On the occurrence of λ Boötis stars in star clusters

ABSTRACT $\lambda$ Boötis stars are a subset of chemically peculiar A-stars that display Solar abundances in lighter elements (C, N, O, S, etc.) but a deficiency in Iron-peak elements. This difference has been attributed to the A-stars accreting pristine (metal deficient) gas from the Interstellar Medium. However, the recent discovery of $\lambda$ Boötis stars in clusters challenges this theory, due to the presence of ionizing radiation from intermediate/massive ($>$ 5 M$_\odot$) stars, which could prevent accretion of pristine ISM gas. We use N-body simulations to track the dynamical histories of A-stars during the evolution of a star cluster. We find that some stars leave the confines of the cluster and travel beyond the tidal radius, where they may be able to accrete pristine ISM gas. These A-stars then sometimes move back into the inner regions of the cluster, but the photoionizing radiation flux they receive is not high enough to prevent $\lambda$ Boötis abundances from occurring in these A-stars. We find that A-stars can develop $\lambda$ Boötis abundances and subsequently form a wide (${>}100$ au) binary system, meaning that observations of binary systems that have different abundances between the component stars would not rule out the ISM accretion scenario. Whilst we have shown that $\lambda$ Boötis stars can reside in and around star clusters, further research is required to assess the validity of the accretion rates required to explain their abundance patterns.