  The formation of globular clusters is still an unsolved problem. Though most
scenarios assume a massive molecular cloud as the progenitor, it is unclear,
how the cloud is transformed into a star cluster. Here a scheme of supernova
(SN) induced cluster formation is investigated. In this scenario the expanding
SN shell accumulates the mass of the cloud. This is accompanied by
fragmentation resulting in star formation in the shell. If this stellar shell
expands sufficiently slow, its self-gravity leads to a recollapsing shell, by
this forming one or several stellar clusters.
  In this paper N-body simulations of collapsing shells moving on circular
orbits in a galactic potential are presented. It is shown that typical shells
(10^5 Msun, 30 pc) evolve to twin clusters in the galactocentric distance range
between 3 and 11 kpc. Their masses show a strong radial trend: on orbits inside
5 kpc both clusters have almost equal mass. Outside 5 kpc the more massive twin
cluster contains about 55% of the shell's mass, whereas the mass of the smaller
decreases linearily to 15% at 11 kpc. Outside 11 kpc the collapsing shells end
up in a single cluster. Inside 3 kpc the shells are tidally disrupted and only
fragments substantially less massive than the initial shell survive.
