Signatures of Planet Migration in Cluster Chemistry
Tuesday 3 July, 10:10
Stellar formation models assume stars form in chemically well mixed clouds leading to readily observable consequences for binary stars and clusters. All of the dwarf stars in a cluster should be chemically homogeneous, as should binaries that formed together. Planet migration should occasionally result in planets being pushed into their stellar host, and evidence of this pollution has been clearly seen in white dwarfs, their normally smooth spectra temporarily sprinkled with metal lines. The thin atmospheres of main sequence F and G dwarfs can retain a record of planet engulfment in their observed chemical abundance patterns. Using MESA stellar evolutionary models, we explored the magnitude of these signatures for a selection of stars. We have also obtained high resolution spectra of both the Hyades and Praesepe to derive abundances and place constraints on the frequency of migration that results in planet engulfment.