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

Abstract

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-rays (CR) distribution function (in one momentum dimension), as first done by Falle. Following Kang and Jones and collaborators, we show how the adaptive mesh refinement technique (AMR) greatly helps accommodating the extremely demanding numerical resolution requirements of realistic (Bohm-like) CR diffusion coefficients. We also present the paral lelization 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.

accepted for publication in MNRAS by the Royal Astronomical Society and Blackwell Publishing

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Cited by in corpus (6)

• On the shape of the spectrum of cosmic-rays accelerated inside superbubbles
• p, He, and C to Fe cosmic-ray primary fluxes in diffusion models: Source and transport signatures on fluxes and ratios
• Cosmic ray acceleration at perpendicular shocks in supernova remnants
• 3D Simulations of the Thermal X-ray Emission from Young Supernova Remnants Including Efficient Particle Acceleration
• Embedded star clusters as sources of high-energy cosmic rays: Modelling and constraints
• Nonlinear particle reacceleration by multiple shocks