Understanding the physical mechanisms that control galaxy formation is a fundamental
challenge in contemporary astrophysics. Recent advances in the field of astrophysical …

To undergo diffusive shock acceleration, electrons need to be preaccelerated to increase
their energies by several orders of magnitude, else their gyroradii will be smaller than the …

Strong nonrelativistic shocks are known to accelerate particles up to relativistic energies.
However, for diffusive shock acceleration, electrons must have a highly suprathermal …

Thermal electrons have gyroradii many orders of magnitude smaller than the finite width of a
shock, thus need to be pre-accelerated before they can cross it and be accelerated by …

Electron Heating in 2D Particle-in-cell Simulations of Quasi-perpendicular Low-beta Shocks -
IOPscience Skip to content IOP Science home Accessibility Help Search Journals Journals list …

Collisionless low-Mach-number shocks are abundant in astrophysical and space plasma
environments, exhibiting complex wave activity and wave–particle interactions. In this paper …

Supernova remnants (SNRs) are believed to produce the majority of galactic cosmic rays
(CRs). SNRs harbor non-relativistic collisionless shocks responsible for the acceleration of …

Shocks are ubiquitous in astrophysical sources, many of which involve relativistic bulk
motions, leading to the formation of relativistic shocks. Such relativistic shocks have so far …

Energy dissipation in collisionless shocks is a key mechanism in various astrophysical
environments. Its nonlinear nature complicates analytical understanding and necessitates …

Collisionless shocks tend to send charged particles into the upstream, driving electric
currents through the plasma. Using kinetic particle-in-cell simulations, we investigate how …