  Protostellar jets and outflows are signatures of star formation and promising
mechanisms for driving supersonic turbulence in molecular clouds. We quantify
outflow-driven turbulence through three-dimensional numerical simulations using
an isothermal version of the robust total variation diminishing code. We drive
turbulence in real-space using a simplified spherical outflow model, analyse
the data through density probability distribution functions (PDF), and
investigate the Core Formation Rate per free-fall time (CFR_ff). The real-space
turbulence driving method produces a negatively skewed density PDF possessing
an enhanced tail on the low-density side. It deviates from the log-normal
distributions typically obtained from Fourier-space turbulence driving at low
densities, but can provide a good fit at high-densities, particularly in terms
of mass weighted rather than volume weighted density PDF. Due to this fact, we
suggest that the CFR_ff determined from a Fourier-driven turbulence model could
be comparable to that of our particular real-space driving model, which has a
ratio of solenoidal to compressional components from the resulting turbulence
velocity fields of ~0.6.
