By emphasizing the dynamical role of Cosmic Rays (CR's) in galactic haloes, it is argued that the region can be divided into a lower part, 120 pc less-than-or-equal-to Absolute value of z less-than-or-equal-to 1 kpc, typically (also called the disk-halo interface), where CR diffusion prevails and an upper part, Absolute value of z greater-than-or-equal-to 1 kpc, which is the site of galactic wind formation due to a strong coupling between the CR's and self-excited hydromagnetic waves (cf Paper 1). A stationary, but non-static model for the lower halo is described, in which the thermal and the CR pressure push the gas against a gravitational pull, which can either increase with distance from the disk or remain approximately constant. Since the halo gas is shock heated material (approximately 10(6) K) from supernova remnants, we allow for mass loading of the flow. We present analytical solutions for typical disk parameters such as gas density, gas and CR pressure, appropriate for the Galaxy, and show that it is possible to match them to the outflow solutions in the upper halo. It turns out that the flow of the disk-halo interface is always subsonic. In order to obtain physically reasonable velocity profiles in that region, we find that the observationally permitted range of mass loading is considerably restricted. The effect of the CR's on the flow is that for a diffusion coefficient kappaBAR less-than-or-equal-to kappa(crit)BAR the halo density exhibits a maximum. The problem of stability of these stationary solutions is also discussed within the context of overturning and cooling.
