We study the effects of cosmic rays (CRs) on outflows from star-forming galaxies in the circum and inter-galactic medium (CGM/IGM), in high-resolution, fully-cosmological FIRE-2 simulations (accounting for mechanical and radiative stellar feedback, magnetic fields, anisotropic conduction/viscosity/CR diffusion and streaming, and CR losses). We showed previously that massive ($M_{rm halo}gtrsim 10^{11},M_{odot}$), low-redshift ($zlesssim 1-2$) halos can have CR pressure dominate over thermal CGM pressure and balance gravity, giving rise to a cooler CGM with an equilibrium density profile. This dramatically alters outflows. Absent CRs, high gas thermal pressure in massive halos traps galactic outflows near the disk, so they recycle. With CRs injected in supernovae as modeled here, the low-pressure halo allows escape and CR pressure gradients continuously accelerate this material well into the IGM in fast outflows, while lower-density gas at large radii is accelerated in-situ into slow outflows that extend to $>$Mpc scales. CGM/IGM outflow morphologies are radically altered: they become mostly volume-filling (with inflow in a thin mid-plane layer) and coherently biconical from the disk to $>$Mpc. The CR-driven outflows are primarily cool ($Tsim10^{5},$K) and low-velocity. All of these effects weaken and eventually vanish at lower halo masses ($lesssim 10^{11},M_{odot}$) or higher redshifts ($zgtrsim 1-2$), reflecting the ratio of CR to thermal+gravitational pressure in the outer halo. We present a simple analytic model which explains all of the above phenomena.
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