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A suggested explanation for the observed differences in chemical abundances in binary stars has been planet formation (e.g. Tucci Maia et al. 2014). If a star hosts a planet, the planet may have depleted the protoplanetary disc in volatiles and refractories. Assuming that the star accretes the remaining protoplanetary disc (neglecting photoevaporation), the depletion of the disc may alter the chem
