  We present results from the first three-dimensional calculations ever to
follow the collapse of a molecular cloud core (~ 10^{-18} g cm^{-3}) to stellar
densities (> 0.01 g cm^{-3}). The calculations resolve structures over 7 orders
of magnitude in spatial extent (~ 5000 AU - 0.1 R_\odot), and over 17 orders of
magnitude in density contrast. With these calculations, we consider whether
fragmentation to form a close binary stellar system can occur during the second
collapse phase. We find that, if the quasistatic core that forms before the
second collapse phase is dynamically unstable to the growth of non-axisymmetric
perturbations, the angular momentum extracted from the central regions of the
core, via gravitational torques, is sufficient to prevent fragmentation and the
formation of a close binary during the subsequent second collapse.
