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The fragmentation of prestellar cores can depend on many factors, such as
the initial levels of thermal, rotational and turbulent energies, the
geometry of the core and the total mass. We investigate the fragmentation
of low-mass prestellar cores driven mainly by rotation by performing numerical
experiments using SPH. In particular, we see how the initial properties
of the core translate to the properties of primordial binaries generated in
the simulations. We consider how our results relate to the observed properties
of binaries in various star-forming regions and young clusters, with particular
focus on small-separation (a < 10 AU) binaries.
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