The Turbulent Origin of Outflow and Spin Misalignment in Multiple Star
  Systems
  The protostellar outflows of wide-separation forming binaries frequently
appear misaligned. We use magneto-hydrodynamic simulations to investigate the
alignment of protostellar spin and molecular outflows for forming binary pairs.
We show that the protostellar pairs, which form from turbulent fragmentation
within a single parent core, have randomly oriented angular momenta. Although
the pairs migrate to closer separations, their spins remain partially
misaligned. We produce $^{12}$CO(2-1) synthetic observations of the simulations
and characterize the outflow orientation in the emission maps. The
CO-identified outflows exhibit a similar random distribution and are also
statistically consistent with the observed distribution of molecular outflows.
We conclude that observed misalignment provides a clear signature of binary
formation via turbulent fragmentation. The persistence of misaligned outflows
and stellar spins following dynamical evolution may provide a signature of
binary origins for more evolved multiple star systems.
