Despite problems with calibration issues, a large amount of valuable data was collected by the satellite, improving our knowledge of stars with already known excesses and discovering a number of new candidates. Since it appears that a large percentage of stars exhibit these excesses, it would be useful to analyze what effects they might have on the evolution of their parent star. This would indicate that older stars either more efficiently accrete the material in their disks or that lower mass stars are less likely to form detectable disks. However, I am more interested in how disks affect the chemical abundances of their parents stars. There are two possible scenarios other than the null possibility where disk stars are identical chemically to non-disk stars, either the disk will enhance the metal content of the star through accretion or it will lower the metalicity of the parent star by acting as a sink for iron and other heavy elements.
Planetesimals appear to have iron cores surrounded by shells of silicates and ice.
There is strong evidence that at least Beta Pictoris has a region approximately the size of our solar system which is relatively free of dust. From this we can infer, along with corroborating models, that within a certain radius at least the star is fairly efficient at accreting the material in its disk. If this is the case, and the rate of the accretion was high enough, then we could expect to see increased abundances of the elements present in the cloud, most notably iron and silicates. It is also easy to conceive of the alternative scenario where heavier elements entering the region around the star that would normally have incresed the abundances of the star actually is caught up in the disk in the process of planet formation. In this case there would be notable low abundances of heavier elements, and perhaps even lighter ones as they are used to form planets and other large particles.