Speaker
Description
Supernova remnants are considered major contributors to the Galactic cosmic-ray population. However, many existing numerical models of particle acceleration at the remnants shocks still rely on over-simplified geometries that cannot reproduce the rich and asymmetric emission morphologies that many remnants show on account of their interaction with their inhomogeneous surroundings.
In this talk we present a way to address this limitation, thanks to a new addition to our RATPaC code, where we split-up the geometry of the remnant into cones, assuming a piecewise spherical symmetry. As a consequence, we solve the coupled system of hydrodynamics, cosmic-ray transport, magnetic fields, and turbulence in a fully time-dependent manner for each cone. This makes RATPaC a powerful tool for studying supernova remnants and cosmic-ray sources in the area in high-resolution astronomy, especially in the face of the upcoming CTAO.
We will describe the new feature and code architecture and we will show the first applications of it to both simulated data and observed data, such as that of SN1987A. We think that this 3D mapping tool enriches RATPaC’s modeling capabilities by enabling systematic studies of geometry-driven effects in supernova remnants and other cosmic-ray sources.
