  Some aspects of disk-halo interactions for models of in and out of
equilibrium disk galaxies are reviewed. Specifically, we focus on disk-halo
resonant interaction without and in the presence of a gas component. Another
issue is the disk growth within an assembling triaxial dark matter halo. We
argue that while the triaxiality is the result of the merger process and the
radial orbit instability, it is the developing chaos that damps the first
generation of bars and washes out the halo prolateness. This chaos is triggered
by the gravitational quadrupole interaction(s) in the system and supported by a
number of other processes which are characteristic of baryons.
