Anomalous Cosmic Rays in the Heliosheath: Simulation with a Blunt Termination Shock

We present numerical simulations modeling acceleration of ACRs at a blunt termination shock with the spiral field lines intersecting the shock multiple times. The 2‐D model includes parallel and perpendicular diffusion. Our results confirm the qualitative expectations: the nose segment of the blunt shock is inefficient to accelerate particles to ACR energies, which results in a continuing increase of the ACR flux and a gradual unfolding of the ACR spectrum behind the shock, as seen by Voyager‐1. We also present a simple analytically tractable test‐case to illustrate physical effects at a 2‐D shock with a structure along the shock‐front.