Résumé
Cosmic rays (CRs) are an important source of feedback in a variety of astrophysical contexts. Magneto-hydrodynamical (MHD) simulations treating CRs as a fluid have shown that how their feedback operates is strongly dependent on their transport properties such as diffusion and streaming. In this paper we introduce the numerical implementation, in the adaptive-mesh-refinement MHD code RAMSES, of the grey two-moment formulation of CR fluid dynamics, which follows the energy density and its associated three-dimensional flux. This method is tested for CR diffusion, streaming, and advection in a series of multi-dimensional tests including shocks to check the robustness and stability of this numerical two-moment CRMHD solver. We finally use the new two-moment CR implementation in a complex simulation of an isolated galactic disc producing galaxy-wide outflows launched by small-scale supernova explosions, and compare it with a previously existing one-moment formulation in the same code.