Young stars accrete material from their protoplanetary disks, which can contaminate the stellar photosphere. This is especially noticeable in hot stars with radiative envelopes, where slower mixing in the photosphere preserves these contamination signatures over longer timescales. The accreted material carries a chemical imprint, particularly in disks with gaps, where dust is trapped at the outer edge while gas moves inward. This results in the accretion of dust-poor material, leading to a photospheric abundance pattern with depletion of refractory elements (e.g. - Fe, Mg), while volatile elements (e.g. - C, O) remain unchanged. These chemically peculiar stars are known as lambda Bootis-type stars. These contamination signatures at the stellar photosphere give us valuable insights into the elemental composition of the inner disk since the accreted material comes from this region.

In our recent work, we explore young, hot stars hosting debris disks, a later stage in protoplanetary disk evolution. While debris disks have low accretion rates that don't significantly affect the stellar photosphere, there has been little work on abundance anomalies in these stars. We analyzed high-resolution spectra of six such stars and identified two that exhibit lambda Bootis-type peculiarities. This talk will discuss the origins of these peculiarities in these two stars and compare young debris disk-hosting stars with their protoplanetary disk-hosting counterparts. Understanding these anomalies may provide insights into similar lambda Bootis-type stars over 100 million years old, where accretion from a circumstellar disk is not expected.

recording: www.youtube.com/watch