Electron acceleration at supernova remnants by Artem Bohdan. on Monday 28 November

Supernova remnants (SNRs) are believed to produce the majority of galactic

cosmic rays (CRs). SNRs harbor non-relativistic collisionless shocks

responsible for acceleration of CRs via diffusive shock acceleration (DSA), in

which particles gain their energies via repeated interactions with the shock

front. As the DSA theory involves pre-existing mildly energetic particles, a

means of pre-acceleration is required, especially for electrons. Electron

injection remains one of the most troublesome and still unresolved issues and

our physical understanding of it is essential to fully comprehend the physics

of SNRs. To study any electron-scale phenomena responsible for

pre-acceleration, we require a method capable of resolving these small kinetic

scales and Particle-in-cell (PIC) simulations fulfill this criterion. Here I

report on the latest achievements made by utilising kinetic simulations of

non-relativistic high Mach number shocks. I discuss how the physics of SNR

shocks depend on the shock parameters (e.g., the shock obliquity, Mach numbers,

the ion-to-electron mass ratio) as well as processes responsible for the

electron heating and acceleration.

arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.13992v1