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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 | Abstract: | Fully 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 | Services: | Forum | Review | PDF | Favorites |
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