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Published online by Cambridge University Press: 05 April 2019
The binary fraction of metal-poor stars provides important constraints on star formation in the early Galaxy, and is a key piece of information in the understanding the origin of the observed high frequency of C enhanced metal-poor stars. It is now widely accepted that a majority of solar metallicity stars are in binaries; it is not clear, however, if this is the case for metal-poor stars. While state-of-the-art models agree in predicting an increase in the binary fraction and a shift towards lower values for the orbital period distribution at extremely low metallicities, the observational findings paint a patchier picture. This chapter summarises the key motivations for the study of binaries in the very metal-poor regime and reviews the current state of the field and the plans for the future.
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