Abstract
Observations of star-forming regions show that they are turbulent, with complex morphologies and velocity structures. Nonetheless, published calculations of the collapse and fragmentation of molecular cloud cores have either assumed highly symmetric, quiescent initial conditions or have included turbulence on scales too large to resolve the details of collapse and fragmentation. We present a method for the first step in producing realistic, turbulent molecular cloud core models. Simulated observations of these models show excellent agreement with observed cores.
