Formation of the galactic stellar halo: Origin of the metallicity-eccentricity relation

Kenji Bekki, Masashi Chiba

Research output: Contribution to journalArticlepeer-review

17 Citations (Scopus)


Motivated by the recently improved knowledge on the kinematic and chemical properties of the Galactic metal-poor stars, we present the numerical simulation for the formation of the Galactic stellar halo to interpret the observational results. As a model for the Galaxy contraction, we adopt the currently standard theory of galaxy formation based on the hierarchical assembly of the cold dark matter fluctuations. We find, for the simulated stars with [Fe/H] ≤ -1.0, that there is no strong correlation between metal abundances and orbital eccentricities, in good agreement with the observations. Moreover, the observed fraction of the low-eccentricity stars is reproduced correctly for [Fe/H] ≤ - 1.6 and approximately for the intermediate abundance range of -1.6 < [Fe/H] ≤ -1.0. We show that this successful reproductior of the kinematics of the Galactic halo is a natural consequence of the hierarchical evolution of the subgalactic clumps seeded from the cold dark matter density fluctuations.

Original languageEnglish
Pages (from-to)L89-L92
JournalAstrophysical Journal
Issue number1 PART 2
Publication statusPublished - 2000 May 1
Externally publishedYes


  • Galaxy: abundances
  • Galaxy: evolution
  • Galaxy: halo

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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