  The meter-size barrier in protoplanetary disks is a major challenge in planet
formation, for which many solutions were suggested. One of the leading
solutions is dust traps, that halt or slow the inward migration of dust
particles. The source and profile of these traps are still not completely
known. Warped disks are ubiquitous among accretion disks in general and
protoplanetary disks in particular, and the warping could lead naturally to the
formation of dust traps. Dust traps in warped disks could rise not only from
pressure gradients, but also due to different precession rates between gas and
dust. Here we derive analytically the radial drift in warped disks, and
demonstrate derivation for some specific conditions. The radial drift in warped
protoplanetary disks is qualitatively different, and depending on the structure
of the disk, dust traps could form due to the warping. Similar processes could
lead to the formation of traps also in other accretion disks such as AGN disks.
