Dynamical evolution of star clusters with top-heavy IMF
  Several observational and theoretical studies suggest that the initial mass
function (IMF) slope for massive stars in globular clusters (GCs) depends on
the initial cloud density and metallicity, such that the IMF becomes
increasingly top-heavy with decreasing metallicity and increasing the gas
density of the forming object. Using N-body simulations of GCs starting with a
top-heavy IMF and undergo early gas expulsion within a Milky Way-like
potential, we show how such a cluster would evolve. By varying the degree of
top-heaviness, we calculate the dissolution time and the minimum cluster mass
needed for the cluster to survive after 12 Gyr of evolution.
