  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]$\le-1.0$, 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]$\le-1.6$ and approximately for the intermediate abundance
range of $-1.6<$[Fe/H]$\le-1.0$. 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.
