Binary Star Formation and the Outflows from their Discs
  We carry out magnetohydrodynamical simulations with FLASH of the formation of
a single, a tight binary ($a\sim$2.5 AU) and a wide binary star ($a\sim$45 AU).
We study the outflows and jets from these systems to understand the
contributions the circumstellar and circumbinary discs have on the efficiency
and morphology of the outflow. In the single star and tight binary case we
obtain a single pair of jets launched from the system, while in the wide binary
case two pairs of jets are observed. This implies that in the tight binary case
the contribution of the circumbinary disc on the outflow is greater than that
in the wide binary case. We also find that the single star case is the most
efficient at transporting mass, linear and angular momentum from the system,
while the wide binary case is less efficient ($\sim$50$\%, \sim$33$\%,
\sim$42$\%$ of the respective quantities in the single star case). The tight
binary's efficiency falls between the other two cases ($\sim$71$\%, \sim$66$\%,
\sim$87$\%$ of the respective quantities in the single star case). By studying
the magnetic field structure we deduce that the outflows in the single star and
tight binary star case are magnetocentrifugally driven, whereas in the wide
binary star case the outflows are driven by a magnetic pressure gradient.
