  We use a series of high-resolution N-body simulations of a `Milky-Way' halo,
coupled to semi-analytic techniques, to study the formation of our own Galaxy
and of its stellar halo. Our model Milky Way galaxy is a relatively young
system whose physical properties are in quite good agreement with observational
determinations. In our model, the stellar halo is mainly formed from a few
massive satellites accreted early on during the galaxy's lifetime. The stars in
the halo do not exhibit any metallicity gradient, but higher metallicity stars
are more centrally concentrated than stars with lower abundances. This is due
to the fact that the most massive satellites contributing to the stellar halo
are also more metal rich, and dynamical friction drags them closer to the inner
regions of the host halo.
