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Metal-poor stars hold the key to our understanding of the origin of theelements and the chemical evolution of the Universe. This chapter describes theprocess of discovery of these rare stars, the manner in which their surfaceabundances (produced in supernovae and other evolved stars) are determined fromthe analysis of their spectra, and the interpretation of their abundancepatterns to elucidate questions of origin and evolution. More generally,studies of these stars contribute to other fundamental areas that includenuclear astrophysics, conditions at the earliest times, the nature of the firststars, and the formation and evolution of galaxies -- including our own MilkyWay. We illustrate this with results from studies of lithium formed during theBig Bang; of stars dated to within ~1 Gyr of that event; of the most metal-poorstars, with abundance signatures very different from all other stars; and ofthe build-up of the elements over the first several Gyr. The combination ofabundance and kinematic signatures constrains how the Milky Way formed, whilerecent discoveries of extremely metal-poor stars in the Milky Way's dwarfgalaxy satellites constrain the hierarchical build-up of its stellar halo fromsmall dark-matter dominated systems. [abridged]

Metal-Poor Stars and the Chemical Enrichment of the Universe