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Fig. 14


Cosmic-ray pressure maps of the turbulent box simulation, with η0 = 0.1 and , in a thin plane within the x-plane of the middle of the box at time t = 10 Myr (top panels) and t = 20 Myr (bottom panels) for the simulation without CR streaming and without (left panels) or with (right panels) obliquity dependency for CR acceleration, and with obliquity and CR streaming (right panels). The black segments depict the orientation of the unitary magnetic vectors. The simulation without obliquity builds the CR pressure faster. The presence of the streaming instability allows for a more uniform distribution of CRs in the simulated volume.

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