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Binary star systems are assumed to be co-natal and coeval, thus to haveidentical chemical composition. In this work we aim to test the hypothesis thatthere is a connection between observed element abundance patterns and theformation of planets using binary stars. Moreover, we also want to test howatomic diffusion might influence the observed abundance patterns. We conduct astrictly line-by-line differential chemical abundance analysis of 7 binarysystems. Stellar atmospheric parameters and elemental abundances are obtainedwith extremely high precision (< 3.5%) using the high quality spectra fromVLT/UVES and Keck/HIRES. We find that 4 of 7 binary systems show subtleabundance differences (0.01 - 0.03 dex) without clear correlations with thecondensation temperature, including two planet-hosting pairs. The other 3binary systems exhibit similar degree of abundance differences correlating withthe condensation temperature. We do not find any clear relation between theabundance differences and the occurrence of known planets in our systems.Instead, the overall abundance offsets observed in the binary systems (4 of 7)could be due to the effects of atomic diffusion. Although giant planetformation does not necessarily imprint chemical signatures onto the host star,the differences in the observed abundance trends with condensation temperature,on the other hand, are likely associated with diverse histories of planetformation (e.g., formation location). Furthermore, we find a weak correlationbetween abundance differences and binary separation, which may provide a newconstraint on the formation of binary systems.

Detailed elemental abundances of binary stars: Searching for signatures of planet formation and atomic diffusion