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28 March 2024
 
  » arxiv » 1004.3789

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The Dual Origin of Stellar Halos II: Chemical Abundances as Tracers of Formation History
Adi Zolotov ; Beth Willman ; Alyson Brooks ; Fabio Governato ; David W. Hogg ; Sijing Shen ; James Wadsley ;
Date 21 Apr 2010
AbstractFully cosmological, high resolution N-Body + SPH simulations are used to investigate the chemical abundance trends of stars in simulated stellar halos as a function of their origin. These simulations employ a physically motivated supernova feedback recipe, as well as metal enrichment, metal cooling and metal diffusion. As presented in an earlier paper, the simulated galaxies in this study are surrounded by stellar halos whose inner regions contain both stars accreted from satellite galaxies and stars formed in situ in the central regions of the main galaxies and later displaced by mergers into their inner halos. The abundance patterns ([Fe/H] and [O/Fe]) of halo stars located within 10 kpc of a solar-like observer are analyzed. We find that for galaxies which have not experienced a recent major merger, high metallicity in situ stars are more alpha-rich than accreted stars at similar metallicities. This dichotomy in the [O/Fe] of halo stars at a given metallicity results from the different potential wells within which in situ and accreted halo stars form. These results qualitatively match recent observations of local Milky Way halo stars. It may thus be possible for observers to uncover the relative contribution of different physical processes to the Milky Way’s halo formation by observing such trends in stellar populations.
Source arXiv, 1004.3789
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