  We found that 10 metal-poor globular clusters are greately distinguished for
anomalously small masses on the "destruction rate--mass" plain. As it turned
out, these poor clusters, situated 15 kpc farther from the Galactic centre, are
somewhat younger than the bulk of the metal-poor globulars, and have
anomalously red horizontal branches. All these clusters are supposed to belong
to the "young halo" subsystem, i.e. they are supposed to have been captured by
the Galaxy at different stages of their evolution. We discovered a significant
correlation between the ages found from isochrones and masses of globulars
which lie at galactocentric distances greater than the radius of the solar
orbit. At the same time, deficiency of distant massive clusters is noticeable
with increasing distance from the galactic centre. So we see unticorrelation
between the galactocentric distance and masses of distant clusters. Both
relations are negligible for the inner clusters of the Galaxy. We assume that
favourable conditions for violent dissipation with considerable loss of mass
are realised inside the protoglobulars which formed far from the Galactic
centre.
