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.
