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 ] \leq - 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 ] \leq - 1.6 and approximately for the intermediate abundance range of -1.6 < [ Fe/H ] \leq - 1.0 .
We show that this successful reproduction 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 .