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Fully cosmological, high resolution N-Body + SPH simulations are used toinvestigate the chemical abundance trends of stars in simulated stellar halosas a function of their origin. These simulations employ a physically motivatedsupernova feedback recipe, as well as metal enrichment, metal cooling and metaldiffusion. As presented in an earlier paper, the simulated galaxies in thisstudy are surrounded by stellar halos whose inner regions contain both starsaccreted from satellite galaxies and stars formed in situ in the centralregions of the main galaxies and later displaced by mergers into their innerhalos. The abundance patterns ([Fe/H] and [O/Fe]) of halo stars located within10 kpc of a solar-like observer are analyzed. We find that for galaxies whichhave not experienced a recent major merger, in situ stars at the high [Fe/H]end of the metallicity distribution function are more [alpha/Fe]-rich thanaccreted stars at similar [Fe/H]. This dichotomy in the [O/Fe] of halo stars ata given [Fe/H] results from the different potential wells within which in situand accreted halo stars form. These results qualitatively match recentobservations of local Milky Way halo stars. It may thus be possible forobservers to uncover the relative contribution of different physical processesto the formation of stellar halos by observing such trends in the halopopulations of the Milky Way, and other local L* galaxies.

The Dual Origin of Stellar Halos II: Chemical Abundances as Tracers of Formation History