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In models of galaxy formation, feedback driven both by supernova (SN) andactive galactic nucleus (AGN) is not efficient enough to quench star formationin massive galaxies. Models of smaller galaxies have suggested that cosmic rays(CRs) play a major role in expelling material from the star forming regions bydiffusing SN energy to the lower density outskirts. We therefore run gasdynamical simulations of galactic outflows from a galaxy contained in a halowith $5\times10^{12}$~M$_{\odot}$ that resembles a local ultraluminous galaxy,including both SN thermal energy and a treatment of CRs using the samediffusion approximation as Salem & Bryan. We find that CR pressure drives alow-density bubble beyond the edge of the shell swept up by thermal pressure,but the main bubble driven by SN thermal pressure overtakes it later, whichcreates a large-scale biconical outflow. CRs diffusing into the disk are unableto entrain its gas in the outflows, yielding a mass-loading rate of only$\sim0.1~\%$ with varied CR diffusion coefficients. We find no significantdifference in mass-loading rates in SN driven outflows with or without CRpressure. Our simulations strongly suggest that it is hard to drive a heavilymass-loaded outflow with CRs from a massive halo potential, although moredistributed star formation could lead to a different result.

Cosmic Ray Driven Outflows in an Ultraluminous Galaxy