THE INITIAL CONDITIONS OF YOUNG GLOBULAR-CLUSTERS IN THE LARGE-MAGELLANIC-CLOUD

N-body simulations are used to model the early evolution of globular c lusters. These simulations include residual gas which was not turned i nto stars, which is expelled from the globular cluster by the actions of massive (> 8 M-.) stars. The results of these simulations are compa red with observations of eight LMC globular clusters less than 100 Myr old. These observations are used to constrain the initial conditions that may have produced these clusters. It is found that the observatio ns can be accounted for in a model where the globular clusters form fr om proto-cluster clouds similar to Plummer models with length-scales i n the range 1 < R-s/pc < 3 where the star formation efficiency varies between 25 and 60 per cent. Using these derived initial conditions the survivability of these clusters in both the Galaxy and the LMC is ass essed. If the slope of the initial mass function is around alpha = 2.3 5 then two or three of these clusters may be able to survive for a Hub ble time even in the Galactic halo. In this case these clusters may re present young versions of the Galactic globular cluster population whi ch was severely depleted by the destruction of many of its original me mbers. In the case where alpha = 1.50, however, none of these clusters would be expected to survive for more than a few Gyr at most, even wi thin the LMC.