The formation mechanism and resulting properties of brown dwarfs

We present results from the most complex hydrodynamical star formation calculation performed to date. It follows the collapse and fragmentation of a large-scale turbulent molecular cloud to form dozens of stars and brown dwarfs. It resolves all fragmentation down to the opacity limit, binary stars with separations as small as 1 AU, and circumstellar disks with radii down to approximate to 10 AU. In this proceedings, we examine the formation mechanism of the brown dwarfs-and compare the initial mass function and the properties of the brown dwarfs with observations.