE, the X-ray Imaging-Polarimetry Satellite
• Energy partition in collisionless counterstreaming plasmas
• Fermi acceleration in relativistic collisionless plasma shocks correlates with anisotropic energy gains
• Interplay between the non-resonant streaming instability and self-generated pressure anisotropies
• Statistical analysis of interplanetary shock waves measured by a Solar Wind Analyzer and a magnetometer onboard the Solar Orbiter Mission in 2023
• Three-dimensional structure and stability of discontinuities between unmagnetized pair plasma and magnetized electron-proton plasma
• The mechanism of efficient electron acceleration at parallel non-relativistic shocks
• The structure of cluster merger shocks: turbulent width and the electron heating timescale
• Can superbubbles accelerate ultra-high energy protons?
• Distributions of particles accelerated by strong Alfvénic turbulence