We have undertaken a series of hydrodynamic + N-body simulations in order to explore the properties of young stars .
Our results suggest that the IMF may be sensitive to environment in its substellar region , with more brown dwarfs being formed where clusters are denser or more compact .
We find that multiple stars are a natural outcome of collapsing turbulent flows , with a high incidence of N > 2 multiples .
We find a positive correlation of multiplicity with primary mass but a companion frequency that decreases with age .
Binary brown dwarfs are rarely formed , in conflict with observations .
Brown dwarfs as companions are predominantly found orbiting binaries or triples at large separations .