marcos, a numerical tool for the simulation of multiple time-dependent non-linear diffusive shock acceleration

We present a new code aimed at the simulation of diffusive shock acceleration (DSA), and discuss various test cases which demonstrate its ability to study DSA in its full time-dependent and non-linear developments. We present the numerical methods implemented, coupling the hydrodynamical evolution o...

Full description

Saved in:
Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2008-01, Vol.383 (1), p.41-56
Main Authors: Ferrand, Gilles, Downes, Turlough, Marcowith, Alexandre
Format: Article
Language:English
Subjects:
acceleration of particles
Astronomy
Astrophysics
Cosmology and Extra-Galactic Astrophysics
Earth, ocean, space
Exact sciences and technology
Fluid dynamics
methods: numerical
Nonlinear systems
Physics
Simulation
Stars & galaxies
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:We present a new code aimed at the simulation of diffusive shock acceleration (DSA), and discuss various test cases which demonstrate its ability to study DSA in its full time-dependent and non-linear developments. We present the numerical methods implemented, coupling the hydrodynamical evolution of a parallel shock (in one space dimension) and the kinetic transport of the cosmic-ray (CR) distribution function (in one momentum dimension), as first done by Falle & Giddings. Following Kang & Jones and collaborators, we show how the adaptive mesh refinement technique greatly helps accommodating the extremely demanding numerical resolution requirements of realistic (Bohm-like) CR diffusion coefficients. We also present the parallelization of the code, which allows us to run many successive shocks at the cost of a single shock, and thus to present the first direct numerical simulations of linear and non-linear multiple DSA, a mechanism of interest in various astrophysical environments such as superbubbles, galaxy clusters and early cosmological flows.
ISSN:0035-8711
1365-2966
DOI:10.1111/j.1365-2966.2007.12511.x