  We study the evolution of the galactic globular cluster system to determine
its initial mass-function and the fraction of halo stars that could have come
from disrupted globular clusters. We study the cluster evolution under the
influence of two destruction mechanisms: Two-body relaxation and dynamical
friction. New results of N-body simulations are used for the lifetimes of
clusters dissolving under the influence of two-body relaxation.
  Two different mass-functions are studied: A gaussian initial distribution in
log(M_C) with mean mass and scatter similar to what one observes for the
galactic globular cluster system, and a power-law distribution resembling what
is seen for clusters in merging and interacting galaxies. We find that in the
inner parts of the galaxy, both distributions evolve in such a way that they
are consistent with the observations. In the outer parts, a gaussian initial
distribution gives the better fit. This might change however if elliptic orbits
are considered, or there are undiscovered low-mass clusters in the galactic
halo. In any case, only a small fraction of the stellar halo of the Milky Way
originated in globular clusters.
