We use numerical simulations to investigate the orbital characteristics of tidal debris from satellites whose orbits are dragged into the plane of galact ic disks by dynamical friction before disruption. We find that these satellites may deposit a s ignificant fraction of their stars into the disk components of a galaxy, and use our results to motivate the search for accretion relicts in samples of metal-poor disk stars in the vicinity o f the Sun. Satellites disrupted on very eccentric orbits coplanar with the disk are expected to shed stars in “trails” of distinct orbital energy and angular momentum during each pericentric passage. To an observer located between the pericenter and apocenter of such orbits, these trails would show as distinct groupings of stars with low vertical velocity and a broad, symmetric, often double-peaked distribution of Galactocentric radial velocities. One group of st ars with these characteristics stands out in available compilations of nearby metal-poor stars. These stars have specific angular momenta similar to that of the globular cluster ωCen, long hypothesized to be the nucleus of a dwarf galaxy disrupted by the Milky Way tidal field. In addit ion to their kindred kinematics, stars in the ωCen group share distinct chemical abundance characteristics, and trace a welldefined track in the [ α/Fe] versus [Fe/H] plane, consistent with simple closed-box enrichment models and a protracted star formation history. The dynamical and chemical coherence of this group suggests that it consists of stars that once belonged t o the dwarf that brought ωCen into the Galaxy. The presence of this and other “tidal relicts” in the solar neighbourhood suggest an extra-Galactic origin for the presence of nearby stars with odd kinematics and chemistry, and implies that accounting for stars contributed by distin ct satellite galaxies may be crucial to the success of models of Galactic chemical enrichment.