  A highly misaligned gas disk around one component of a binary star system can
undergo global Kozai-Lidov (KL) oscillations for which the disk inclination and
eccentricity are exchanged. With hydrodynamical simulations of a gas and dust
disk we explore the effects of these oscillations on the dust density
distribution. For dust that is marginally coupled to the gas (${\rm St} \approx
1$), we find that the dust undergoes similar dynamical behaviour to the gas
disk but the radial distribution of dust may be very different to the gas. The
inward radial drift of the dust is faster in an eccentric disk leading to a
smaller outer dust disk radius. The dust breaks into multiple narrow eccentric
rings during the highly eccentric disk phase. Eccentric dust ring formation may
have significant implications for the formation of planets in misaligned disks.
We suggest that multiple dust rings may generally occur within gas disks that
have sufficiently strong eccentricity peaks at intermediate radii.
