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

¹ Institut d’Astrophysique de Paris, UMR 7095, CNRS, UPMC University of Paris VI, 98 bis boulevard Arago, 75014 Paris, France
e-mail: dubois@iap.fr
² Centre de Recherche Astrophysique de Lyon UMR5574, ENS de Lyon, Universite Lyon 1, CNRS, Université de Lyon, 69007 Lyon, France
³ Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier, CNRS/IN2P3, CC72, place Eugène Bataillon, 34095 Montpellier Cedex 5, France

Received: 9 July 2019
Accepted: 19 September 2019

Abstract

Cosmic rays (CRs) are thought to play a dynamically important role in several key aspects of galaxy evolution, including the structure of the interstellar medium, the formation of galactic winds, and the non-thermal pressure support of halos. We introduce a numerical model solving for the CR streaming instability and acceleration of CRs at shocks with a fluid approach in the adaptive mesh refinement code RAMSES. CR streaming is solved with a diffusion approach and its anisotropic nature is naturally captured. We introduce a shock finder for the RAMSES code that automatically detects shock discontinuities in the flow. Shocks are the loci for CR injection, and their efficiency of CR acceleration is made dependent on the upstream magnetic obliquity according to the diffuse shock acceleration mechanism. We show that the shock finder accurately captures shock locations and estimates the shock Mach number for several problems. The obliquity-dependent injection of CRs in the Sedov solution leads to situations where the supernova bubble exhibits large polar caps (homogeneous background magnetic field), or a patchy structure of the CR distribution (inhomogeneous background magnetic field). Finally, we combine both accelerated CRs with streaming in a simple turbulent interstellar medium box, and show that the presence of CRs significantly modifies the structure of the gas.