The formation of a cluster of stars and brown dwarfs in a turbulent molecular cloud

We present preliminary results from the first hydrodynamic calculation to follow the collapse and fragmentation of a large-scale turbulent molecular cloud into a stellar cluster while resolving beyond the opacity limit for fragmentation. The calculation produces a mixture of single and binary stars with comparable numbers of stars and brown dwarfs. Without exception, the brown dwarfs are formed by ejection from unstable multiple systems. The calculation produces a stellar initial mass function in agreement with observations. However, at this stage in the calculation, no high-mass (> 0.03 M-circle dot) brown dwarfs have been formed because they are ejected too soon after formation to have accreted much mass.