Stellar and brown dwarf properties from numerical simulations

We review the statistical properties of stars and brown dwarfs obtained from the first hydrodynamical simulation of star cluster formation to produce more than a thousand stars and brown dwarfs while simultaneously resolving the lowest mass brown dwarfs (those with masses set by the opacity limit for fragmentation), binaries with separations down to ∼ 1 AU, and discs with radii greater than ∼ 10 AU. In particular, we present the eccentricity distribution of the calculation’s very-low-mass and brown dwarf binaries which has not been previously published.