  We investigate the tilting and warping of galactic disks in response to tidal
torquing. The strength of the torque is determined from cosmological N-body
simulations. We find the tidal torques to be dominated by substructure in the
galactic halo, such as dwarf satellites, and by a misalignment between the disk
angular momentum and the figure axes of the dark matter halo. The radial
dependence of the torque can approximated by a power law of index -2.5. A
massless disk subjected to such a torque develops a trailing warp similar to
those seen in a large number of disk galaxies, i.e. the inner regions of the
disk tilt faster than the outer disk. In the case of massive disks, self
gravity causes the inner disk to stay locally flat and only the outer regions
show the signatures of warps. The radius outside of which a massive disk is
warped depends on the local surface density of the disk and on the product of
the strength of the torque and the exposure time to this torque.
