  We construct self-consistent dynamical models for disk galaxies with
triaxial, cuspy halos. We begin with an equilibrium, axisymmetric,
disk-bulge-halo system and apply an artificial acceleration to the halo
particles. By design, this acceleration conserves energy and thereby preserving
the system's differential energy distribution even as its phase space
distribution function is altered. The halo becomes triaxial but its
spherically-averaged density profile remains largely unchanged. The final
system is in equilibrium, to a very good approximation, so long as the halo's
shape changes adiabatically. The disk and bulge are ``live'' while the halo is
being deformed; they respond to the changing gravitational potential but also
influence the deformation of the halo. We test the hypothesis that halo
triaxiality can explain the rotation curves of low surface brightness galaxies
by modelling the galaxy F568-3.
