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Cosmic rays (CRs) are thought to play a dynamically important role in severalkey aspects of galaxy evolution, including the structure of the interstellarmedium, the formation of galactic winds, and the non-thermal pressure supportof halos. We introduce a numerical model solving for the CR streaminginstability and acceleration of CRs at shocks with a fluid approach in theadaptive mesh refinement code ramses. CR streaming is solved with a diffusionapproach and its anisotropic nature is naturally captured. We introduce a shockfinder for the ramses code that automatically detects shock discontinuities inthe flow. Shocks are the loci for CR injection, and their efficiency of CRacceleration is made dependent on the upstream magnetic obliquity according tothe diffuse shock acceleration mechanism. We show that the shock finderaccurately captures shock locations and estimates the shock Mach number forseveral problems. The obliquity-dependent injection of CRs in the Sedovsolution leads to situations where the supernova bubble exhibits large polarcaps (homogeneous background magnetic field), or a patchy structure of the CRdistribution (inhomogeneous background magnetic field). Finally, we combineboth accelerated CRs with streaming in a simple turbulent interstellar mediumbox, and show that the presence of CRs significantly modifies the structure ofthe gas.

Shock-accelerated cosmic rays and streaming instability in the adaptive mesh refinement code Ramses