Cosmic ray acceleration at perpendicular shocks in supernova remnants

Understand

Supernova remnants (SNRs) are believed to accelerate particles up to high energies through the mechanism of diffusive shock acceleration (DSA).

• Except for direct plasma simulations, all modeling efforts must rely on a given form of the diffusion coefficient, a key parameter that embodies the interactions of energetic charged particles with the magnetic turbulence.
• The so-called Bohm limit is commonly employed.
• In this paper we revisit the question of acceleration at perpendicular shocks, by employing a realistic model of perpendicular diffusion.