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We investigate the impact of gas accretion in streams on the evolution ofdisc galaxies, using magneto-hydrodynamic simulations including advection andanisotropic diffusion of cosmic rays generated by supernovae as the only sourceof feedback. Stream accretion has been suggested as an important galaxy growthmechanism in cosmological simulations and we vary their orientation and angularmomentum in idealised setups. We find that accretion streams trigger theformation of galactic rings and enhanced star formation. The star formationrates and consequently the cosmic ray driven outflow rates are higher for lowangular momentum accretion streams, which also result in more compact, lowerangular momentum discs. The cosmic ray generated outflows show a characteristicstructure. At low outflow velocities (< 50 km/s) the angular momentumdistribution is similar to the disk and the gas is in a fountain flow. Gas athigh outflow velocities (> 200 km/s), penetrating deep into the halo, has closeto zero angular momentum, and originates from the centre of the galaxies. Asthe mass loading factors of the cosmic ray driven outflows are of order unityand higher, we conclude that this process is important for the removal of lowangular momentum gas from evolving disk galaxies and the transport of,potentially metal enriched, material from galactic centres far into thegalactic haloes.

The angular momentum structure of cosmic ray driven galactic outflows triggered by stream accretion