Young stars constantly accrete material from their protoplanetary disks. For hot stars, this accretion signature can be detected in the composition of the stellar photosphere because of the slow mixing of materials compared to convective mixing in cooler stars. The formation of giant planets carves out gaps in the protoplanetary disks. These gaps produce a unique signature in the composition of the accreting material and, thus, also on the stellar photosphere. With the disk evolution, the protoplanetary disk transitions into a debris disk similar to the Kuiper belt of our Solar system. At this stage, the accretion of material from the debris disk onto the star is insufficient to produce any significant accretion signature. Although this is true, there has been no targeted investigation of the composition of stars hosting debris disks. In this work, we measured the stellar abundances of six young debris disk-hosting stars to check for any anomaly in their composition and identify their potential origins.